FN Thomson Reuters Web of Science™ VR 1.0 PT S AU Neudeck, PG Spry, DJ Trunek, AJ AF Neudeck, Philip G. Spry, David J. Trunek, Andrew J. BE Devaty, RP TI Measurements of breakdown field and forward current stability in 3C-SiC pn junction diodes grown on step-free 4H-SiC SO SILICON CARBIDE AND RELATED MATERIALS 2005, PTS 1 AND 2 SE Materials Science Forum LA English DT Proceedings Paper CT International Conference on Silicon Carbide and Related Materials (ICSCRM 2005) CY SEP 18-23, 2005 CL Pittsburgh, PA SP Aixtron, Cree Inc, Dow Corning, GE Global Res Ctr, II VI, Inc, Intrins Semicond, KLA Tencor, SiCED, SiCrystal AG DE 3C-SiC; pn junction; p(+)n diode; rectifier; reverse breakdown; breakdown field; heteroepitaxy; epitaxial growth; electroluminescence; mesa; bipolar diode AB This paper reports on initial fabrication and electrical characterization of 3C-SiC p(+)n junction diodes grown on step-free 4H-SiC mesas. Diodes with n-blocking-layer doping ranging from similar to 2 x 10(16) cm(-3) to similar to 5 x 10(17) cm(-3) were fabricated and tested. No optimization of junction edge termination or ohmic contacts was employed. Room temperature reverse characteristics of the best devices show excellent low-leakage behavior, below previous 3C-SiC devices produced by other growth techniques, until the onset of a sharp breakdown knee. The resulting estimated breakdown field of 3C-SiC is at least twice the breakdown field of silicon, but is only around half the breakdown field of < 0001 > 4H-SiC for the doping range studied. Initial high current stressing of 3C diodes at 100 A/cm(2) for more than 20 hours resulted in less than 50 mV change in similar to 3 V forward voltage. C1 [Neudeck, Philip G.] NASA, Glenn Res Ctr, OAI, MS 77-1,21000 Brookpk Rd, Cleveland, OH 44135 USA. [Spry, David J.; Trunek, Andrew J.] NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Neudeck, PG (reprint author), NASA, Glenn Res Ctr, OAI, MS 77-1,21000 Brookpk Rd, Cleveland, OH 44135 USA. EM Neudeck@nasa.gov; David.J.Spry@grc.nasa.gov; Andrew.J.Trunek@grc.nasa.gov FU Ultra Efficient Engine Technology Project at NASA Glenn Research Center FX This work was funded and carried out under the Ultra Efficient Engine Technology Project at NASA Glenn Research Center. The authors thank G. Hunter, E. Benavage, R. Okojie, J. A. Powell, B. Osborn, M. Mrdenovich, G. Beheim, R. Meredith, T. Ferrier, D. Lukco, K. Laster, C. Blaha, P. Lampard, J. Gonzalez, D. Androjna, and L. Matus at NASA Glenn and Prof. M.-C. Cheng at Clarkson University for their support. NR 12 TC 6 Z9 6 U1 0 U2 0 PU TRANS TECH PUBLICATIONS LTD PI DURNTEN-ZURICH PA KREUZSTRASSE 10, 8635 DURNTEN-ZURICH, SWITZERLAND SN 0255-5476 J9 MATER SCI FORUM PY 2006 VL 527-529 BP 1335 EP + PG 2 WC Materials Science, Multidisciplinary SC Materials Science GA BFS29 UT WOS:000244227200315 ER PT S AU Yan, F Xin, XB Alexandrov, P Stahle, CM Guan, B Zhao, JH AF Yan, Feng Xin, Xiaobin Alexandrov, Petre Stahle, Carl M. Guan, Bing Zhao, Jian H. BE Devaty, RP TI Development of ultra high sensitivity UV silicon carbide detectors SO Silicon Carbide and Related Materials 2005, Pts 1 and 2 SE MATERIALS SCIENCE FORUM LA English DT Proceedings Paper CT International Conference on Silicon Carbide and Related Materials (ICSCRM 2005) CY SEP 18-23, 2005 CL Pittsburgh, PA SP Aixtron, Cree Inc, Dow Corning, GE Global Res Ctr, II VI, Inc, Intrins Semicond, KLA Tencor, SiCED, SiCrystal AG DE detector; detectivity; ultraviolet; avalanche photodiode; photon-counter AB A variety of silicon carbide (SiC) detectors have been developed to Study their sensitivity, including Schottky photodiodes, p-i-n photodiodes, avalanche photodiodes (APDs), and single photon-counting APDs. Due to the very wide bandgap and thus extremely low leakage Current, SiC photo-detectors show excellent sensitivity. The specific detectivity, D*, of SiC photodiodes are many orders of magnitude higher than the D* of other solid state detectors, and for the first time, comparable to that of photomultiplier tubes (PMTs). SiC APDs have also been fabricated to pursue the ultimate sensitivity. By operating the SiC APDs at a linear mode gain over 10(6), single photon-counting avalanche photodiodes (SPADs) in UV have been demonstrated. C1 NASA, Goddard Space Flight Ctr, Detector Syst Branch, Greenbelt, MD 20771 USA. Rutgers State Univ, Dept ECE, Piscataway, NJ 08854 USA. United Silicon Carbide Inc, New Brunswick, NJ 08902 USA. RP Yan, F (reprint author), NASA, Goddard Space Flight Ctr, Detector Syst Branch, Code 553, Greenbelt, MD 20771 USA. NR 7 TC 7 Z9 8 U1 0 U2 0 PU TRANS TECH PUBLICATIONS LTD PI STAFA-ZURICH PA LAUBLSRUTISTR 24, CH-8717 STAFA-ZURICH, SWITZERLAND SN 0255-5476 J9 MATER SCI FORUM PY 2006 VL 527-529 BP 1461 EP 1464 PG 4 WC Materials Science, Multidisciplinary SC Materials Science GA BFS29 UT WOS:000244227200346 ER PT S AU Eddy, CR Bassim, ND Mastro, MA Henry, RL Twigg, ME Holm, RT Culbertson, JC Neudeck, PG Powell, JA Trunek, AJ AF Eddy, C. R., Jr. Bassim, N. D. Mastro, M. A. Henry, R. L. Twigg, M. E. Holm, R. T. Culbertson, J. C. Neudeck, P. G. Powell, J. A. Trunek, A. J. BE Devaty, RP TI Reduction of defects in GaN epitaxial films grown heteroepitaxially on SiC SO Silicon Carbide and Related Materials 2005, Pts 1 and 2 SE MATERIALS SCIENCE FORUM LA English DT Proceedings Paper CT International Conference on Silicon Carbide and Related Materials (ICSCRM 2005) CY SEP 18-23, 2005 CL Pittsburgh, PA SP Aixtron, Cree Inc, Dow Corning, GE Global Res Ctr, II VI, Inc, Intrins Semicond, KLA Tencor, SiCED, SiCrystal AG DE GaN; defects; heteroepitaxy ID MOLECULAR-BEAM EPITAXY; VAPOR-PHASE EPITAXY; ALN BUFFER LAYERS; ELECTRON-MICROSCOPY; STRUCTURAL DEFECTS; THIN-FILMS; TEMPERATURE; NUCLEATION; INTERFACE; SUBSTRATE AB Silicon carbide (SiC) has become the substrate of choice for III-N epilayers applied to electronic devices due to the lack of a native III-N substrate. This is particularly true for high power applications, since the thermal conductivity of the substrate enhances device performance. Although the GaN lattice match is slightly better for SiC than for sapphire, the dislocation densities that result are still very high (generally in the high 10(8) cm(-2) range) and often deleterious to device performance. Screw-component dislocations are especially critical since they serve as leakage paths in vertically conducting III-N devices. In this paper efforts to reduce the extended defect density in III-N films grown on SiC will be reviewed. Details on recent efforts to use step-free SiC mesa surfaces arrayed on commercial 4H-SiC substrates will then be highlighted showing dramatic reductions in extended defect densities and the virtual elimination of critical defects for vertically conducting devices. In these experiments, SiC surfaces that are homoepitaxially grown step-free or of very low step density have been used as growth templates for thin (< 3 mu m) GaN films deposited on a novel 1000 angstrom AlN nucleation layer characterized by a total dislocation density two orders of magnitude lower than the previous state-of-the-art, and with no evidence of screw-component dislocations. C1 USN, Res Lab, Div Elect Sci & Technol, Washington, DC 20375 USA. NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. Seat Inc, Cleveland, OH 44135 USA. OAI, Cleveland, OH 44135 USA. RP Eddy, CR (reprint author), USN, Res Lab, Div Elect Sci & Technol, Washington, DC 20375 USA. NR 31 TC 2 Z9 2 U1 0 U2 2 PU TRANS TECH PUBLICATIONS LTD PI STAFA-ZURICH PA LAUBLSRUTISTR 24, CH-8717 STAFA-ZURICH, SWITZERLAND SN 0255-5476 J9 MATER SCI FORUM PY 2006 VL 527-529 BP 1483 EP 1488 PG 6 WC Materials Science, Multidisciplinary SC Materials Science GA BFS29 UT WOS:000244227200351 ER PT S AU Bassim, ND Twigg, ME Mastro, MA Neudeck, P Eddy, CR Henry, RL Holm, RN Powel, JA Trunek, AJ AF Bassim, N. D. Twigg, M. E. Mastro, M. A. Neudeck, P. Eddy, C. R., Jr. Henry, R. L. Holm, R. N. Powel, J. A. Trunek, A. J. BE Devaty, RP TI Electron microscopy investigation of the role of surface steps in the generation of dislocations during MOCVD growth of GaN on 4H-SiC SO Silicon Carbide and Related Materials 2005, Pts 1 and 2 SE MATERIALS SCIENCE FORUM LA English DT Proceedings Paper CT International Conference on Silicon Carbide and Related Materials (ICSCRM 2005) CY SEP 18-23, 2005 CL Pittsburgh, PA SP Aixtron, Cree Inc, Dow Corning, GE Global Res Ctr, II VI, Inc, Intrins Semicond, KLA Tencor, SiCED, SiCrystal AG DE surface step; 4H-SiC; GaN; TEM; dislocation; heteroepitaxy ID NUCLEATION; EPITAXY; FILMS AB Through the use of specially-prepared on-axis SiC substrates with patterned mesa tops completely free of atomic-scale surface steps, we have previously reported the growth of high-quality GaN heteroepitaxial films with greatly reduced threading dislocation densities on the order of 10(7)/cm(2). In these films, we reported a defect substructure in which lateral a-type dislocations are present in the nucleation layer but do not bow into threading dislocations during the subsequent GaN growth. This study focuses further on the role of SiC substrate surface steps in the generation of misfit, a-type, and threading dislocations at the heteroepitaxial interface. By using weak-beam imaging (both to eliminate Moire effects and to observe narrow dislocation images) from plan-view transmission electron microscopy (TEM), we identify dislocations generated on stepped and unstepped mesas and compare their geometries. We observe that misfit dislocations nucleated on an unstepped SiC mesa are confined to one set of a-type Burgers vectors of the form g=1/3 [2 (1) over bar(1) over bar0], straight and well-ordered so that they are less likely to interact with each other. On the other hand, misfit dislocation structures on a stepped SiC mesa surface are not nearly as well-ordered, having bowed structure with threading dislocations that appear to nucleate at SiC surface steps. C1 USN, Res Lab, Div Elect Sci & Technol, Washington, DC 20375 USA. NASA, Glenn Res Ctr, Cleveland, OH USA. NASA, Sest Inc, Cleveland, OH USA. NASA, OAI, Cleveland, OH USA. RP Bassim, ND (reprint author), USN, Res Lab, Div Elect Sci & Technol, Washington, DC 20375 USA. NR 12 TC 3 Z9 3 U1 0 U2 2 PU TRANS TECH PUBLICATIONS LTD PI STAFA-ZURICH PA LAUBLSRUTISTR 24, CH-8717 STAFA-ZURICH, SWITZERLAND SN 0255-5476 J9 MATER SCI FORUM PY 2006 VL 527-529 BP 1509 EP 1512 PG 4 WC Materials Science, Multidisciplinary SC Materials Science GA BFS29 UT WOS:000244227200357 ER PT S AU Wang, X Shakouri, A Yu, B Sun, XH Meyyappan, M AF Wang, Xi Shakouri, Ali Yu, Bin Sun, Xuhui Meyyappan, Meyya GP IEEE TI Phonon confinement in Germanium nanowires SO SIXTEENTH BIENNIAL UNIVERSITY/GOVERNMENT/INDUSTRY MICROELECTRONICS SYMPOSIUM, PROCEEDINGS SE PROCEEDINGS - UNIVERSITY/GOVERNMENT/INDUSTRY MICROELECTRONICS SYMPOSIUM LA English DT Proceedings Paper CT 16th Biennial University/Government/Industry Microelectronics Symposium CY JUN 25-28, 2006 CL San Jose State Univ, San Jose, CA SP SJSU Coll Engn, Opt Associates Incorp, Intel, Synopsys, Cadence Design Syst HO San Jose State Univ ID SILICON NANOWIRES; STOKES AB Raman spectra for different size Ge nanowires were measured with different excitation laser powers and wavelengths. By eliminating the heating of the sample under illumination, the phonon confinement effect for small size nanowires was clearly identified. C1 [Wang, Xi; Shakouri, Ali] Univ Calif Santa Cruz, Baskin Sch Engn, Santa Cruz, CA 95064 USA. [Yu, Bin; Sun, Xuhui; Meyyappan, Meyya] NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. RP Wang, X (reprint author), Univ Calif Santa Cruz, Baskin Sch Engn, Santa Cruz, CA 95064 USA. EM ali@soe.ucsc.edu NR 12 TC 0 Z9 0 U1 0 U2 1 PU IEEE PI NEW YORK PA 345 E 47TH ST, NEW YORK, NY 10017 USA SN 0749-6877 BN 978-1-4244-0267-0 J9 P UNIV GOVT IND MICR PY 2006 BP 183 EP + PG 2 WC Engineering, Electrical & Electronic; Nanoscience & Nanotechnology SC Engineering; Science & Technology - Other Topics GA BGO25 UT WOS:000248935100035 ER PT B AU Choudhari, M Fischer, P AF Choudhari, M Fischer, P BE Govindarajan, R TI Roughness induced transient growth: Nonlinear effects SO SIXTH IUTAM SYMPOSIUM ON LAMINAR-TURBULENT TRANSITION SE Fluid Mechanics and Its Applications LA English DT Proceedings Paper CT 6th IUTAM Symposium on Laminar-Turbulent Transition CY DEC 13-17, 2004 CL Bangalore, INDIA SP Int Union Theoret & Appl Mech ID PLATE BOUNDARY-LAYER; OPTIMAL DISTURBANCES; BYPASS TRANSITION; INSTABILITY AB Numerical simulations are used to model the disturbance field associated with a spanwise periodic array of circular disks in a laminar boundary layer. Besides capturing the major trends from the recent wind tunnel measurements by White and Ergin (2003), the simulations reveal the intricate effects of disturbance nonlinearity and roughness geometry on the transient growth characteristics in the wake of the roughness array and provide a numerical database for validating detailed features of optimal growth theory in the context of roughness induced stationary disturbances. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. Argonne Natl Lab, 9700 S Cass Ave, Argonne, IL 60439 USA. RP NASA, Langley Res Ctr, Hampton, VA 23681 USA. RI Choudhari, Meelan/F-6080-2017 OI Choudhari, Meelan/0000-0001-9120-7362 NR 15 TC 0 Z9 0 U1 0 U2 0 PU SPRINGER PI DORDRECHT PA PO BOX 17, 3300 AA DORDRECHT, NETHERLANDS BN 1-4020-3459-8 J9 FLUID MECH APPL PY 2006 VL 78 BP 237 EP + PG 2 WC Mechanics SC Mechanics GA BED95 UT WOS:000236905600031 ER PT J AU Arsintescu, L Colletti, LM Caldwell, JA Mallis, MA AF Arsintescu, L. Colletti, L. M. Caldwell, J. A. Mallis, M. A. TI The relative effects of work hours and circadian factors on pilot perfomance SO SLEEP LA English DT Meeting Abstract CT 20th Annual Meeting of the Associated-Professional-Sleep-Societies CY JUN 17-22, 2006 CL Salt Lake City, UT SP Associated Process Sleep Soc C1 San Jose State Univ Fdn, San Jose, CA USA. QSS Inc, Mountain View, CA USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Alertness Solut, Cupertino, CA USA. NR 0 TC 0 Z9 0 U1 1 U2 3 PU AMER ACADEMY SLEEP MEDICINE PI WESTCHESTER PA ONE WESTBROOK CORPORATE CENTER STE 920, WESTCHESTER, IL 60154 USA SN 0161-8105 J9 SLEEP JI Sleep PY 2006 VL 29 SU S MA 177 BP A60 EP A60 PG 1 WC Clinical Neurology; Neurosciences SC Neurosciences & Neurology GA 047ZH UT WOS:000237916700178 ER PT J AU Nguyen-Vu, TDB Chen, H Cassell, AM Andrews, R Meyyappan, M Li, J AF Nguyen-Vu, TDB Chen, H Cassell, AM Andrews, R Meyyappan, M Li, J TI Vertically aligned carbon nanofiber arrays: An advance toward electrical-neural interfaces SO SMALL LA English DT Article DE carbon nanofibers; electrodes; interfaces; prosthetics; tissue engineering ID PC12 CELLS; ELECTRODES; STIMULATION; IMPEDANCE; MECHANISM; RELEASE C1 NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. RP Li, J (reprint author), NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. EM jli@mail.arc.nasa.gov RI Li, Jun/H-7771-2013; OI Li, Jun/0000-0002-3689-8946; Nguyen-Vu, T.D. Barbara/0000-0002-4708-1982 FU NINDS NIH HHS [1 R21 NS047721-01 A1, R21 NS047721] NR 23 TC 122 Z9 126 U1 8 U2 27 PU WILEY-V C H VERLAG GMBH PI WEINHEIM PA PO BOX 10 11 61, D-69451 WEINHEIM, GERMANY SN 1613-6810 J9 SMALL JI Small PD JAN PY 2006 VL 2 IS 1 BP 89 EP 94 DI 10.1002/smll.200500175 PG 6 WC Chemistry, Multidisciplinary; Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Chemistry; Science & Technology - Other Topics; Materials Science; Physics GA 996WH UT WOS:000234205600014 PM 17193561 ER PT S AU Rodgers, SD Charnley, SB AF Rodgers, S. D. Charnley, S. B. BA Jorda, L BF Jorda, L BE Worms, JC Anselmo, L TI Sulfur chemistry in cometary comae SO SMALL BODIES IN THE SOLAR SYSTEM; SPACE DEBRIS 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 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, MS 245-3, 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 FU NASA; SETI Institute; NASA Ames [NCC2-1412] FX This work was supported by NASAs Planetary Atmospheres Program, with funds allocated to the SETI Institute by NASA Ames under Cooperative Agreement No. NCC2-1412. NR 37 TC 0 Z9 0 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 9 BP 1928 EP + DI 10.1016/j.asr.2005.10.006 PG 3 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BFW07 UT WOS:000245035100004 ER PT S AU Johnson, NL AF Johnson, Nicholas L. BA Jorda, L BF Jorda, L BE Worms, JC Anselmo, L TI The new Jettison Policy for the International Space Station SO SMALL BODIES IN THE SOLAR SYSTEM; SPACE DEBRIS 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 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 1 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 oil-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 oil 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, Lyndon B Johnson Space Ctr, Orbital Debris Program Off, Houston, TX 77058 USA. RP Johnson, NL (reprint author), NASA, Lyndon B Johnson Space Ctr, Orbital Debris Program Off, 2101 NASA Pkwy, Houston, TX 77058 USA. EM nicholas.l.johnson@nasa.gon NR 3 TC 0 Z9 0 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 9 BP 2077 EP 2083 DI 10.1016/j.asr.2006.09.006 PG 7 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BFW07 UT WOS:000245035100029 ER PT S AU Noebe, R Padula, S Bigelowo, G Rios, O Garg, A Lercf, B AF Noebe, Ronald Padula, Santo, II Bigelowo, Glen Rios, Orlando Garg, Anita Lercf, Brad BE Armstrong, WD TI Properties of a Ni(19.5)Pd(30)Ti(50.5)high-temperature shape memory alloy in tension and compression - art. no. 617010 SO Smart Structures and Materials 2006: Active Materials: Behavior and Mechanics SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Smart Structures and Materials 2006 Conference CY FEB 27-MAR 02, 2006 CL San Diego, CA SP SPIE, Amer Soc Mech Engineers, Intelligent Mat Forum, Jet Propuls Lab, Natl Sci Fdn DE high-temperature shape memory alloy; NiTiPd; tensile properties; compression; specific work output; shape memory behavior; dynamic modulus; transformation strain; transformation temperatures. ID IMPROVEMENT; TITANIUM AB Potential applications involving high-temperature shape memory alloys have been growing in recent years. Even in those cases where promising new alloys have been identified, the knowledge base for such materials contains gaps crucial to their maturation and implementation in actuator and other applications. We begin to address this issue by characterizing the mechanical behavior of a Ni19.5Pd30Ti50.5 high-temperature shape memory alloy in both uniaxial tension and compression at various temperatures. Differences in the isothermal uniaxial deformation behavior were most notable at test temperatures below the martensite finish temperature. The elastic modulus of the material was very dependent on strain level; therefore, dynamic Young's Modulus was determined as a function of temperature by an impulse excitation technique. More importantly, the performance of a thermally activated actuator material is dependent on the work output of the alloy. Consequently, the strain-temperature response of the Ni19.5Pd30Ti50.5 alloy under various loads was determined in both tension and compression and the specific work output calculated and compared in both loading conditions. It was found that the transformation strain and thus, the specific work output were similar regardless of the loading condition. Also, in both tension and compression, the strain-temperature loops determined under constant load conditions did not close due to the fact that the transformation strain during cooling was always larger than the transformation strain during heating. This was apparently the result of permanent plastic deformation of the martensite phase with each cycle. Consequently, before this alloy can be used under cyclic actuation conditions, modification of the microstructure or composition would be required to increase the resistance of the alloy to plastic deformation by slip. C1 NASA Glenn Res Ctr, Mat & Struct Div, Cleveland, OH 44135 USA. RP Noebe, R (reprint author), NASA Glenn Res Ctr, Mat & Struct Div, Cleveland, OH 44135 USA. RI Rios, Orlando/E-6856-2017 OI Rios, Orlando/0000-0002-1814-7815 NR 22 TC 4 Z9 4 U1 0 U2 2 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6223-3 J9 P SOC PHOTO-OPT INS PY 2006 VL 6170 BP 17010 EP 17010 AR 617010 DI 10.1117/12.658023 PG 13 WC Instruments & Instrumentation; Materials Science, Multidisciplinary; Materials Science, Characterization & Testing SC Instruments & Instrumentation; Materials Science GA BEO52 UT WOS:000238449400032 ER PT S AU Bar-Cohen, Y AF Bar-Cohen, Yoseph BE BarCohen, Y TI Biologically inspired technology using electroactive polymers (EAP) SO SMART STRUCTURES AND MATERIALS 2006: ELECTROACTIVE POLYMER ACTUATORS AND DEVICES (EAPAD) SE Proceedings of SPIE LA English DT Proceedings Paper CT Smart Structures and Materials 2006 Conference CY FEB 27-MAR 02, 2006 CL San Diego, CA SP SPIE, Amer Soc Mech Engineers, Intelligent Mat Forum, Jet Propuls Lab, Natl Sci Fdn DE biomimetics; biologically inspired technologies; robotics; EAP; electroactive polymers AB Evolution allowed nature to introduce highly effective biological mechanisms that are incredible inspiration for innovation. Humans have always made efforts to imitate nature's inventions and we are increasingly making advances that it becomes significantly easier to imitate, copy, and adapt biological methods, processes and systems. This brought us to the ability to create technology that is far beyond the simple mimicking of nature. Having better tools to understand and to implement nature's principles we are now equipped like never before to be inspired by nature and to employ our tools in far superior ways. Effectively, by bio-inspiration we can have a better view and value of nature capability while studying its models to learn what can be extracted, copied or adapted. Using electroactive polymers (EAP) as artificial muscles is adding an important element to the development of biologically inspired technologies. This paper reviews the various aspects of the field of biomimetics and the role that EAP plays and the field outlook. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Bar-Cohen, Y (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM yosi@jpl.nasa.gov NR 14 TC 0 Z9 0 U1 2 U2 6 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6221-7 J9 PROC SPIE PY 2006 VL 6168 AR 616803 DI 10.1117/12.657514 PG 6 WC Instruments & Instrumentation; Physics, Condensed Matter; Polymer Science SC Instruments & Instrumentation; Physics; Polymer Science GA BEO50 UT WOS:000238445800003 ER PT S AU Sherrit, S Doty, B Badescu, M Bao, XQ Bar-Cohen, Y Aldrich, J Chang, ZS AF Sherrit, Stewart Doty, Benjamin Badescu, Mircea Bao, Xiaoqi Bar-Cohen, Yoseph Aldrich, Jack Chang, Zensheu BE White, EV Davis, LP TI Studies of acoustic-electric feed-throughs for power transmission through structures - art. no. 617102 SO Smart Structures and Materials 2006: Industrial and Commercial Applications of Smart Structures Technologies SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Smart Structures and Materials 2006 Conference CY FEB 27-MAR 02, 2006 CL San Diego, CA SP SPIE, Amer Soc Mech Engineers, Intelligent Mat Forum, Jet Propuls Lab, Natl Sci Fdn DE Ultrasonic; Bulk Acoustic Waves; power conversion; isolation; pressure vessels AB There are numerous engineering, design problems where the use of wires to transfer power and communicate data thru the walls of a structure is prohibitive or significantly difficult that it may require a complex design. Using physical feedthroughs in such systems may make them susceptible to leakage of chemicals or gasses, loss of pressure or vacuum, as well as difficulties in providing adequate thermal or electrical insulation. Moreover, feeding wires thru a wall of a structure reduces the strength of the structure and makes the structure prone to cracking due to fatigue that can result from cyclic loading and stress concentrations. One area that has already been identified to require a wireless alternative to electrical feedthroughs would be the container of any Mars Sample Return Mission, which would need wireless sensors to sense a pressure leak and to avoid potential contamination. The idea of using elastic or acoustic waves to transfer power was suggested recently by [Y. Hu, et al., July 2003]. This system allows for the avoidance of cabling or wiring. The technology is applicable to the transfer of power for actuation, sensing and other tasks inside any sealed container or vacuum/pressure vessel. An alternative approach to the modeling presented previously [Sherrit et al., 2005] used network analysis to solve the same problem in a clear and expandable manner. Experimental tests on three different designs of these devices were performed. The three designs used different methods of coupling the piezoelectric element to the wall. In the first test the piezoelectric material was bolted using a backing structure. In the second test the piezoelectric was clamped after the application of grease. Finally the piezoelectric element was attached using a conductive epoxy. The mechanical clamp with grease produced the highest measured efficiency of 53% however this design was the least practical from a fabrication viewpoint. The power transfer efficiency of conductive epoxy joint was 40% and the stress bolts (12%). The experimental results on a variety of designs will be presented and the thermal and non-linear issues will be discussed. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Sherrit, S (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. NR 8 TC 8 Z9 8 U1 2 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 0-8194-6224-1 J9 P SOC PHOTO-OPT INS PY 2006 VL 6171 BP 17102 EP 17102 AR 617102 DI 10.1117/12.657736 PG 8 WC Engineering, Multidisciplinary SC Engineering GA BEO53 UT WOS:000238449900002 ER PT S AU Chang, ZS Sherrit, S Badescu, M Bao, XQ Bar-Cohen, Y Backes, P AF Chang, Zensheu Sherrit, Stewart Badescu, Mircea Bao, Xiaoqi Bar-Cohen, Yoseph Backes, Paul BE White, EV Davis, LP TI Reaction force of percussive corer, rotary-friction corer, and rotary-percussive corer - art. no. 617106 SO Smart Structures and Materials 2006: Industrial and Commercial Applications of Smart Structures Technologies SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Smart Structures and Materials 2006 Conference CY FEB 27-MAR 02, 2006 CL San Diego, CA SP SPIE, Amer Soc Mech Engineers, Intelligent Mat Forum, Jet Propuls Lab, Natl Sci Fdn DE Ultrasonic Percussive corer; Rotary-friction corer; Rotary-percussive corer AB Future NASA exploration missions will increasingly require sampling, in-situ analysis and possibly the return of material to Earth for laboratory analysis. To address these objectives, effective and optimized drilling, techniques are needed. This requires developing comprehensive tools to be able to determine analytically what takes place during, the operation and what are the control parameters that can be enhanced. In this study, three types of coring techniques were studied and were identified as potential candidates for operation from a possible future Mars Sample Return (MSR) mission rover. These techniques include percussive, rotary-friction, and rotary-percussive coring. Theoretical models were developed to predict the dynamic reaction forces transmitted from these three types of corers to the robotic arms that hold them. The predicted reaction forces will then be used in a dynamic simulation environment to simulate a representative corer tool to obtain a best estimate of a tool that can be operated from a small rover. The predicted dynamic reaction forces will be presented in this paper. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Chang, ZS (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 4 TC 0 Z9 0 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 0-8194-6224-1 J9 P SOC PHOTO-OPT INS PY 2006 VL 6171 BP 17106 EP 17106 AR 617106 DI 10.1117/12.658075 PG 8 WC Engineering, Multidisciplinary SC Engineering GA BEO53 UT WOS:000238449900006 ER PT S AU Badescu, M Sherrit, S Olorunsola, A Aldrich, J Bao, X Bar-Cohen, Y Chang, Z Doran, PT Fritsen, CH Kenig, F Mckay, CP Murray, A Du, S Peterson, T Song, T AF Badescu, M. Sherrit, S. Olorunsola, A. Aldrich, J. Bao, X. Bar-Cohen, Y. Chang, Z. Doran, P. T. Fritsen, C. H. Kenig, F. Mckay, C. P. Murray, A. Du, S. Peterson, T. Song, T. BE White, EV Davis, LP TI Ultrasonic/sonic Gopher for subsurface ice and brine sampling: Analysis and fabrication challenges, and testing results - art. no. 617107 SO Smart Structures and Materials 2006: Industrial and Commercial Applications of Smart Structures Technologies SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Smart Structures and Materials 2006 Conference CY FEB 27-MAR 02, 2006 CL San Diego, CA SP SPIE, Amer Soc Mech Engineers, Intelligent Mat Forum, Jet Propuls Lab, Natl Sci Fdn DE planetary sampling; ice drilling; ultrasonic horn; ultrasonic drilling; piezoelectric devices AB Rock, soil, and ice penetration by coring, drilling or abrading is of great importance to a large number of space and earth applications. Proven techniques to sample Mars subsurface will be critical for future NASA astrobiology missions that will search for records of past and present life on the planet. An Ultrasonic/Sonic Drill/Corer (USDC) has been developed as an adaptable tool for many of these applications [Bar-Cohen et al., 2001]. The USDC uses a novel drive mechanism to transform the ultrasonic or sonic vibrations of the tip of a horn into a sonic hammering of a drill bit through an intermediate free-flying mass. The USDC design was modified to fabricate an Ultrasonic/Sonic Ice Gopher that is designed to core down to meters depth for in situ analysis and sample collection. This technology was demonstrated at Lake Vida in the Dry Valleys, Antarctica. Coring ice at -20 degrees C as in Lake Vida has been a challenge and efforts were made to develop the required ice core cutting, ice chip handling and potential ice melting (and refreezing) during drilling. The analysis and fabrication challenges and testing results are presented in this paper. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Badescu, M (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 67-119, Pasadena, CA 91109 USA. OI Kenig, Fabien/0000-0003-4868-5232 NR 6 TC 0 Z9 0 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 0-8194-6224-1 J9 P SOC PHOTO-OPT INS PY 2006 VL 6171 BP 17107 EP 17107 AR 617107 DI 10.1117/12.657487 PG 9 WC Engineering, Multidisciplinary SC Engineering GA BEO53 UT WOS:000238449900007 ER PT S AU Bao, X Bar-Cohen, Y Chang, Z Sherrit, S Badescu, M Du, S Song, T Peterson, T AF Bao, X. Bar-Cohen, Y. Chang, Z. Sherrit, S. Badescu, M. Du, S. Song, T. Peterson, T. BE White, EV Davis, LP TI USDC based rapid penetrator of packed soil - art. no. 617108 SO Smart Structures and Materials 2006: Industrial and Commercial Applications of Smart Structures Technologies SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Smart Structures and Materials 2006 Conference CY FEB 27-MAR 02, 2006 CL San Diego, CA SP SPIE, Amer Soc Mech Engineers, Intelligent Mat Forum, Jet Propuls Lab, Natl Sci Fdn DE ultrasonic/sonic; soil penetration; chemical detect; embedded container AB Environment protection requires more testing and analysis tools. To detect buried chemical containers or other objects embedded in soil and avoid possible damage to them, a penetrator was developed for packed soil that requires low penetration force (the force needed to push rod probe into the soil). The design was based on the novel mechanism used by the ultrasonic/sonic driller/corer (USDC) that was developed jointly by scientists at the NDEAA lab at JPL and engineers at Cybersonics, Inc. [Bar-Cohen et al 2001, Bao et al 2003]. In the penetrator, a small free-flying mass is energized by a piezoelectric transducer and impacts a rod probe on its shoulder at frequencies of several hundred Hetz. The impacts help the probe to penetrate the packed soil with low pushing force. A large reduction of the penetration force was achieved. Preliminary tests show that the effects of the penetrator on plastic containers and other objectors are minimal. The details of the design of the prototype penetrator and the results of performance tests are presented. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Bao, X (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 4 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 0-8194-6224-1 J9 P SOC PHOTO-OPT INS PY 2006 VL 6171 BP 17108 EP 17108 AR 617108 DI 10.1117/12.658630 PG 6 WC Engineering, Multidisciplinary SC Engineering GA BEO53 UT WOS:000238449900008 ER PT S AU Aldrich, J Sherrit, S Bao, XQ Bar-Cohen, Y Badescu, M Chang, ZS AF Aldrich, Jack Sherrit, Stewart Bao, Xiaoqi Bar-Cohen, Yoseph Badescu, Mircea Chang, Zensheu BE Lindner, DK TI Extremum-seeking control for an Ultrasonic/Sonic Driller/Corer (USDC) driven at high-power SO SMART STRUCTURES AND MATERIALS 2006: MODELING, SIGNAL PROCESSING, AND CONTROL SE Proceedings of SPIE LA English DT Proceedings Paper CT Smart Structures and Materials 2006 Conference CY FEB 27-MAR 02, 2006 CL San Diego, CA SP SPIE, Amer Soc Mech Engineers, Intelligent Mat Forum, Jet Propuls Lab, Natl Sci Fdn DE high-power piezoelectric actuator; Ultrasonic/Sonic Driller/Corer; peek-seeking estimation and control AB Future NASA exploration missions will increasingly require sampling, in-situ analysis and possibly the return of material to Earth for further tests. One of the challenges to addressing this need is the ability to drill using minimal reaction force and torque while operating from light weight platforms (e.g., lander, rover, etc.) as well as operate at planets with low gravity., For this purpose, the authors developed the Ultrasonic/Sonic Driller/Corer (USDC) jointly with Cybersonics Inc. Studies of the operation of the USDC at high power have shown there is a critical need to selftune to maintain the operation of the piezoelectric actuator at resonance. Performing such tuning is encountered with difficulties and to address them an extremum-seeking control algorithm is being investigated. This algorithm is designed to tune the driving frequency of a time-varying resonating actuator subjected to both random and high-power impulsive noise disturbances. Using this algorithm, the performance of the actuator is monitored on a time-scale that is compatible with its slowly time-varying physical characteristics. The algorithm includes a parameter estimator, which estimates the coefficients of a function that characterizes the quality factor of the USDC. Since the parameter estimator converges sufficiently faster than the time-varying drift of the USDC's actuator physical parameters, this extremum-seeking estimation and control algorithm potentially allows for use in closed-loop monitoring of the operation of the USDC. Specifically, this system may be programmed to automatically adjust the duty-cycle of the sinusoidal driver signal to monitor the quality factor of the USDC not to fall below a user-defined set-point. Such fault-tolerant functionality is especially important in automated drilling applications where it is essential not to inadvertently drive the piezoelectric ceramic elements of the USDC beyond their operation capability. The details of the algorithm and experimental results are described and discussed in this paper. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Aldrich, J (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM jaldrich@jpl.nasa.gov NR 9 TC 0 Z9 0 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 0-8194-6219-5 J9 PROC SPIE PY 2006 VL 6166 AR 616618 DI 10.1117/12.658872 PG 9 WC Automation & Control Systems; Engineering, Electrical & Electronic; Instruments & Instrumentation; Materials Science, Multidisciplinary SC Automation & Control Systems; Engineering; Instruments & Instrumentation; Materials Science GA BEO48 UT WOS:000238444300034 ER PT S AU Choi, SH Elliott, JR King, GC Lillehei, PT AF Choi, Sang H. Elliott, James R. King, Glen C. Lillehei, Peter T. BE Varadan, VK TI Wireless power technology for application-specific scenarios of High Altitude Airships - art. no. 61721D SO Smart Structures and Materials 2006: Smart Electronics, Mems, Biomems, and Nanotechnology SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Smart Structures and Materials 2006 Conference CY FEB 27-MAR 02, 2006 CL San Diego, CA SP SPIE, Amer Soc Mech Engineers, Intelligent Mat Forum, Jet Propuls Lab, Natl Sci Fdn ID MICROWAVE AB A new power concept has been contemplated for High Altitude Airship (HAA) under the consideration of direct energy conversion cycles, such as photovoltaic (PV) cells and advanced thermoelectric (ATE) generator. The HAA has various potential applications and mission scenarios that require onboard energy harvesting and power distribution systems. Both PV cells and an ATE system were briefly compared to identify the advantages of ATE for HAA applications in this study. Utilizing the estimated high efficiency of a three-staged ATE in a tandem mode, the ATE generates a higher quantity of harvested energy than PV cells for mission scenarios. The ATE's performance figure of merit of 5 was considered to estimate the cascaded efficiency of a three-staged ATE system. The estimated efficiency of a tandem system appears to be 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 14 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 0-8194-6225-X J9 P SOC PHOTO-OPT INS PY 2006 VL 6172 BP D1721 EP D1721 AR 61721D DI 10.1117/12.657130 PG 8 WC Engineering, Electrical & Electronic; Nanoscience & Nanotechnology; Telecommunications SC Engineering; Science & Technology - Other Topics; Telecommunications GA BEO54 UT WOS:000238450100042 ER PT S AU Sokolowski, W Ghaffarian, R AF Sokolowski, Witold Ghaffarian, Reza BE Inaudi, D Ecke, W Culshaw, B Peters, KJ Udd, E TI Surface control of cold hibernated elastic memory self-deployable structure - art. no. 61670Y SO Smart Structures and Materials 2006: Smart Sensor Monitoring Systems and Applications SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Smart Structures and Materials 2006 Conference CY FEB 27-MAR 02, 2006 CL San Diego, CA SP SPIE, Amer Soc Mech Engineers, Intelligent Mat Forum, Jet Propuls Lab, Natl Sci Fdn DE shape memory polymers; open cellular structures; glass transition temperature Tg; piezoelectric actuator AB A new class of simple, reliable, lightweight, low packaging volume and cost, self-deployable structures has been developed for use in space and commercial applications. This technology called "cold hibernated elastic memory" (CHEM) utilizes shape memory polymers (SMP) in open cellular (foam) structure or sandwich structures made of shape memory polymer foam cores and polymeric composite skins. Some of many potential CHEM space applications require a high precision deployment and surface accuracy during operation. However, a CHEM structure could be slightly distorted by the thermo-mechanical processing as well as by thermal space environment. Therefore, the sensor system is desirable to monitor and correct the potential surface imperfection. During these studies, the surface control of CHEM smart structures was demonstrated using a Macro-Fiber Composite (MFC) actuator developed by the NASA LaRC and US Army ARL. The test results indicate that the MFC actuator performed well before and after processing cycles. It reduced some residue compressive strain that in turn corrected very small shape distortion after each processing cycle. The integrated precision strain gages were detecting only a small flat shape imperfection indicating a good recoverability of original shape of the CHEM test structure. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Sokolowski, W (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 9 TC 3 Z9 3 U1 1 U2 9 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6220-9 J9 P SOC PHOTO-OPT INS PY 2006 VL 6167 BP Y1670 EP Y1670 AR 61670Y DI 10.1117/12.657485 PG 12 WC Instruments & Instrumentation; Materials Science, Multidisciplinary; Optics SC Instruments & Instrumentation; Materials Science; Optics GA BEO49 UT WOS:000238445300026 ER PT S AU Turner, TL Cabell, RH Cano, RJ Fleming, GA AF Turner, Travis L. Cabell, Randolph H. Cano, Roberto J. Fleming, Gary A. BE Matsuzaki, Y TI Design, fabrication, and testing of a SMA hybrid composite jet engine chevron - art. no. 61731B SO Smart Structures and Materials 2006: Smart Structures and Integrated Systems SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Smart Structures and Materials 2006 Conference CY FEB 27-MAR 02, 2006 CL San Diego, CA SP SPIE, Amer Soc Mech Engineers, Intelligent Mat Forum, Jet Propuls Lab, Natl Sci Fdn DE shape memory alloys; Nitinol; embedded actuators; jet engine chevrons; active chevrons; shape control; deflection control; jet noise control; flow effectors; flow control ID SHAPE CONTROL; ACTUATION; BEAMS AB Control of jet noise continues to be an important research topic. Exhaust nozzle chevrons have been shown to reduce jet noise, but parametric effects are not well understood. Additionally, thrust loss due to chevrons at cruise suggests significant benefit from deployable chevrons. The focus of this study is development of an active chevron concept for the primary purpose of parametric studies for jet noise reduction in the laboratory and technology development to leverage for full scale systems. The active chevron concept employed in this work consists of a laminated composite structure with embedded shape memory alloy (SMA) actuators, termed a SMA hybrid composite (SMAHC). The actuators are embedded on one side of the middle surface such that thermal excitation generates a moment and deflects the structure. A brief description of the chevron design is given followed by details of the fabrication approach. Results from bench top tests are presented and correlated with numerical predictions from a model for such structures that was recently implemented in MSC.Nastran and ABAQUS. Excellent performance and agreement with predictions is demonstrated. Results from tests in a representative flow environment are also presented. Excellent performance is again achieved for both open- and closed-loop tests, the latter demonstrating control to a specified immersion into the flow. The actuation authority and immersion performance is shown to be relatively insensitive to nozzle pressure ratio (NPR). Very repeatable immersion control with modest power requirements is demonstrated. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Turner, TL (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. NR 29 TC 0 Z9 0 U1 2 U2 3 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6226-8 J9 P SOC PHOTO-OPT INS PY 2006 VL 6173 BP B1731 EP B1731 AR 61731B DI 10.1117/12.660844 PG 15 WC Automation & Control Systems; Instruments & Instrumentation; Materials Science, Multidisciplinary SC Automation & Control Systems; Instruments & Instrumentation; Materials Science GA BEO55 UT WOS:000238450200039 ER PT S AU Hale, K Flatau, A AF Hale, Kathleen Flatau, Alison BE Matsuzaki, Y TI Galfenol tactile sensor array and visual mapping system - art. no. 61730Y SO Smart Structures and Materials 2006: Smart Structures and Integrated Systems SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Smart Structures and Materials 2006 Conference CY FEB 27-MAR 02, 2006 CL San Diego, CA SP SPIE, Amer Soc Mech Engineers, Intelligent Mat Forum, Jet Propuls Lab, Natl Sci Fdn AB The smart material, Galfenol, is being explored for its uses as a magnetostrictive material. This project seeks to determine if Galfenol can be used as a tactile sensor in a 2-D grid array, magnetic circuit system. When used within a magnetic circuit, Galfenol indicates induced stress and force as a change in flux, due to a change in permeability of the material. The change in flux is detected by Giant MagnetoResistive (GMR) Sensors, which produce a voltage change proportional to the field change. By using Galfenol in an array, this research attempts to create a sensory area. Galfenol is an alloy made of Iron and Gallium. Fe100-xGax, where 15 <= x <= 28, creates a material with useful mechanical and transduction attributes (Clark et al. and Kellogg). Galfenol is also distinguished by the crystalline structure of the material. Two types currently exist: single crystal and polycrystalline. Single crystal has higher transduction coefficients than polycrystalline, but is more costly. Polycrystalline Galfenol is currently available as either production or research grade. The designations are related to the sample growth rate with the slower rate being the research grade. The slower growth rate more closely resembles the single crystal Galfenol properties. Galfenol 17.5-18% research grade is used for this experiment, provided by Etrema Products Inc. The magnetic circuit and sensor array is first built at the macro scale so that the design can be verified. After the macro scale is proven, further development will move the system to the nano-level. Recent advances in nanofabrication have enabled Galfenol to be grown as nanowires. Using the nanowires, research will seek to create high resolution tactile sensors with spatial resolutions similar to human finger tips, but with greater force ranges and sensitivity capabilities (Flatau & Stadler). Possible uses of such systems include robotics and prosthetics. C1 NASA, Goddard Space Flight Ctr, Washington, DC 20546 USA. RP Hale, K (reprint author), NASA, Goddard Space Flight Ctr, 300 E St SW, Washington, DC 20546 USA. RI Craft, Kathleen/C-2067-2016 OI Craft, Kathleen/0000-0001-7313-3187 NR 4 TC 0 Z9 0 U1 1 U2 3 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6226-8 J9 P SOC PHOTO-OPT INS PY 2006 VL 6173 BP Y1730 EP Y1730 AR 61730Y DI 10.1117/12.660132 PG 12 WC Automation & Control Systems; Instruments & Instrumentation; Materials Science, Multidisciplinary SC Automation & Control Systems; Instruments & Instrumentation; Materials Science GA BEO55 UT WOS:000238450200028 ER PT B AU Clare, L Clement, B Gao, J Hutcherson, J Jennings, E AF Clare, L. Clement, B. Gao, J. Hutcherson, J. Jennings, E. GP IEEE Computer Society TI Space-based networking technology developments in the interplanetary network directorate information technology program SO SMC-IT 2006: 2ND IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 2nd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 17-20, 2006 CL Pasadena, CA SP IEEE Comp Soc, TCCX, Task Force Autonom & Autonomous Syst, Jet Propuls Lab, Calif Inst Technol AB We present advanced technology developments in space networking achieved under the Interplanetary Network Directorate Information Technology Program. Progress has been made in three primary areas: (1) distributed on-board scheduling, as it applies to communications, (2) middleware services, and (3) communications protocols. Demonstrations of these capabilities have been provided using a simulation environment capable of providing a realistic representation of the underlying space communications network environment. C1 [Clare, L.; Clement, B.; Gao, J.; Hutcherson, J.; Jennings, E.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Clare, L (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Loren.P.Clare@jpl.nasa.gov; Bradley.J.Clement@jpl.nasa.gov; Jay.L.Gao@jpl.nasa.gov; Joseph.O.Hutcherson@jpl.nasa.gov; Esther.H.Jennings@jpl.nasa.gov 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 0-7695-2644-6 PY 2006 BP 13 EP + PG 2 WC Engineering, Aerospace; Computer Science, Information Systems SC Engineering; Computer Science GA BEW90 UT WOS:000239914200001 ER PT B AU Pedersen, L Brummett, R AF Pedersen, Liam Brummett, Robert GP IEEE Computer Society TI Collaborative Decision Systems project summary of technology developments for human-robotics interactions SO SMC-IT 2006: 2ND IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 2nd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 17-20, 2006 CL Pasadena, CA SP IEEE Comp Soc, TCCX, Task Force Autonom & Autonomous Syst, Jet Propuls Lab, Calif Inst Technol C1 [Pedersen, Liam; Brummett, Robert] NASA, Ames Res Ctr, Intelligent Syst Div, MS 269-1, Moffett Field, CA 94035 USA. RP Pedersen, L (reprint author), NASA, Ames Res Ctr, Intelligent Syst Div, MS 269-1, Moffett Field, CA 94035 USA. EM robert.c.brummett@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 0-7695-2644-6 PY 2006 BP 47 EP + PG 2 WC Engineering, Aerospace; Computer Science, Information Systems SC Engineering; Computer Science GA BEW90 UT WOS:000239914200006 ER PT B AU Biswas, R Kwak, D Kiris, C Lawrence, S AF Biswas, Rupak Kwak, Dochan Kiris, Cetin Lawrence, Scott GP IEEE Computer Society TI Impact of the Columbia supercomputer on NASA space and exploration missions SO SMC-IT 2006: 2ND IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 2nd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 17-20, 2006 CL Pasadena, CA SP IEEE Comp Soc, TCCX, Task Force Autonom & Autonomous Syst, Jet Propuls Lab, Calif Inst Technol AB NASA's 10,240-processor Columbia supercomputer gained worldwide recognition in 2004 for increasing the space agency's computing capability ten-fold, and enabling U.S. scientists and engineers to perform significant, breakthrough simulations. Columbia has amply demonstrated its capability to accelerate NASA's key missions in space operations, exploration systems, science, and aeronautics. Columbia is part of an integrated high-end computing (HEC) environment comprised of massive storage and archive systems, highspeed networking, high-fidelity modelin; and simulation tools, application performance optimization, and advanced data analysis and visualization. In this paper, we illustrate the impact Columbia is having on NASA's numerous space and exploration applications, such as the development of the Crew Exploration and Launch Vehicles (CEV/CLJ), effects of long-duration human presence in space, and damage assessment and repair recommendations for remaining shuttle flights. We conclude by discussing HEC challenges that must be overcome to solve space-related science problems in the future. C1 [Biswas, Rupak; Kwak, Dochan; Kiris, Cetin] NASA, Ames Res Ctr, Adv Supercomp Div, Moffett Field, CA 94035 USA. [Lawrence, Scott] NASA, Ames Res Ctr, Syst Anal & Integrat Branch, Moffett Field, CA USA. RP Biswas, R (reprint author), NASA, Ames Res Ctr, Adv Supercomp Div, Moffett Field, CA 94035 USA. EM Rupak.Biswas@nasa.gov; Dochan.Kwak@nasa.gov; Cetin.C.Kiris@nasa.gov; Scott.L.Lawrence@nasa.gov 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 0-7695-2644-6 PY 2006 BP 51 EP + PG 2 WC Engineering, Aerospace; Computer Science, Information Systems SC Engineering; Computer Science GA BEW90 UT WOS:000239914200007 ER PT B AU Sterritt, R Hinchey, M Rouff, C Rash, J Truszkowski, W AF Sterritt, Roy Hinchey, Mike Rouff, Christopher Rash, James Truszkowski, Walt GP IEEE Computer Society TI Sustainable and autonomic Space Exploration Missions SO SMC-IT 2006: 2ND IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 2nd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 17-20, 2006 CL Pasadena, CA SP IEEE Comp Soc, TCCX, Task Force Autonom & Autonomous Syst, Jet Propuls Lab, Calif Inst Technol ID SYSTEMS AB Visions for future space exploration have long term science missions in sight, resulting in the need for sustainable missions. Survivability is a critical property of sustainable systems and may be addressed through autonomicity, an emerging paradigm for self-management of future computer-based systems based on inspiration from the human autonomic nervous system. This paper examines some of the ongoing research efforts to realize these survivable systems visions, with specific emphasis on developments in Autonomic Policies. C1 [Sterritt, Roy] Univ Ulster, Coleraine BT52 1SA, Londonderry, North Ireland. [Hinchey, Mike; Rash, James; Truszkowski, Walt] NASA GSFC, Greenbelt, MD USA. [Rouff, Christopher] SAIC ACBU, Mclean, VA USA. RP Sterritt, R (reprint author), Univ Ulster, Coleraine BT52 1SA, Londonderry, North Ireland. EM r.sterritt@ulster.ac.uk; michael.g.hinchey@nasa.gov; rouffc@saic.com; james.l.rash@nasa.gov; walter.f.truszkowski@nasa.gov FU NASA Office of Systems and Mission Assurance (OSMA) through its Software Assurance Research Program (SARP); Formal Approaches to Swarm Technologies (FAST); NASA Software Engineering Laboratory; Goddard Space Flight Center; Computer Science Research Institute (CSRI); Centre for Software Process Technologies (CSPT); Invest NI through the Centres of Excellence Programme under EU 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, under the EU Peace II initiative. NR 35 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 0-7695-2644-6 PY 2006 BP 59 EP + PG 3 WC Engineering, Aerospace; Computer Science, Information Systems SC Engineering; Computer Science GA BEW90 UT WOS:000239914200008 ER PT B AU Diaconescu, RE Zima, HP AF Diaconescu, Roxana E. Zima, Hans P. GP IEEE Computer Society TI User-defined data distributions in high-level programming languages SO SMC-IT 2006: 2ND IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 2nd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 17-20, 2006 CL Pasadena, CA SP IEEE Comp Soc, TCCX, Task Force Autonom & Autonomous Syst, Jet Propuls Lab, Calif Inst Technol AB One of the characteristic features of today's high performance computing systems is a physically distributed memory. Efficient management of locality is essential for meeting key performance requirements for these architectures. The standard technique for dealing with this issue has involved the extension of traditional sequential programming languages with explicit message passing, in the context of a processor-centric view of parallel computation. This has resulted in complex and error-prone assembly-style codes in which algorithms and communication are inextricably interwoven. This paper presents a high-level approach to the design and implementation of data distributions. Our work is motivated by the need to improve the current parallel programming methodology by introducing a paradigm supporting the development of efficient and reusable parallel code. This approach is currently being implemented in the context of a new programming language called Chapel, which is designed in the HPCS project Cascade. C1 [Diaconescu, Roxana E.] CALTECH, Ctr Adv Comp Res, Pasadena, CA 91125 USA. [Zima, Hans P.] Jet Prop Lab, California Inst Technol, Pasadena, CA USA. RP Diaconescu, RE (reprint author), CALTECH, Ctr Adv Comp Res, Pasadena, CA 91125 USA. EM roxana@caltech.edu; zima@jpl.nasa.gov FU Defense Advanced Research Projects Agency [NBCH3039003] FX This paper is based upon work supported by the Defense Advanced Research Projects Agency under its Contract No. NBCH3039003. The research described in this paper was partially carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National .Aeronautics and Space Administration NR 24 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 0-7695-2644-6 PY 2006 BP 67 EP + PG 3 WC Engineering, Aerospace; Computer Science, Information Systems SC Engineering; Computer Science GA BEW90 UT WOS:000239914200009 ER PT B AU Indictor, MB Dvorak, DL Ingham, MD Hutcherson, JO Torres, RJ Wax, AH AF Indictor, Mark B. Dvorak, Daniel L. Ingham, Michel D. Hutcherson, Joseph O. Torres, Recaredo J. Wax, Allan H. GP IEEE Computer Society TI A software development approach to implementing control systems specified through state analysis SO SMC-IT 2006: 2ND IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 2nd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 17-20, 2006 CL Pasadena, CA SP IEEE Comp Soc, TCCX, Task Force Autonom & Autonomous Syst, Jet Propuls Lab, Calif Inst Technol C1 [Indictor, Mark B.; Dvorak, Daniel L.; Ingham, Michel D.; Hutcherson, Joseph O.; Torres, Recaredo J.; Wax, Allan H.] CALTECH, Jet Prop Lab, Syst & Software Div, Pasadena, CA USA. RP Indictor, MB (reprint author), CALTECH, Jet Prop Lab, Syst & Software Div, Pasadena, CA USA. EM mark.b.indicator@jpl.nasa.gov; daniel.l.dvorak@jpl.nasa.gov; michel.d.ingham@jpl.nasa.gov; joseph.o.hutcheson@jpl.nasa.gov; recaredo.j.torres@jpl.nasa.gov; allan.h.wax@jpl.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 0-7695-2644-6 PY 2006 BP 79 EP 79 PG 1 WC Engineering, Aerospace; Computer Science, Information Systems SC Engineering; Computer Science GA BEW90 UT WOS:000239914200010 ER PT B AU Horvath, G Ingham, M Chung, S Martin, O Williams, B AF Horvath, Gregory Ingham, Michel Chung, Seung Martin, Oliver Williams, Brian GP IEEE Computer Society TI Practical application of model-based programming and state-based architecture to space missions SO SMC-IT 2006: 2ND IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 2nd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 17-20, 2006 CL Pasadena, CA SP IEEE Comp Soc, TCCX, Task Force Autonom & Autonomous Syst, Jet Propuls Lab, Calif Inst Technol AB Innovative systems and software engineering solutions are required to meet the increasingly challenging demands of deep-space robotic missions. While recent advances in the development of integrated systems and software engineering approaches have begun to address some of these issues, these methods are still at the core highly manual and, therefore, error-prone. This paper describes a task aimed at infusing MIT's model-based executive, Titan, into JPL's Mission Data System (MDS), a unified state-based architecture, systems engineering process, and supporting software framework. Results of the task are presented, including a discussion of the benefits and challenges associated with integrating mature model-based programming techniques and technologies into a rigorously-defined domain specific architecture. C1 [Horvath, Gregory; Ingham, Michel] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Chung, Seung; Martin, Oliver; Williams, Brian] CSAIL, MIT, Cambridge, MA USA. RP Horvath, G (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM gregory.horvath@jpl.nasa.gov; michel.ingham@jpl.nasa.gov; chung@mit.edu; omartin@mit.edu; williams@mit.edu 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 0-7695-2644-6 PY 2006 BP 80 EP + PG 2 WC Engineering, Aerospace; Computer Science, Information Systems SC Engineering; Computer Science GA BEW90 UT WOS:000239914200011 ER PT B AU Pressburger, T Feather, MS Hinchey, M Markosian, L AF Pressburger, Thomas Feather, Martin S. Hinchey, Michael Markosian, Lawrence GP IEEE Computer Society TI Infusing software engineering technology into practice at NASA SO SMC-IT 2006: 2ND IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 2nd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 17-20, 2006 CL Pasadena, CA SP IEEE Comp Soc, TCCX, Task Force Autonom & Autonomous Syst, Jet Propuls Lab, Calif Inst Technol AB We present an ongoing effort of the NASA Software Engineering Initiative to encourage the use of advanced software engineering technology on NASA projects. Technology infusion is in general a difficult process yet this effort seems to have found a modest approach that is successful for some types of technologies. We outline the process and describe the experience of the technology infusions that occurred over a two year period We also present some lessons from the experiences. C1 [Pressburger, Thomas] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Feather, Martin S.] Jet Prop Lab, California Inst Technol, Pasadena, CA USA. [Hinchey, Michael] NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. [Markosian, Lawrence] NASA, QSS Grp, Ames Res Ctr, Moffett Field, CA USA. RP Pressburger, T (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM Tom.Pressburger@nasa.gov; Michael.G.Hinchey@jpl.nasa.gov; Martin.S.Feather@nasa.gov; lzmarkosian@email.arc.nasa.gov NR 2 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 0-7695-2644-6 PY 2006 BP 89 EP + PG 2 WC Engineering, Aerospace; Computer Science, Information Systems SC Engineering; Computer Science GA BEW90 UT WOS:000239914200012 ER PT B AU Chowdhury, PK Atiquzzaman, M Ivancic, W AF Chowdhury, Pulak K. Atiquzzaman, Mohammed Ivancic, William GP IEEE Computer Society TI Handover schemes in space networks: Classification and performance comparison SO SMC-IT 2006: 2ND IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 2nd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 17-20, 2006 CL Pasadena, CA SP IEEE Comp Soc, TCCX, Task Force Autonom & Autonomous Syst, Jet Propuls Lab, Calif Inst Technol ID LEO SATELLITE NETWORKS; MANAGEMENT; SYSTEMS AB Third Generation (3G) communication networks based on Low Earth Orbit (LEO) satellites provide a new trend in future mobile communications. LEO satellites provide lower end-to-end delays and efficient frequency spectrum utilization, making it suitable for Personal Communication Services (PCS). However ongoing communications using LEO satellite systems experience frequent handover due to high rotational speed of satellites. In this paper, we provide a comprehensive literature survey on proposed handover schemes for LEO satellite systems. We also present a detailed classification of handover schemes in the literature. Finally, we compare the handover schemes using different Quality of Service. C1 [Chowdhury, Pulak K.; Atiquzzaman, Mohammed] Univ Oklahoma, Sch Comp Sci, Norman, OK 73019 USA. [Ivancic, William] NASA, Satellite Networks & Architectures Branch, Glenn Res Ctr, Cleveland, OH 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 17 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 0-7695-2644-6 PY 2006 BP 101 EP + PG 2 WC Engineering, Aerospace; Computer Science, Information Systems SC Engineering; Computer Science GA BEW90 UT WOS:000239914200013 ER PT B AU Chowdhury, PK Atiquzzaman, M Ivancic, W AF Chowdhury, Pulak K. Atiquzzaman, Mohammed Ivancic, William GP IEEE Computer Society TI SINEMO: An IP-diversity based approach for Network Mobility in space SO SMC-IT 2006: 2ND IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 2nd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 17-20, 2006 CL Pasadena, CA SP IEEE Comp Soc, TCCX, Task Force Autonom & Autonomous Syst, Jet Propuls Lab, Calif Inst Technol ID PERFORMANCE; SIGMA AB IETF proposed Network Mobility (NEMO) Basic Support Protocol (BSP) to support network mobility. NEMO BSP is an extension of Mobile IP v6 (MIPv6), and inherits all the drawbacks of MIPv6 (like inefficient routing, high handover latency and packet loss rate). Satellites equipped with several IP-enabled devices is an example of network mobility in space networks. In this paper, we propose an IP-diversity based network mobility architecture called SINEMO, and show that SINEMO can exhibit better performance than NEMO BSP in satellite IP networks. C1 [Atiquzzaman, Mohammed] Univ Oklahoma, Sch Comp Sci, Norman, OK 73019 USA. [Ivancic, William] NASA, Satellite Networks & Architectures Branch, Glenn Res ctr, Cleveland, OH 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 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 0-7695-2644-6 PY 2006 BP 109 EP + PG 2 WC Engineering, Aerospace; Computer Science, Information Systems SC Engineering; Computer Science GA BEW90 UT WOS:000239914200014 ER PT B AU Pang, J Pingree, PJ Torgerson, JL AF Pang, Jackson Pingree, Paula J. Torgerson, J. Leigh GP IEEE Computer Society TI TRIGA: Telecommunications protocol processing subsystem using Reconfigurable Interoperable Gate Arrays SO SMC-IT 2006: 2ND IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 2nd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 17-20, 2006 CL Pasadena, CA SP IEEE Comp Soc, TCCX, Task Force Autonom & Autonomous Syst, Jet Propuls Lab, Calif Inst Technol AB We present the Telecommunications protocol processing subsystem using Reconfigurable Interoperable Gate Arrays (TRIGA), a novel approach that unifies fault tolerance and inter-planetary communication protocol offloading to implement CCSDS File Delivery Protocol and Datalink layers. The new reconfigurable architecture offers more than one order of magnitude throughput increase while reducing footprint requirements in memory, command and data handling processor utilization, communication system interconnects and power consumption. C1 [Pang, Jackson; Pingree, Paula J.; Torgerson, J. Leigh] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Pang, J (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM Jackson.Pang@jpl.nasa.gov; Paula.J.Pingree@jpl.nasa.gov; Jordan.L.Torgerson@jpl.nasa.gov NR 17 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 0-7695-2644-6 PY 2006 BP 116 EP + PG 3 WC Engineering, Aerospace; Computer Science, Information Systems SC Engineering; Computer Science GA BEW90 UT WOS:000239914200015 ER PT B AU Hancher, MD Hornby, GS AF Hancher, Matthew D. Hornby, Gregory S. GP IEEE Computer Society TI A modular robotic system with applications to space exploration SO SMC-IT 2006: 2ND IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 2nd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 17-20, 2006 CL Pasadena, CA SP IEEE Comp Soc, TCCX, Task Force Autonom & Autonomous Syst, Jet Propuls Lab, Calif Inst Technol AB Modular robotic systems offer potential advantages as versatile, fault-tolerant, cost-effective platforms for space exploration, but a sufficiently mature system is not yet available. We describe the possible applications of such a System, and present prototype hardware intended as a step in the right direction. We also present elements of an automated design and optimization framework aimed at making modular robots easier to design and use, and discuss the results of applying the system to a gait optimization problem. Finally, we discuss the potential near-term applications of modular robotics to terrestrial robotics research. C1 [Hancher, Matthew D.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Hornby, Gregory S.] Univ Calif Santa Cruz, Moffett Field, CA USA. RP Hancher, MD (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM mdh@email.arc.nasa.gov; hornby@email.arc.nasa.gov NR 19 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 0-7695-2644-6 PY 2006 BP 125 EP + PG 2 WC Engineering, Aerospace; Computer Science, Information Systems SC Engineering; Computer Science GA BEW90 UT WOS:000239914200016 ER PT B AU Johnston, MD Rabe, KJ AF Johnston, Mark D. Rabe, Kenneth J. GP IEEE Computer Society TI Integrated planning for telepresence with time delays SO SMC-IT 2006: 2ND IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 2nd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 17-20, 2006 CL Pasadena, CA SP IEEE Comp Soc, TCCX, Task Force Autonom & Autonomous Syst, Jet Propuls Lab, Calif Inst Technol ID SPACE AB Teleoperation of remote robotic systems over time delays in the range of 2-10 seconds poses a unique set of challenges. In the context of a supervisory control system for the JSC Robonaut humanoid robot, we have developed an "intelligent assistant" that integrates an Artificial Intelligence planner (JSHOP2) with execution monitoring of the state of both the human supervisor and the remote robot. The assistant reasons simultaneously about the world state on both sides of the time delay, which represents a novel application of this technology. The purpose of the assistant is to provide advice to the human supervisor about current and future activities, derived from a sequence of high-level goals to be achieved. To do this, the assistant must simultaneously monitor and react to various data sources, including actions taken by the supervisor who is issuing commands to the robot (e.g. with a data glove), actions taken by the robot, and the environment of the robot, both as currently perceived over the time delay, along with the current sequence of goals. We have developed a "leader/follower" software architecture to handle the dual time-shifted streams of execution feedback. In this paper we describe the integrated planner and its executive, and how it operates in normal and anomaly situations. C1 [Johnston, Mark D.; Rabe, Kenneth J.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Johnston, MD (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM mark.d.johnston@jpl.nasa.gov; kenneth.rabe@jpl.nasa.gov NR 11 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 0-7695-2644-6 PY 2006 BP 140 EP + PG 2 WC Engineering, Aerospace; Computer Science, Information Systems SC Engineering; Computer Science GA BEW90 UT WOS:000239914200018 ER PT B AU Jain, A Cameron, J Lim, C Guineau, J AF Jain, Abhinandan Cameron, Jonathan Lim, Christopher Guineau, John GP IEEE Computer Society TI SIMSCAPE: Terrain modeling toolkit SO SMC-IT 2006: 2ND IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 2nd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 17-20, 2006 CL Pasadena, CA SP IEEE Comp Soc, TCCX, Task Force Autonom & Autonomous Syst, Jet Propuls Lab, Calif Inst Technol AB Planetary space mission applications involving landers and surface exploration vehicles make extensive use of terrain models within their simulation testbeds. Such terrain models are large, complex and have a variety of attributes including topography, reflectivity, soil mechanics, and hazard information. Sources for the terrain models include planetary data archives, field tests, and analytically constructed models. Simulation uses of such models include surface rover vehicles' kinematics and dynamics models, instrument models, camera models and robotic arm models. This paper describes the SIMSCAPE middleware toolkit for providing a common infrastructure to represent terrain model data from multiple data sources and make them available to simulation applications. SIMSCAPE simplifies the overall simulation design by eliminating the traditional need for custom terrain model interfaces to terrain data sources for simulation users. SIMSCAPE provides a collection of libraries and tools to use and manage terrain environment models within the simulation applications. C1 [Jain, Abhinandan; Cameron, Jonathan; Lim, Christopher; Guineau, John] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Jain, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. FU National Aeronautics and Space Administration; National Science Foundation [ASC 92 19368] FX We would like to thank Meemong Lee and James Wood for their many suggestions during the design and implementation of the S IM S CAPE software and Michael Wagner for the im- plementation of the S IM S CAPE GUI. 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, and has been supported partly by the National Science Foundation Grant ASC 92 19368. NR 2 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 0-7695-2644-6 PY 2006 BP 149 EP + PG 2 WC Engineering, Aerospace; Computer Science, Information Systems SC Engineering; Computer Science GA BEW90 UT WOS:000239914200019 ER PT B AU Jain, A Biesiadecki, J AF Jain, Abhinandan Biesiadecki, Jeffrey GP IEEE Computer Society TI YAM - A framework for rapid software development SO SMC-IT 2006: 2ND IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 2nd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 17-20, 2006 CL Pasadena, CA SP IEEE Comp Soc, TCCX, Task Force Autonom & Autonomous Syst, Jet Propuls Lab, Calif Inst Technol AB YAM is a software development framework with tools for facilitating the rapid development of software in a concurrent software development environment. YAM provides solutions for thorny development challenges associated with software reuse, managing multiple software configurations, developing of software product-lines, and multiple platform development and build management. YAM uses release-early, release-often development cycles to allow developers to incrementally integrate their changes into the system on a continual basis. YAM facilitates the creation and merging of branches to support the isolated development of immature software to avoid impacting the stability of the development effort. YAM uses modules and packages to organize and share software across multiple software products. It uses the concepts of link and work modules to reduce sandbox setup times even when the code-base is large. One side-benefit is the enforcement of a strong module-level encapsulation of a module's functionality and interface. This increases design transparency, system stability as well as software reuse. YAM is in use by several mid-size software development teams including several developing mission-critical software. C1 [Jain, Abhinandan; Biesiadecki, Jeffrey] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Jain, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. FU National Aeronautics and Space Administration; National Science Foundation [ASC 92 19368] FX We would like to thank Garth Watney for the many constructive suggestions that have helped improve Y A M s usability over the years. 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, and has been partly supported by the National Science Foundation Grant ASC 92 19368. NR 1 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 0-7695-2644-6 PY 2006 BP 182 EP + PG 2 WC Engineering, Aerospace; Computer Science, Information Systems SC Engineering; Computer Science GA BEW90 UT WOS:000239914200023 ER PT B AU Lincoln, WP Hua, H Weisbin, CR AF Lincoln, William P. Hua, Hook Weisbin, Charles R. GP IEEE Computer Society TI Temporal investment strategy to enable JPL future space missions SO SMC-IT 2006: 2ND IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 2nd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 17-20, 2006 CL Pasadena, CA SP IEEE Comp Soc, TCCX, Task Force Autonom & Autonomous Syst, Jet Propuls Lab, Calif Inst Technol AB The Jet Propulsion Laboratory (JPL) formulates and conducts deep space missions for NASA (the National Aeronautics and Space Administration). The Chief Technologist of JPL has the responsibility for strategic planning of the laboratory's advanced technology program to assure that the required technological capabilities to enable future JPL deep space missions are ready as needed; as such he is responsible for the development of a Strategic Plan. As part of the planning effort, he has supported the development of a structured approach to technology prioritization based upon the work of the START (Strategic Assessment of Risk and Technology) team. A major innovation reported here is the addition of a temporal model that supports scheduling of technology development as a function of time. The JPL Strategic Technology Plan divides the required capabilities into 13 strategic themes. The results reported here represent the analysis of an initial seven. C1 [Lincoln, William P.; Hua, Hook; Weisbin, Charles R.] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Lincoln, WP (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. EM William.Lincoln@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 0-7695-2644-6 PY 2006 BP 208 EP + PG 2 WC Engineering, Aerospace; Computer Science, Information Systems SC Engineering; Computer Science GA BEW90 UT WOS:000239914200026 ER PT B AU Segui, J Jennings, E AF Segui, John Jennings, Esther GP IEEE Computer Society TI Delay Tolerant Networking - Bundle Protocol simulation SO SMC-IT 2006: 2ND IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 2nd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 17-20, 2006 CL Pasadena, CA SP IEEE Comp Soc, TCCX, Task Force Autonom & Autonomous Syst, Jet Propuls Lab, Calif Inst Technol AB In space exploration missions, the coordinated use of spacecraft as communication relays increases the efficiency of the endeavors. To conduct trade-off studies of the performance and resource usage of different communication protocols and network designs, JPL designed a comprehensive extendable tool, the Multi-mission Advanced Communications Hybrid Environment for Test and Evaluation (MACHETE). The design and development of MACHETE began in 2000 and is constantly evolving. Currently, MACHETE contains Consultative Committee for Space Data Systems (CCSDS) protocol standards such as Proximity-1, Advanced Orbiting Systems (AOS), Packet Telemetry/Telecoinmand Space Communications Protocol Specification (SCPS), and the CCSDS File Delivery Protocol (CFDP). Delay Tolerant Networking (DTN) is an end-to-end network architecture designed to provide communication in and/or through highly stressed networking environments. Stressed networking environments include those with intermittent connectivity, large and/or variable delays, and high bit error rates. The DTN research group (DTNRG) leads the field in DTN research. Members of the DTNRG created the Bundle Protocol (BP) to implement the D77V architecture. The key capabilities of the bundle protocols include custody-based reliability, ability to cope with intermittent connectivity, ability to take advantage of scheduled and opportunistic connectivity, and late binding of names to addresses. In this paper, we report on the addition of MACHETE Bundle Protocol model needed to support DTN research. To illustrate the use of MACHETE with the additional BP model, we provide an example simulation and benchmark its performance. We demonstrate the use of the Bundle Protocol and discuss statistics gathered concerning the total time needed to simulate numerous bundle transmissions. C1 [Segui, John; Jennings, Esther] Jet Propuls Lab, Pasadena, CA 91109 USA. RP Segui, J (reprint author), Jet Propuls Lab, Pasadena, CA 91109 USA. EM John.S.Segui@jpl.nasa.gov; Esther.H.Jennings@jpl.nasa.gov FU National Aeronautics and Space Administration FX The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 10 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 0-7695-2644-6 PY 2006 BP 235 EP + PG 3 WC Engineering, Aerospace; Computer Science, Information Systems SC Engineering; Computer Science GA BEW90 UT WOS:000239914200030 ER PT B AU Esfandiari, M Ramapriyan, H Behnke, J Sofinowski, E AF Esfandiari, M. Ramapriyan, H. Behnke, J. Sofinowski, E. GP IEEE Computer Society TI Evolving a ten year old data system SO SMC-IT 2006: 2ND IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 2nd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 17-20, 2006 CL Pasadena, CA SP IEEE Comp Soc, TCCX, Task Force Autonom & Autonomous Syst, Jet Propuls Lab, Calif Inst Technol AB The Earth Observing System (EOS) Data and Information System (EOSDIS) is a comprehensive distributed system designed to support NASA Is Earth Science missions. Designed in the early 1990's, EOSDIS has been archiving, managing, and distributing Earth science data since 1994. Over the life of EOSDIS an on-going process of technology updates and improvements in user access, distribution mechanisms, and archive management has attempted to keep the system current. However, data volumes have grown rapidly and the science community has gained experience and,capability in processing and analyzing their data The result is a growing desire to re-examine the current operations for gains and improvements in a variety of areas. The objectives of the evolution of EOSDIS are to: increase end-to-end data system efficiency while decreasing operations costs, increase data interoperability and usability by the science research, application, and modeling communities, improve data access and processing, and ensure safe stewardship. C1 [Esfandiari, M.; Ramapriyan, H.; Behnke, J.] NASA, Goddard Space Flight Ctr, Washington, DC 20001 USA. [Sofinowski, E.] SGT Inc, Greenbelt, MD USA. RP Esfandiari, M (reprint author), NASA, Goddard Space Flight Ctr, Washington, DC 20001 USA. EM Mary.A.Esfandiari@nasa.gov FU NASA's Science Mission Directorate; NASA and SGT,Inc [NNG05CA99C] FX This work was performed by the first three authors as part of their duties as U.S. Government employees. It was supported by the NASAs Science Mission Directorate. The fourth author worked as a contractor supporting this effort under contract NNG05CA99C between NASA and SGT, Inc. The opinions expressed are those of the authors and do not necessarily reflect the official position of NASA. NR 4 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 0-7695-2644-6 PY 2006 BP 243 EP + PG 2 WC Engineering, Aerospace; Computer Science, Information Systems SC Engineering; Computer Science GA BEW90 UT WOS:000239914200032 ER PT B AU McCurdy, M Pyrzak, G Ratterman, C Vera, A AF McCurdy, Michael Pyrzak, Guy Ratterman, Christian Vera, Alonso GP IEEE Computer Society TI The design of efficient ground software tools SO SMC-IT 2006: 2ND IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 2nd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 17-20, 2006 CL Pasadena, CA SP IEEE Comp Soc, TCCX, Task Force Autonom & Autonomous Syst, Jet Propuls Lab, Calif Inst Technol C1 [McCurdy, Michael; Vera, Alonso] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Pyrzak, Guy; Ratterman, Christian] San Jose State Univ, San Jose, CA 95192 USA. [Vera, Alonso] Carnegie Mellon Univ, Pittsburgh, PA 15213 USA. RP McCurdy, M (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. 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 0-7695-2644-6 PY 2006 BP 257 EP 257 PG 1 WC Engineering, Aerospace; Computer Science, Information Systems SC Engineering; Computer Science GA BEW90 UT WOS:000239914200034 ER PT B AU Ng, TK Herath, JA AF Ng, Tak-Kwong Herath, Jeffrey A. GP IEEE Computer Society TI Radiation Tolerant Intelligent Memory Stack (RTIMS) SO SMC-IT 2006: 2ND IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 2nd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 17-20, 2006 CL Pasadena, CA SP IEEE Comp Soc, TCCX, Task Force Autonom & Autonomous Syst, Jet Propuls Lab, Calif Inst Technol AB The Radiation Tolerant Intelligent Memory Stack (RTIMS), suitable for both geostationary and low earth orbit missions, has been developed The memory module is fully functional and undergoing environmental and radiation characterization. A self-contained 'flight-like" module is expected to be completed in 2006 RTIMS provides reconfigurable circuitry and 2 gigabits of error corrected or 1 gigabit of triple redundant digital memory in a small package. RTIMS utilizes circuit stacking of heterogeneous components and radiation shielding technologies. A reprogrammable field programmable gate array (FPGA), six synchronous dynamic random access memories, linear regulator, and the radiation mitigation circuitries are stacked into a module of 42.7mm x 42.7mm x 13.00mm. Triple module redundancy, current limiting, configuration scrubbing, and single event function interrupt detection are employed to mitigate radiation effects. The mitigation techniques significantly simplify system design. RTIMS is well suited for deployment in real-time data processing, reconfigurable computing, and memory intensive applications. C1 [Ng, Tak-Kwong; Herath, Jeffrey A.] NASA, Langley Res Ctr, Hampton, VA 23630 USA. RP Ng, TK (reprint author), NASA, Langley Res Ctr, Hampton, VA 23630 USA. EM t.ng@nasa.gov; jeffrey.a.herath@nasa.gov NR 3 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 0-7695-2644-6 PY 2006 BP 270 EP + PG 2 WC Engineering, Aerospace; Computer Science, Information Systems SC Engineering; Computer Science GA BEW90 UT WOS:000239914200037 ER PT B AU Park, HG Barrett, A Baumann, E Grage, M Narasimhan, S AF Park, Han G. Barrett, Anthony Baumann, Erwin Grage, Michael Narasimhan, Sriram GP IEEE Computer Society TI Modular architecture for hybrid diagnostic reasoners SO SMC-IT 2006: 2ND IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 2nd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 17-20, 2006 CL Pasadena, CA SP IEEE Comp Soc, TCCX, Task Force Autonom & Autonomous Syst, Jet Propuls Lab, Calif Inst Technol AB This paper describes technical progress made in maturing ISHM technologies for hybrid diagnostic reasoners under NASA's Exploration Systems Research & Technology (ESR&T) program by Northrop Grumman Corporation and its NASA partners at ARC, GRC, JPL, and JSC A layered architecture was developed that supports both distributed and hierarchical reasoning as well as interoperability and interchangeability of reasoning algorithms. A hybrid reasoner using this: architecture was to be demonstrated performing automated fault detection and isolation in an "Apollo 13"-like failure scenario. C1 [Park, Han G.; Barrett, Anthony] NASA, Ames Res Ctr, Jet Propuls Lab, Moffett Field, CA USA. [Park, Han G.; Baumann, Erwin; Grage, Michael] Northop Grummam Corp, Falls Church, VA USA. [Narasimhan, Sriram] NASA Ames Res Ctr, Ames, IA USA. RP Park, HG (reprint author), NASA, Ames Res Ctr, Jet Propuls Lab, Moffett Field, CA USA. EM Han.Park@ngc.com FU NASAs Exploration Systems Mission Directorate (ESMD) Exploration Systems Research and Technology (ESRT) program FX This project was funded under the NASAs Exploration Systems Mission Directorate (ESMD) Exploration Systems Research and Technology (ESR&T) program. The authors would like to thank Dr. Robert Morris of NASA Ames Research Center for his guidance and support as NASAs Contracting Office Technical Representative (COTR), and Dan Dvorak of JPL for his original discussions on diagnostic reasoning methods. 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 BN 0-7695-2644-6 PY 2006 BP 277 EP + PG 2 WC Engineering, Aerospace; Computer Science, Information Systems SC Engineering; Computer Science GA BEW90 UT WOS:000239914200038 ER PT B AU Shab, T AF Shab, Ted GP IEEE Computer Society TI XBoard: A framework for integrating and enhancing collaborative work practices SO SMC-IT 2006: 2nd IEEE International Conference on Space Mission Challenges for Information Technology, Proceedings LA English DT Proceedings Paper CT 2nd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 17-20, 2006 CL Pasadena, CA SP IEEE Comp Soc, TCCX, Task Force Autonom & Autonomous Syst, Jet Propuls Lab, Calif Inst Technol AB Teams typically collaborate in different modes including face-to-face meetings, meetings that are synchronous (i.e. require parties to participate at the same time) but distributed geographically, and meetings involving asynchronously working on common tasks at different times. The XBoard platform was designed to create an integrated environment for creating applications that enhance collaborative work practices. Specifically, it takes large, touch-screen enabled displays as the starting point for enhancing face-to-face meetings by providing common facilities such as whiteboarding/electronic flipcharts, laptop projection, web access, screen capture and content distribution. These capabilities are built upon by making these functions inherently distributed by allowing these sessions to be easily connected between two or more systems at different locations. Finally, an information repository is integrated into the functionality to provide facilities for work practices that involve work being done at different times, such as reports that span different shifts. The XBoard has been used on the Mars Exploration Rovers mission at JPL, and is currently being used or considered for use in pilot projects at Johnson Space Center (JSC) Mission Control, the University of Arizona Lunar and Planetary Laboratory (Phoenix Mars Lander), and MBARI (Monterey Bay Aquarium Research Institute). C1 NASA, Ames Res Ctr, QSS, Moffett Field, CA USA. RP Shab, T (reprint author), NASA, Ames Res Ctr, QSS, Moffett Field, CA USA. NR 2 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 0-7695-2644-6 PY 2006 BP 285 EP 290 PG 6 WC Engineering, Aerospace; Computer Science, Information Systems SC Engineering; Computer Science GA BEW90 UT WOS:000239914200039 ER PT B AU Orosz, M Kichkaylo, T Balaban, E Goforth, A Sweet, A Neches, R AF Orosz, Michael Kichkaylo, Tatiana Balaban, Edward Goforth, Andre Sweet, Adam Neches, Robert GP IEEE Computer Society TI Tracking logistical constraints across missions and organizations: A multipurpose information infrastructure SO SMC-IT 2006: 2ND IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 2nd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 17-20, 2006 CL Pasadena, CA SP IEEE Comp Soc, TCCX, Task Force Autonom & Autonomous Syst, Jet Propuls Lab, Calif Inst Technol AB The goal of many enterprises is to develop and execute plans and schedules that achieve stated goals while simultaneously minimizing the cost of logistics management and maximizing resource productivity. This goal is a challenge in space flight environments where just-in-time logistics management can't be supported and large scale planning and scheduling requires collaborations and negotiations that cross many divisions and departments. Although there have been many systems proposed and/or developed that address one or more of these concerns, a key element missing in these systems is the tight coupling that is necessary between maintenance, logistics, and operations. This close relationship is particularly important in space operations where changes to scheduled missions and/or the logistics chain can greatly impact overall operations. Based on previous work on combined maintenance and operations planning/scheduling for Marine Aviation, we propose a software-based infrastructure that coordinates planning, scheduling, and execution across multiple departments and disciplines. C1 [Orosz, Michael; Kichkaylo, Tatiana; Neches, Robert] Univ Southern Calif, Inst Informat Sci, 4676 Admiralty Way, Marina Del Rey, CA 90292 USA. [Balaban, Edward; Sweet, Adam] NASA, Ames Res Ctr, QSS Grp Inc, Moffett Field, CA 94035 USA. [Goforth, Andre] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Orosz, M (reprint author), Univ Southern Calif, Inst Informat Sci, 4676 Admiralty Way, Marina Del Rey, CA 90292 USA. FU NASA [NNA05CS29A] FX This research was supported by NASA grant NNA05CS29A. The authors would like to acknowledge the contributions of their CMMD teammates from USC ISI, Vanderbilt University, JSC, and Hamilton Sundstrand who devoted their considerable talents and energy to making this project possible (in alphabetical order): Chris Van Buskirk, Steven Gonzalez, Shashi Gowda, Gabor Karsai, Keith Massei, Himanshu Neema, Sandy Peterson, Carolina Quinteros, and Suzie Shimamoto. The authors would also like to express their gratitude to following individuals affiliated with JSC, Hamilton Sundstrand, and USA for being exceptionally generous with their time and expertise in helping the CMMD team: Melissa Arnold, Frank Birkenseher, Heath Borders, Susan Brandt, Stephen Broussard, Anthony Butina, Wade Frost, Michele Gonzales, David Hughes, Joseph Kitchen, Robert Knight, David Korth, Kenneth Kruse, Troy LeBlanc, Kathleen Leary, Chris Looper, Robert McCormick, Patricia Meyer, Blair Nader, Carlos Noriega, William Robbins, Jim Ruszkowski, Sarah Shull, Ernest Smith, Kenneth Todd, Debbie Trainor, Mark Trevino, Kevin Watson, and Dennis Webb. NR 8 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 0-7695-2644-6 PY 2006 BP 306 EP + PG 2 WC Engineering, Aerospace; Computer Science, Information Systems SC Engineering; Computer Science GA BEW90 UT WOS:000239914200043 ER PT B AU Larchev, GV Lohn, JD AF Larchev, Gregory V. Lohn, Jason D. GP IEEE Computer Society TI Evolutionary based techniques for fault tolerant Field Programmable Gate Arrays SO SMC-IT 2006: 2ND IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 2nd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 17-20, 2006 CL Pasadena, CA SP IEEE Comp Soc, TCCX, Task Force Autonom & Autonomous Syst, Jet Propuls Lab, Calif Inst Technol AB The use of SRAM-based Field Programmable Gate Arrays (FPGAs) is becoming more and more prevalent in space applications. Commercial-grade FPGAs are potentially susceptible to permanently debilitating Single-Event Latchups (SELs). Repair methods based on Evolutionary Algorithms may be applied to FPGA circuits to enable successful fault recovery. This paper presents the experimental results of applying such methods to repair four commonly used circuits (quadrature decoder, 3-by-3-bit multiplier, 3-by-3-bit adder, 4-to-7 decoder) into which a number of simulated faults has been introduced. The results suggest that evolutionary repair techniques can improve the process of fault recovery when used instead of, or as a supplement to Triple Modular Redundancy (TMR), which is currently the predominant method for mitigating FPGA faults. C1 [Larchev, Gregory V.] Univ Calif Santa Cruz, Res Ctr, Santa Cruz, CA 95064 USA. [Larchev, Gregory V.; Lohn, Jason D.] NASA, Ames Res Ctr, Moffett Field, CA USA. RP Larchev, GV (reprint author), Univ Calif Santa Cruz, Res Ctr, Santa Cruz, CA 95064 USA. EM glarchev@mail.arc.nasa.gov; jlohn@email.arc.nasa.gov NR 14 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 0-7695-2644-6 PY 2006 BP 314 EP + PG 2 WC Engineering, Aerospace; Computer Science, Information Systems SC Engineering; Computer Science GA BEW90 UT WOS:000239914200044 ER PT B AU Malakooti, B Kim, H Bhasin, K AF Malakooti, Behnam Kim, Hyun Bhasin, Kul GP IEEE Computer Society TI Human & robotics technology space exploration communication scenarios: Characteristics, challenges & scenarios for developing Intelligent Internet Protocols SO SMC-IT 2006: 2ND IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 2nd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 17-20, 2006 CL Pasadena, CA SP IEEE Comp Soc, TCCX, Task Force Autonom & Autonomous Syst, Jet Propuls Lab, Calif Inst Technol AB In this paper, we provide a comprehensive view of current and future space communications systems, and scenarios in relation with Intelligent Internet Protocol (HP). IIP is an innovative network layer protocol developed to meet the shortcomings of existing Internet Protocol (IP) in an adverse space networking environment and provide future communication support for NASA space exploration activities. LIP distinguishes itself from other existing/proposed protocols with six signature functionalities: a) multiple criteria routing, b) reconfigurability, c) automatic routing and tracking, d) dynamic routing, e) human-in-space routing, and f) intelligent routing. Each of these functionalities provides unique capabilities to overcome constraints of space networks. To demonstrate the applicability of the IIP six functionalities, we present a comprehensive scenario for each of surface, orbital, and backbone networks where each scenario closely resembles the actual operations and problems encountered in space. In each scenario, we provide network characteristics, requirements, and applications of IIP functionalities. C1 [Malakooti, Behnam; Kim, Hyun] Case Western Reserve Univ, Cleveland, OH 44106 USA. [Bhasin, Kul] NASA, Glenn Res Ctr, Cleveland, OH USA. RP Malakooti, B (reprint author), Case Western Reserve Univ, Cleveland, OH 44106 USA. EM bxm4@case.edu; hsk5@case.edu; Kul.B.Bhasin@grc.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 BN 0-7695-2644-6 PY 2006 BP 322 EP + PG 2 WC Engineering, Aerospace; Computer Science, Information Systems SC Engineering; Computer Science GA BEW90 UT WOS:000239914200045 ER PT B AU Cai, Y Hu, YX AF Cai, Yang Hu, Yongxiang GP IEEE Computer Society TI Onboard inverse physics from sensor web SO SMC-IT 2006: 2ND IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 2nd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 17-20, 2006 CL Pasadena, CA SP IEEE Comp Soc, TCCX, Task Force Autonom & Autonomous Syst, Jet Propuls Lab, Calif Inst Technol ID FPGA IMPLEMENTATION; PROCESSOR AB Onboard sensory data mining from multiple spacecraft platforms has been an increasingly important task in space missions. In this paper, a Field Programmable Gate Array (FPGA)-based reconfigurable physical inversion prototype is developed for real-time retrieving of physical properties of the investigated area. The generalized inversion processor is able to fuse the data from multi-platform sensors, eliminate redundant algorithm development and provide a vehicle for autonomous onboard image analysis and physics-based data compressions. From our empirical study, we found that the FPGA system is faster than the Pentium-based PC by at least two to three orders of magnitude. The fixed point Radial Basis Function algorithm demonstrates parallelism as tire number of bases increase. C1 [Cai, Yang] Carnegie Mellon Univ, Pittsburgh, PA 15213 USA. [Hu, Yongxiang] NASA, Langley Res Ctr, Moffett Field, CA USA. RP Cai, Y (reprint author), Carnegie Mellon Univ, Pittsburgh, PA 15213 USA. EM ycai@cmu.edu; yongxiang.hu-1@nasa.gov RI Hu, Yongxiang/K-4426-2012 FU NASA ESTO-AIST Program; Army Research Office; NASA Langley Creativity and Innovation Initiative FX We would like to thank the managers and engineers from National Instruments for their comments and support. The work was sponsored in part by NASA ESTO-AIST Program, NASA Langley Creativity and Innovation Initiative and the Army Research Office. NR 25 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 0-7695-2644-6 PY 2006 BP 337 EP + PG 3 WC Engineering, Aerospace; Computer Science, Information Systems SC Engineering; Computer Science GA BEW90 UT WOS:000239914200047 ER PT B AU Rice, K Le Moigne, J Jain, P AF Rice, Kevin Le Moigne, Jacqueline Jain, Peyush GP IEEE Computer Society TI Analyzing range maps data for future space robotics applications SO SMC-IT 2006: 2ND IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 2nd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 17-20, 2006 CL Pasadena, CA SP IEEE Comp Soc, TCCX, Task Force Autonom & Autonomous Syst, Jet Propuls Lab, Calif Inst Technol C1 [Rice, Kevin] GST Corp, 7855 Walker Dr,Suite 200, Greenbelt, MD 20770 USA. [Le Moigne, Jacqueline; Jain, Peyush] NASA, Goddard Space Flight Ctr, Adv Architectures & Automat Branch, Greenbelt, MD 20771 USA. RP Rice, K (reprint author), GST Corp, 7855 Walker Dr,Suite 200, Greenbelt, MD 20770 USA. 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 0-7695-2644-6 PY 2006 BP 357 EP 357 PG 1 WC Engineering, Aerospace; Computer Science, Information Systems SC Engineering; Computer Science GA BEW90 UT WOS:000239914200050 ER PT B AU Rabideau, G Tran, D Chien, S Cichy, B Sherwood, R Mandl, D Frye, S Shulman, S Szwaczkowski, J Boyer, D Van Gaasbeck, J AF Rabideau, Gregg Tran, Daniel Chien, Steve Cichy, Benjamin Sherwood, Rob Mandl, Dan Frye, Stuart Shulman, Seth Szwaczkowski, Joseph Boyer, Darrell Van Gaasbeck, Jim GP IEEE Computer Society TI Mission operations of Earth Observing-1 with onboard autonomy SO SMC-IT 2006: 2ND IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 2nd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 17-20, 2006 CL Pasadena, CA SP IEEE Comp Soc, TCCX, Task Force Autonom & Autonomous Syst, Jet Propuls Lab, Calif Inst Technol AB Space mission operations are extremely labor and knowledge-intensive and are driven by the ground and flight systems. Inclusion of an autonomy capability can have dramatic effects on mission operations. We describe the prior, labor and knowledge intensive mission operations flow for the Earth Observing-1 (EO-1) spacecraft as well as the new autonomous operations as part of the Autonomous Sciencecraft Experiment (ASE). C1 [Rabideau, Gregg; Tran, Daniel; Chien, Steve; Cichy, Benjamin; Sherwood, Rob] CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. [Mandl, Dan] Goddard Space Flight Ctr, Greenbelt, MD USA. [Frye, Stuart] Goddard Space Flight Ctr, Mitre Tek, Greenbelt, MD USA. [Shulman, Seth; Szwaczkowski, Joseph] Goddard Space Flight Ctr, Honeywell, Greenbelt, MD USA. [Boyer, Darrell; Van Gaasbeck, Jim] Interface & Control Syst, Houston, TX USA. RP Rabideau, G (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. FU National Aeronautics and Space Administration at Jet Propulsion Laboratory, California Institute of Technology FX Portions of this work were performed at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. NR 8 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 0-7695-2644-6 PY 2006 BP 367 EP + PG 3 WC Engineering, Aerospace; Computer Science, Information Systems SC Engineering; Computer Science GA BEW90 UT WOS:000239914200052 ER PT B AU Knight, R AF Knight, Russell GP IEEE Computer Society TI Solving swath problems optimally SO SMC-IT 2006: 2nd IEEE International Conference on Space Mission Challenges for Information Technology, Proceedings LA English DT Proceedings Paper CT 2nd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 17-20, 2006 CL Pasadena, CA SP IEEE Comp Soc, TCCX, Task Force Autonom & Autonomous Syst, Jet Propuls Lab, Calif Inst Technol AB We present the first optimal algorithms for swath segment scheduling for orbiting spacecraft. We present a comparison between an integer program formulation and a branch and bound formulation that makes use of a flow network transformation, each capable of solving instances of these problems optimally. We also compare our techniques with the current state of the practice: the Aster scheduling algorithm. No technique strictly dominates all others, and we characterize their respective advantages and disadvantages. Note that this problem is NP-complete. The primary goal of our work is to solve the largest swath problems possible, both quickly, and where feasible, optimally.. C1 CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA. RP Knight, R (reprint author), CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA. NR 14 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 0-7695-2644-6 PY 2006 BP 380 EP 385 PG 6 WC Engineering, Aerospace; Computer Science, Information Systems SC Engineering; Computer Science GA BEW90 UT WOS:000239914200054 ER PT B AU Morris, RA Dungan, JL Bresina, JL AF Morris, Robert A. Dungan, Jennifer L. Bresina, John L. GP IEEE Computer Society TI An information infrastructure for coordinating Earth science observations SO SMC-IT 2006: 2ND IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 2nd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 17-20, 2006 CL Pasadena, CA SP IEEE Comp Soc, TCCX, Task Force Autonom & Autonomous Syst, Jet Propuls Lab, Calif Inst Technol AB Earth scientists require timely, coordinated access to remote sensing resources, either directly by requesting that the resource be targeted at a specific location, or indirectly through access to data that has been, or will be acquired and stored in data archives. The information infrastructure for effective coordinated observing does not currently exist. This paper describes a set of capabilities for enabling model-based observing, the idea of linking scheduling observation resources more directly to science goals. Model-based observing is realized in this paper by an approach based on concepts of distributed planning and scheduling. The problem raises challenging issues related to planning under uncertainty, monitoring and repair of plans, and reasoning about human objectives and preferences. C1 [Morris, Robert A.; Dungan, Jennifer L.; Bresina, John L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Morris, RA (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM morris@email.arc.nasa.gov RI Dungan, Jennifer/G-9921-2016 OI Dungan, Jennifer/0000-0002-4863-1616 NR 9 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 0-7695-2644-6 PY 2006 BP 397 EP + PG 2 WC Engineering, Aerospace; Computer Science, Information Systems SC Engineering; Computer Science GA BEW90 UT WOS:000239914200056 ER PT B AU Benowitz, E Clark, K Watney, G AF Benowitz, Ed Clark, Ken Watney, Garth GP IEEE Computer Society TI Auto-coding UML statecharts for flight software SO SMC-IT 2006: 2ND IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 2nd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 17-20, 2006 CL Pasadena, CA SP IEEE Comp Soc, TCCX, Task Force Autonom & Autonomous Syst, Jet Propuls Lab, Calif Inst Technol AB Statecharts have been used as a means to communicate behaviors in a precise manner between system engineers and software engineers. Hand-translating a statechart to code, as clone on some previous space missions, introduces the possibility of errors in the transformation from chart to code. To improve auto-coding, we have developed a process that generates flight code from UML statecharts. Our process is being used for the flight software on the Space Interferometer Mission (SIM). C1 [Benowitz, Ed; Clark, Ken; Watney, Garth] CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA. RP Benowitz, E (reprint author), CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA. EM Edward.Benowitz@jpl.nasa.gov; Ken.Clark@jpl.nasa.gov; Garth.Watney@jpl.nasa.gov FU NASA's Space Interferometer Mission (SIM); Jet Propulsion Laboratory (JPL); California Institute of Technology under National Aeronautics Administration; JPL's Laboratory for Reliable Software (LaRS); JPL R&TD research proposal award; JPL's section 512 FX This work was supported by the NASAs Space Interferometer Mission (SIM), and by the Jet Propulsion Laboratory (JPL), California Institute of Technology under a contract with the National Aeronautics Administration. Additional funding was provided by JPLs Laboratory for Reliable Software (LaRS), and by a JPL R&TD research proposal award for "Software Assurance for the Emerging Discipline of Model-Based Design." supported by JPLs section 512. NR 10 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 0-7695-2644-6 PY 2006 BP 413 EP + PG 2 WC Engineering, Aerospace; Computer Science, Information Systems SC Engineering; Computer Science GA BEW90 UT WOS:000239914200058 ER PT B AU Frank, J AF Frank, Jeremy GP IEEE Computer Society TI SOFIA's challenge: Automated scheduling of airborne astronomy observations SO SMC-IT 2006: 2nd IEEE International Conference on Space Mission Challenges for Information Technology, Proceedings LA English DT Proceedings Paper CT 2nd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 17-20, 2006 CL Pasadena, CA SP IEEE Comp Soc, TCCX, Task Force Autonom & Autonomous Syst, Jet Propuls Lab, Calif Inst Technol AB The Stratospheric Observatory for Infrared Astronomy (SOFIA) will require scheduling flights in support of observations proposed by many different investigators. Automation will be crucial to enable efficient and effective scheduling of SOFIA flights. We have designed an Automated Flight Planner (AFP) that accepts as input a set of requested observations, designated flight days, weather predictions and fuel limitations, and searches automatically for high-quality flight plans that satisfy all relevant aircraft and astronomer specified constraints. The AFP can generate one week's worth of flights in tens of minutes of computation time, a feat beyond the capabilities of human flight planners. The rate at which the AFP can generate flights enables a small staff to assess and analyze complex tradeoffs between fuel consumption, estimated science quality and the percentage of scheduled observations. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Frank, J (reprint author), NASA, Ames Res Ctr, Mail Stop N269-3, Moffett Field, CA 94035 USA. NR 8 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 0-7695-2644-6 PY 2006 BP 457 EP 464 PG 8 WC Engineering, Aerospace; Computer Science, Information Systems SC Engineering; Computer Science GA BEW90 UT WOS:000239914200064 ER PT B AU Semmel, GS Boloni, L AF Semmel, Glen S. Boloni, Ladislau GP IEEE Computer Society TI Maturing monitoring agents into model based diagnostic agents for ground processing of the space shuttle and future exploration SO SMC-IT 2006: 2ND IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 2nd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 17-20, 2006 CL Pasadena, CA SP IEEE Comp Soc, TCCX, Task Force Autonom & Autonomous Syst, Jet Propuls Lab, Calif Inst Technol C1 [Semmel, Glen S.] NASA, DX-E1, Kennedy Space Ctr, FL 32899 USA. [Boloni, Ladislau] Univ Cent Florida, Dept Elect & Comp Engn, Orlando, FL 32816 USA. RP Semmel, GS (reprint author), NASA, DX-E1, Kennedy Space Ctr, FL 32899 USA. EM Glenn.S.Semmel@nasa.gov; lboloni@cpe.ucf.edu 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 0-7695-2644-6 PY 2006 BP 465 EP 465 PG 1 WC Engineering, Aerospace; Computer Science, Information Systems SC Engineering; Computer Science GA BEW90 UT WOS:000239914200065 ER PT B AU Bresina, JL Morris, PH AF Bresina, John L. Morris, Paul H. GP IEEE Computer Society TI Mission operations planning: Beyond MAPGEN SO SMC-IT 2006: 2ND IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 2nd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 17-20, 2006 CL Pasadena, CA SP IEEE Comp Soc, TCCX, Task Force Autonom & Autonomous Syst, Jet Propuls Lab, Calif Inst Technol AB The MAPGEN system was deployed in the Mars Exploration Rover mission as a mission-critical component of the ground operations system. MAPGEN, which was jointly developed by ARC and JPL, represents a successful mission infusion of planning technology. The MER mission has operated spectacularly for over two years now, and we have learned valuable lessons regarding application of mixed-initiative planning technology to mission operations. These lessons have spawned new research in mixed-initiative planning and have influenced the design of a new ground operations system, called ENSEMBLE, that is base-lined for the Phoenix and Mars Science Laboratory missions. This paper discusses some of the lessons learned from the MER mission infusion experience and presents a preliminary report on these subsequent developments. C1 [Bresina, John L.; Morris, Paul H.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Bresina, JL (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM John.L.Bresina@nasa.gov; Paul.H.Morris@nasa.gov 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 0-7695-2644-6 PY 2006 BP 477 EP + PG 2 WC Engineering, Aerospace; Computer Science, Information Systems SC Engineering; Computer Science GA BEW90 UT WOS:000239914200067 ER PT B AU Mayorga, A AF Mayorga, Arturo GP IEEE Computer Society TI An auto configuration system for the GMSEC architecture and API SO SMC-IT 2006: 2nd IEEE International Conference on Space Mission Challenges for Information Technology, Proceedings LA English DT Proceedings Paper CT 2nd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 17-20, 2006 CL Pasadena, CA SP IEEE Comp Soc, TCCX, Task Force Autonom & Autonomous Syst, Jet Propuls Lab, Calif Inst Technol C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Mayorga, A (reprint author), NASA, Goddard Space Flight Ctr, Code 583,8800 Greenbelt Rd, Greenbelt, MD 20771 USA. 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 0-7695-2644-6 PY 2006 BP 485 EP 485 PG 1 WC Engineering, Aerospace; Computer Science, Information Systems SC Engineering; Computer Science GA BEW90 UT WOS:000239914200068 ER PT B AU Kulkarni, N Ippolito, C Krishnakumar, K Al-Ali, KM AF Kulkarni, Nilesh Ippolito, Corey Krishnakumar, Kalmanje Al-Ali, Khalid M. GP IEEE Computer Society TI Adaptive inner-loop rover control SO SMC-IT 2006: 2ND IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 2nd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 17-20, 2006 CL Pasadena, CA SP IEEE Comp Soc, TCCX, Task Force Autonom & Autonomous Syst, Jet Propuls Lab, Calif Inst Technol AB Adaptive control technology is developed for the inner-loop speed and steering control of the MAX Rover. MAX a CMU developed Rover, is a compact low-cost 4-wheel drive, 4-wheel steer (double Ackerman), with high-clearance agile durable chassis. It is outfitted with sensors and electronics that make it ideally suited for supporting research relevant to intelligent tele-operation, and as a low-cost autonomous robotic test bed and appliance. The control design consists of a feedback linearization based controller with a proportional-integral (PI) feedback that is augmented by an online adaptive neural network. The adaptation law has guaranteed stability properties for safe operation. The control design is retrofit in nature so that it fits below the outer-loop path planning algorithms. Successful hardware implementation of the controller is illustrated for several scenarios consisting of actuator failures and modeling errors in the nominal design. C1 [Kulkarni, Nilesh; Ippolito, Corey] NASA, QSS Grp Inc, Ames Res Ctr, Moffett Field, CA 94035 USA. [Krishnakumar, Kalmanje] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Al-Ali, Khalid M.] NASA, Carnegie Mellon Univ, Ames Res Ctr, Moffett Field, CA USA. RP Kulkarni, N (reprint author), NASA, QSS Grp Inc, Ames Res Ctr, Moffett Field, CA 94035 USA. EM nilesh@email..arc.nasa.gov; cippolito@mail..arc.nasa.gov; Kahnanje.Krishnakumar@nasa.gov; alali@cmu.edu 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 0-7695-2644-6 PY 2006 BP 497 EP + PG 2 WC Engineering, Aerospace; Computer Science, Information Systems SC Engineering; Computer Science GA BEW90 UT WOS:000239914200070 ER PT B AU Wang, YF Wax, A Larn, R Baldwin, J Borden, C AF Wang, Y. -F. Wax, A. Larn, R. Baldwin, J. Borden, C. GP IEEE Computer Society TI Collaborative scheduling using JMS in a mixed Java and NET environment SO SMC-IT 2006: 2ND IEEE INTERNATIONAL CONFERENCE ON SPACE MISSION CHALLENGES FOR INFORMATION TECHNOLOGY, PROCEEDINGS LA English DT Proceedings Paper CT 2nd IEEE International Conference on Space Mission Challenges for Information Technology CY JUL 17-20, 2006 CL Pasadena, CA SP IEEE Comp Soc, TCCX, Task Force Autonom & Autonomous Syst, Jet Propuls Lab, Calif Inst Technol AB A collaborative framework/environment was proto-typed to prove the feasibility of scheduling space flight missions on NASA's Deep Space Network (DSN) in a distributed fashion. In this environment, effective collaboration relies on efficient communications among all flight mission and DSN scheduling users. Therefore, messaging becomes critical to timely event notification and data synchronization. In the prototype, a rapid messaging system using Java Message Service (JMS) in a mixed Java and NET environment is established This scheme allows both Java and NET applications to communicate with each other for data synchronization and schedule negotiation. The JMS approach we used is based on a centralized messaging scheme. With proper use of a high speed messaging system, all users in this collaborative framework can communicate with each other to generate a schedule collaboratively to meet DSN and projects tracking needs. C1 [Wang, Y. -F.; Wax, A.; Larn, R.; Baldwin, J.; Borden, C.] CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA. RP Wang, YF (reprint author), CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA. EM Yeou-Fang.Wang@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 0-7695-2644-6 PY 2006 BP 505 EP + PG 2 WC Engineering, Aerospace; Computer Science, Information Systems SC Engineering; Computer Science GA BEW90 UT WOS:000239914200071 ER PT S AU Dehlinger, J Lutz, RR AF Dehlinger, Josh Lutz, Robyn R. BE Garcia, A Choren, R Luccena, C Giorgini, P Holvoet, T Romanavsky, A TI A product-line approach to promote asset reuse in multi-agent systems SO SOFTWARE ENGINEERING FOR MULTI-AGENT SYSTEMS IV: RESEARCH ISSUES AND PRACTICAL APPLICATIONS SE Lecture Notes in Computer Science LA English DT Article; Proceedings Paper CT 4th International Workshop on Software Engineering for Large-Scale Multi-Agent Systems CY MAY, 2005 CL St Louis, MO AB Software reuse technologies have been a driving force in significantly reducing both the time and cost of software specification, development, maintenance and evolution. However, the dynamic nature of highly autonomous agents in distributed systems is difficult to specify with existing requirements analysis and specification techniques. This paper offers an approach for open, agent-based distributed software systems to capture requirements specifications in such a way that they can be easily reused during the initial requirements phase as well as later if the software needs to be updated. The contribution of this paper is to provide a reusable requirements specification pattern to capture the dynamically changing design configurations of agents and reuse them for future similar systems. This is achieved by adopting a product-line approach for agent-based software engineering. We motivate and illustrate this work through a specific application, a phased deployment of an agent-based, distributed microsatellite constellation. C1 Iowa State Univ, Dept Comp Sci, Ames, IA 50011 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Dehlinger, J (reprint author), Iowa State Univ, Dept Comp Sci, 226 Atanasoff Hall, Ames, IA 50011 USA. EM dehlinge@cs.iastate.edu; rlutz@cs.iastate.edu RI Holvoet, Tom/A-3649-2015 NR 28 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 3-540-33580-3 J9 LECT NOTES COMPUT SC PY 2006 VL 3914 BP 161 EP 178 PG 18 WC Computer Science, Artificial Intelligence; Computer Science, Software Engineering; Computer Science, Theory & Methods SC Computer Science GA BEN40 UT WOS:000238283600010 ER PT B AU Ewert, MK Bergeron, DJ AF Ewert, Michael K. Bergeron, David J., III GP ASME TI Development of a solar heat pump for space SO Solar Engineering 2005 LA English DT Proceedings Paper CT International Solar Energy Conference CY AUG 06-12, 2005 CL Orlando, FL SP Sharp, Kycera Solar Inc, Univ Florida, Dept Environm, ACCESS, Innovat Design, ASME, Solar Energy Div AB As humans explore space, we find even greater temperature extremes than on Earth. Apollo astronauts, for example, did not stay on the moon past noon when surface temperatures soar to over 100 degrees C. As we have on Earth, future space explorers will likely turn to mechanical heating and cooling systems to maintain comfortable living spaces. Most locations in Earth's neighborhood have an abundant natural energy source from the sun, thus the development effort has taken a systems engineering approach and tried to optimize the heat pump and solar power source together. Earlier studies have shown that vapor compression cycle heat pumps are the most mass and power efficient for space applications. Photovoltaic (PV) cells are the most mature solar power conversion technology to provide electricity to the vapor compressor in space. Hence, these two technologies have been integrated into a solar PV vapor compression heat pump. A "ground-test unit" Solar Heat Pump designed to provide 15 kilowatts of cooling was completed in 2002 and underwent preliminary testing at SunDanzer's previous location in Nevada. Following buildup of a heat pump testbed that will allow simulation of radiator loop temperatures on the moon or Mars, a complete system evaluation will be conducted in 2005 at the Johnson Space Center. Following that, the gravity dependent components of the system, most notably the compressor, will be analyzed and upgraded for the required gravity environment(s). A gravity-independent approach would allow NASA mission designers the most flexibility to use heat pump technology in future mission scenarios, but technical challenges may lead to machines optimized for a particular application. Design data and analysis, as well as the preliminary test results, indicate that the Solar Heat Pump will achieve very good efficiency, near 45% of Carnot efficiency, at a temperature lift of 45 degrees C. A novel motor controller and computer control software allow the heat pump to use solar power directly from the PV array at about 400 volts direct current. These features, referred to as "PV-direct", along with a good thermodynamic design, form a solid basis for the design of a future space-qualified Solar Heat Pump. C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Ewert, MK (reprint author), NASA, Lyndon B Johnson Space Ctr, 2101 NASA Pkwy, Houston, TX 77058 USA. NR 8 TC 0 Z9 0 U1 1 U2 2 PU AMER SOC MECHANICAL ENGINEERS PI NEW YORK PA THREE PARK AVENUE, NEW YORK, NY 10016-5990 USA BN 0-7918-4737-3 PY 2006 BP 707 EP 712 PG 6 WC Energy & Fuels SC Energy & Fuels GA BFO21 UT WOS:000243400500086 ER PT S AU Gopalswamy, N Mewaldt, R Torsti, J AF Gopalswamy, N. Mewaldt, R. Torsti, J. BE Gopalswamy, N Mewaldt, R Torsti, J TI Solar eruptions and energetic particles: An introduction SO Solar Eruptions and Energetic Particles SE GEOPHYSICAL MONOGRAPH SERIES LA English DT Proceedings Paper CT AGU Chapman Conference on Solar Energetic Plasmas and Particles CY AUG 02-06, 2004 CL Univ Turku, Turku, FINLAND SP AGU HO Univ Turku AB This introductory article highlights current issues concerning two related phenomena involving mass emission from the Sun: solar eruptions and solar energetic particles. A brief outline of the chapters is provided indicating how the current issues are addressed in the monograph. The sections in this introduction roughly group the chapters dealing with coronal mass ejections (CMEs), solar energetic particles (SEPs), shocks, and space weather. The concluding remarks include a brief summary of outstanding issues that drive current and future research on CMEs and SEPs. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Gopalswamy, N (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI Gopalswamy, Nat/D-3659-2012 NR 0 TC 3 Z9 3 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0065-8448 BN 0-87590-430-0 J9 GEOPH MONOG SERIES PY 2006 VL 165 BP 1 EP 5 DI 10.1029/165GM02 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BFJ57 UT WOS:000242377100001 ER PT S AU Moore, RL Sterling, AC AF Moore, Ronald L. Sterling, Alphonse C. BE Gopalswamy, N Mewaldt, R Torsti, J TI Initiation of coronal mass ejections SO SOLAR ERUPTIONS AND ENERGETIC PARTICLES SE Geophysical Monograph Series LA English DT Proceedings Paper CT AGU Chapman Conference on Solar Energetic Plasmas and Particles CY AUG 02-06, 2004 CL Univ Turku, Turku, FINLAND SP AGU HO Univ Turku ID SOLAR FILAMENT ERUPTIONS; FLUX ROPE MODEL; MAGNETIC-FIELD; INTERNAL RECONNECTION; EXTERNAL RECONNECTION; BREAKOUT MODEL; EIT CRINKLES; FLARES; ENERGY; EVOLUTION AB This paper is a synopsis of the initiation of the strong-field magnetic explosions that produce large, fast coronal mass ejections. The presentation outlines our current view of the eruption onset, based on results from our own observational work and from the observational and modeling work of others. From these results and from physical reasoning, we and others have inferred the basic processes that trigger and drive the explosion. We describe and illustrate these processes using cartoons. The magnetic field that explodes is a sheared-core bipole that may or may not be embedded in surrounding strong magnetic field, and may or may not contain a flux rope before it starts to explode. We describe three different mechanisms that singly or in combination can trigger the explosion: (1) runaway internal tether-cutting reconnection, (2) runaway external tether-cutting reconnection, and (3) ideal MHD instability or loss or equilibrium. For most eruptions, high-resolution, high-cadence magnetograms and chromospheric and coronal movies (such as from TRACE or Solar-B) of the pre-eruption region and of the onset of the eruption and flare are needed to tell which one or which combination of these mechanisms is the trigger. Whatever the trigger, it leads to the production of an erupting flux rope. Using a simple model flux rope, we demonstrate that the explosion can be driven by the magnetic pressure of the expanding flux rope, provided the shape of the expansion is "fat" enough. C1 George C Marshall Space Flight Ctr, Space Sci Branch, Huntsville, AL 35812 USA. RP Moore, RL (reprint author), George C Marshall Space Flight Ctr, Space Sci Branch, XD12, Huntsville, AL 35812 USA. RI Gopalswamy, Nat/D-3659-2012 NR 53 TC 34 Z9 34 U1 1 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0065-8448 BN 0-87590-430-0 J9 GEOPHYS MONOGR SER PY 2006 VL 165 BP 43 EP 57 DI 10.1029/165GM07 PG 15 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BFJ57 UT WOS:000242377100006 ER PT S AU von Rosenvinge, T Cane, HV AF von Rosenvinge, Tycho Cane, Hilary V. BE Gopalswamy, N Mewaldt, R Torsti, J TI Solar energetic particles: An overview SO Solar Eruptions and Energetic Particles SE GEOPHYSICAL MONOGRAPH SERIES LA English DT Proceedings Paper CT AGU Chapman Conference on Solar Energetic Plasmas and Particles CY AUG 02-06, 2004 CL Univ Turku, Turku, FINLAND SP AGU HO Univ Turku ID ADVANCED COMPOSITION EXPLORER; CORONAL MASS EJECTIONS; II RADIO-BURSTS; X-RAY; INTERPLANETARY SHOCKS; ISOTOPE SPECTROMETER; ELECTRON EVENTS; WIND SPACECRAFT; PROTON FLARES; HIGH-ENERGIES AB This paper presents an overview of what we know about energetic particles from the sun, discusses where progress still needs to be made, and briefly enumerates what steps need to be taken next in order to better understand how and where solar electrons and ions are accelerated to high energies. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP von Rosenvinge, T (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. RI Gopalswamy, Nat/D-3659-2012 NR 71 TC 7 Z9 7 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0065-8448 BN 0-87590-430-0 J9 GEOPH MONOG SERIES PY 2006 VL 165 BP 103 EP 114 DI 10.1029/165GM11 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BFJ57 UT WOS:000242377100010 ER PT S AU Gopalswamy, N AF Gopalswamy, Nat BE Gopalswamy, N Mewaldt, R Torsti, J TI Coronal mass ejections and type II radio bursts SO SOLAR ERUPTIONS AND ENERGETIC PARTICLES SE Geophysical Monograph Book Series LA English DT Proceedings Paper CT AGU Chapman Conference on Solar Energetic Plasmas and Particles CY AUG 02-06, 2004 CL Univ Turku, Turku, FINLAND SP AGU HO Univ Turku ID ENERGETIC PARTICLE EVENTS; 1973 JANUARY 11; 9 R PERIOD; INTERPLANETARY SHOCKS; X-RAY; STATISTICAL-ANALYSIS; SOLAR ERUPTIONS; WIND SPACECRAFT; PROTON EVENTS; NEAR-SUN AB The simultaneous availability of white light data on CMEs from the Solar and Heliospheric Observatory (SOHO) and radio data on shock waves from the Radio and Plasma Wave experiment on board the Wind spacecraft over the past decade have helped in making rapid progress in understanding the CME-driven shocks. I review some recent developments in the type II-CME relationship, focusing on the properties of CMEs as shock drivers and those of the medium supporting shock propagation. I also discuss the solar cycle variation of the type II bursts in comparison with other eruptive phenomena such as CMEs, flares, large solar energetic particle events, and shocks detected in situ. The hierarchical relationship found between the CME kinetic energy and wavelength range of type II radio bursts, non-existence of CMEless type II bursts, and the explanation of type II burst properties in terms of shock propagation with a realistic profile of the fast mode speed suggest that the underlying shocks are driven by CMEs, irrespective of the wavelength domain. Such a unified approach provides an elegant understanding of the entire type II phenomenon (coronal and interplanetary). The blast wave scenario remains an alternative hypothesis for type II bursts only over a small spatial domain (within one solar radius above the solar surface) that is not accessible to in situ observation. Therefore the existence of blast waves cannot be directly confirmed. CMEs, on the other hand, can be remote sensed from this domain. C1 NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Greenbelt, MD 20771 USA. RP Gopalswamy, N (reprint author), NASA, Goddard Space Flight Ctr, Solar Syst Explorat Div, Bldg 21,Room 260,Code 695, Greenbelt, MD 20771 USA. RI Gopalswamy, Nat/D-3659-2012 NR 99 TC 30 Z9 30 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0065-8448 BN 0-87590-430-0 J9 GEOPHYS MONOGR SER PY 2006 VL 165 BP 207 EP 220 DI 10.1029/165GM20 PG 14 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BFJ57 UT WOS:000242377100019 ER PT S AU Chen, B Xi, DJ Pei, QB Han, S Zhou, CW AF Chen, Bin Xi, Donjuan Pei, Qibing Han, Song Zhou, Chongwu BE Vayssieres, L TI Nanomaterial characterization and synthesis for solar energy utilization and hydrogen fuel generation SO Solar Hydrogen and Nanotechnology SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Solar Hydrogen and Nanotechnology CY AUG 14-17, 2006 CL San Diego, CA SP SPIE ID CADMIUM-SULFIDE; RAMAN-SPECTROSCOPY; OPTICAL-PROPERTIES; INDIUM NITRIDE; QUANTUM DOTS; THIN-FILMS; GROWTH; NANOWIRES; INN; CATALYSTS AB Semiconducting metal oxide nanowires represent a class of novel materials that are of superior properties to naoparticles currently used in dye sensitized solar cell and polymer hybrid solar cells. The quasi one-dimensional nanostructure and surface states of nanowires improve carrier mobility and charge transfer through interface interactions of theses nanocomposite materials. Raman spectroscopy, especially resonant Raman spectroscopy, is used to correlate nanomaterial synthesis condition to the structural, optical and electric transport properties that are important to photocatalysis, exciton transport and recombination and hydrogen storage mechanism. For example, highly orientated ZnO nanowires studied with Raman and photoluminescence spectroscopy demonstrated the high efficiency of the phonon and electron coupling. These results are compared with that of other ZnO forms such as thin film, polycrystalline powder and solid. The Raman bandwidths and shifts of nanowires revealed the phonon confinement in the quasi one-dimensional nanostructures, which is further demonstrated with In2O3 nanowires at 5, 10, 20, 30 nm in diameters. Room temperature photoluminescence results also show band gap shifts with nanowire dimensions. Nanowire sizes, defects and strains, controlled by synthesis conditions, have shown to determine band structure and optical phonon properties. We also discuss characterization and synthesis of carbon nanotube based composite materials including polymer electropolymerization and infiltration. Combining significantly enhanced mechanical compressive strength and excellent electric conductivity, these composite materials offer potentials to fuel cell anode materials as multifunctional hydrogen storage media. C1 NASA Ames Res Ctr, SETI Inst, Moffett Field, CA USA. RP Chen, B (reprint author), NASA Ames Res Ctr, SETI Inst, Moffett Field, CA USA. NR 33 TC 0 Z9 0 U1 2 U2 12 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6419-8 J9 P SOC PHOTO-OPT INS PY 2006 VL 6340 BP U57 EP U73 DI 10.1117/12.681466 PG 17 WC Energy & Fuels; Nanoscience & Nanotechnology SC Energy & Fuels; Science & Technology - Other Topics GA BFM09 UT WOS:000243024600006 ER PT B AU West, EA Kobayashi, K Gary, GA Davis, JM AF West, E. A. Kobayashi, K. Gary, G. A. Davis, J. M. BE Casini, R Lites, BW TI The solar ultraviolet magnetograph investigation: Polarization properties SO Solar Polarization 4 SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 4th Solar Polarization Workshop CY SEP 19-23, 2005 CL Boulder, CO SP CSAC, CoMP ID GRATINGS AB This paper describes the objectives of the Marshall Space Flight Center (MSFC) Solar Ultraviolet Magnetograph Investigation (SUMI) and the optical components that have been developed to meet those objectives. A sounding rocket payload is being developed to test the feasibility of rnagnetic-field measurements in the Sun's transition region. The optics have been optimized for simultaneous measurements of two magnetic lines formed in the transition region (C IV 1550 angstrom and Mg II 2800 angstrom). Finally; we illustrate the polarization properties of the SUMI polarimeter and toroidal variable-line-space gratings. C1 NASA, MSFC, NSSTC, Huntsville, AL 35805 USA. RP West, EA (reprint author), NASA, MSFC, NSSTC, Huntsville, AL 35805 USA. NR 8 TC 1 Z9 1 U1 1 U2 1 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-583812-26-6 J9 ASTR SOC P PY 2006 VL 358 BP 161 EP 166 PG 6 WC Astronomy & Astrophysics; Physics, Multidisciplinary SC Astronomy & Astrophysics; Physics GA BGE14 UT WOS:000246255400029 ER PT B AU Gary, GA West, EA Rees, DE Zukic, M Herman, P Li, J AF Gary, G. A. West, E. A. Rees, D. E. Zukic, M. Herman, P. Li, J. BE Casini, R Lites, BW TI CIV vacuum ultraviolet fabry-perot interferometers for transition-region magnetography SO SOLAR POLARIZATION 4 SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT 4th Solar Polarization Workshop CY SEP 19-23, 2005 CL Boulder, CO SP CSAC, CoMP AB The vacuum ultraviolet region allows remote sensing of the upper levels of the solar atmosphere where the magnetic field dominates the physics. Obtaining an imaging interferometer that observes the transition region is the goal of this program. This paper gives a summary of our instrument development program (1998-2005) for a high-spectral-resolution, piezoelectric tunable Vacuum Ultraviolet Fabry-Perot Interferometer (VUV FPI) for obtaining narrow-passband images, magnetograms, and Dopplergrams of the transition region emission line of C IV (155 nm). A VUV interferometer will allow us to observe the magnetic field, flows, and heating events in the mid-transition region. The MSFC VUV FPI has measured values of FWHM similar to 9pm, FSR similar to 62 pm, finesse similar to 5.3, and transmittance similar to 50% at 157 nm. For the measurements, the University of Toronto's F-2 eximer laser was used as an appropriate proxy for C IV 155 nm. This has provided the first tunable interferometer with a FWHM compatible to VUV filter magnetograph. C1 [Gary, G. A.; West, E. A.] NASA, George C Marshall Space Flight Ctr, NSSTC, Huntsville, AL 35805 USA. [Rees, D. E.] Hovemere Ltd, Kent TN145HD, United Kingdom. [Zukic, M.] Cascade Optical Grp, Santa Ana, CA 92705 USA. [Herman, P.; Li, J.] Univ Toronto, Dept Elect & Comp Engn, Toronto, ON M5S 3G4, Canada. RP Gary, GA (reprint author), NASA, George C Marshall Space Flight Ctr, NSSTC, Huntsville, AL 35805 USA. RI Herman, Peter/A-6464-2008 OI Herman, Peter/0000-0002-9157-8259 NR 6 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 978-1-583812-26-6 J9 ASTR SOC P PY 2006 VL 358 BP 181 EP + PG 2 WC Astronomy & Astrophysics; Physics, Multidisciplinary SC Astronomy & Astrophysics; Physics GA BGE14 UT WOS:000246255400033 ER PT B AU West, EA Gary, GA AF West, E. A. Gary, G. A. BE Casini, R Lites, BW TI Large field-of-view KD*P modulator for solar polarization measurements SO Solar Polarization 4 SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT 4th Solar Polarization Workshop CY SEP 19-23, 2005 CL Boulder, CO SP CSAC, CoMP AB This paper describes the evolution of the Marshall Space Flight Center's (MSFC) electro-optical polarimeter with emphasis on the field-of-view characteristics of the KD*P modulator. Understanding those characteristics was essential to the success of the MSFC solar vector magnetograph. We show how the field-of-view (FOV) errors of KD*P look similar to the linear polarization patterns seen in simple sunspots, and why the placement of the KD*P in a collimated beazn was essential in separating the instrumental polarization from the solar signal. Finally, we describe a modulator design which minimizes those FOV errors. C1 NASA, George C Marshall Space Flight Ctr, NSSTC, Huntsville, AL 35805 USA. RP West, EA (reprint author), NASA, George C Marshall Space Flight Ctr, NSSTC, Huntsville, AL 35805 USA. NR 9 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-583812-26-6 J9 ASTR SOC P PY 2006 VL 358 BP 209 EP 212 PG 4 WC Astronomy & Astrophysics; Physics, Multidisciplinary SC Astronomy & Astrophysics; Physics GA BGE14 UT WOS:000246255400040 ER PT J AU Miner, ED Matson, DL Spilker, LJ AF Miner, Ellis D. Matson, Dennis L. Spilker, Linda J. BE Blondel, P Mason, JW TI Cassini at Saturn: The First Results SO SOLAR SYSTEM UPDATE SE Springer-Praxis Books in Astronomy and Planetary Sciences LA English DT Article; Book Chapter ID IMAGING SCIENCE; RADIO-EMISSION; MOON PHOEBE; SOLAR-WIND; TITAN; MAGNETOSPHERE; SYSTEM; SPECTROSCOPY; ATMOSPHERE; AURORAE AB The international Cassini-Huygens Mission is a joint mission of the National Aeronautics and Space Administration and the European Space Agency, with the Italian Space Agency as a major partner. The spacecraft was launched from Cape Canaveral, Florida, on October 15, 1997, and was inserted into orbit around the planet Saturn on July 1, 2004. The Huygens Probe separated from the Cassini Orbiter on December 26, 2004 and coasted to a descent by parachute through the atmosphere of Titan to the surface on January 14, 2005. This chapter summarizes the primary science results to date from both the orbiter and the probe. Many of the analyses are preliminary in nature, and some may be revised as additional data enables better characterization of Saturn and its system of rings, magnetosphere and satellites. The initial results summarized in this chapter include images and other data from a close encounter of Phoebe prior to Saturn orbit insertion, from ring studies and magnetospheric studies during orbit insertion and the first year in orbit, from studies of Titan during the first several flybys and from the Huygens Probe mission, and from close flybys of several of Saturn's icy satellites. The results also include discovery of several new satellites and a new radiation belt between the rings and Saturn's atmosphere. C1 [Miner, Ellis D.] Jet Prop Lab, Lake View Terrace, CA 91342 USA. [Matson, Dennis L.; Spilker, Linda J.] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM ellis.d.miner@jpl.nasa.gov; Dennis.L.Matson@jpl.nasa.gov; Linda.J.Spilker@jpl.nasa.gov NR 49 TC 0 Z9 0 U1 0 U2 1 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY BN 978-3-540-37683-5 J9 S-P B ASTRON PLANET PY 2006 BP 217 EP 249 DI 10.1007/3-540-37683-6_9 D2 10.1007/3-540-37683-6 PG 33 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BLQ78 UT WOS:000270817000010 ER PT S AU Field, C Schmidt, GA Koch, D AF Field, C. Schmidt, G. A. Koch, D. BE Ermolli, I Pap, J Fox, P TI Solar and climatic effects on Be-10 SO SOLAR VARIABILITY AND EARTH'S CLIMATE SE MEMORIE DELLA SOCIETA ASTRONOMICA ITALIANA - SERIES LA English DT Proceedings Paper CT Conference on Solar Variability and Earths Climate CY JUN 27-JUL 01, 2005 CL Rome, ITALY SP Ist Nazl Astrofis, Minist Ambiente Della Tutela Territor, Reg Lazio, Eurpean Space Agcy, Climate & Weather Sun-Earth Syst ID GREENLAND ICE-SHEET; NORTH-ATLANTIC; MODULATION; ANTARCTICA; CYCLES; MODEL; CORE AB To understand contemporary climate change and anthropogenic climate forcings, it is necessary to quantify solar forcing, the most significant natural forcing on centennial timescales. The close correlation between the production of the cosmogenic isotope Be-10 and changes in heliomagnetic activity makes Be-10 an attractive proxy for studying changes in solar output. C1 Columbia Univ, DEES, NASA, GISS, New York, NY 10027 USA. RP Field, C (reprint author), Columbia Univ, DEES, NASA, GISS, New York, NY 10027 USA. EM cfield@giss.nasa.gov NR 22 TC 0 Z9 0 U1 0 U2 0 PU SOC ASTRONOMICA ITALIANA PI FLORENCE PA LARGO ENRICO FERMI 5, FLORENCE, 50125, ITALY SN 0037-8720 J9 MEM SOC ASTRON ITAL PY 2006 VL 76 IS 4 BP 805 EP 809 PG 5 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BEG25 UT WOS:000237205500015 ER PT S AU Prasad, NS Trivedi, SB Kutcher, S Wang, CC Jagannathan, G Hommerich, U Shukla, V Sandangi, R Kear, B AF Prasad, Narasimha S. Trivedi, Sudhir B. Kutcher, Susan Wang, Chen-Chia Jagannathan, G. Hommerich, Uwe Shukla, Vijay Sandangi, Rajendra Kear, Bernard BE Hoffman, HJ Shori, RK TI Development of solid-state ceramic laser material using Nd : Yttria - art. no. 610012 SO Solid State Lasers XV: Technology and Devices SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Solid State Lasers XV CY JAN 23-26, 2006 CL San Jose, CA ID TRANSFORMATION-ASSISTED CONSOLIDATION; COATINGS AB In this paper, recent progress made towards the development of transparent Nd doped ceramic yttria is presented. Using 99.99% pure raw materials and with improved material processing techniques, Nd doped ceramic yttria test samples greater than 99% transmission at 2000nm wavelength and bandedge < 250nm have been produced. The test samples were > 1" x 1'' x 10mm in dimensions. Nd ions were successfully incorporated into undoped ceramic yttria material through diffusion process. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Prasad, NS (reprint author), NASA, Langley Res Ctr, 5 N Dryden St,MS 468, Hampton, VA 23681 USA. 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 0-8194-6142-3 J9 P SOC PHOTO-OPT INS PY 2006 VL 6100 BP 10012 EP 10012 AR 610012 DI 10.1117/12.657763 PG 10 WC Optics SC Optics GA BEF92 UT WOS:000237165400034 ER PT S AU Afzal, RS AF Afzal, Robert S. BE Hoffman, HJ Shori, RK TI Performance of the GLAS laser transmitter - art. no. 610020 SO Solid State Lasers XV: Technology and Devices SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Solid State Lasers XV CY JAN 23-26, 2006 CL San Jose, CA DE solid-state lasers; space lasers; diode-pumped laser ID ALTIMETER AB The Geoscience Laser Altimeter System (GLAS), launched in January 2003, is a laser altimeter and lidar for the Earth Observing System's (EOS) ICESat mission. The laser transmitter requirements, design and qualification test results and in-flight performance for this space-based remote sensing instrument is summarized and presented. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Afzal, RS (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 16 TC 0 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 0-8194-6142-3 J9 P SOC PHOTO-OPT INS PY 2006 VL 6100 BP 10020 EP 10020 AR 610020 DI 10.1117/12.660701 PG 9 WC Optics SC Optics GA BEF92 UT WOS:000237165400061 ER PT S AU Afzal, RS AF Afzal, Robert S. BE Hoffman, HJ Shori, RK TI Review of solid-state lasers for space applications - art. no. 61001U SO Solid State Lasers XV: Technology and Devices SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Solid State Lasers XV CY JAN 23-26, 2006 CL San Jose, CA DE solid-state lasers.; space lasers; diode-pumped laser AB Solid-state lasers have been in use for space applications since the early days of the space program. To date most of the lasers have been pulsed Nd:YAG lasers and with the development of diode laser technology as pump sources, performance improvements in lifetime, weight and efficiency have been the key drivers to enable space missions. This paper will review the lasers used on various missions and discuss their designs and performance in light of their mission requirements. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Afzal, RS (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 12 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6142-3 J9 P SOC PHOTO-OPT INS PY 2006 VL 6100 BP U1001 EP U1001 AR 61001U DI 10.1117/12.660699 PG 5 WC Optics SC Optics GA BEF92 UT WOS:000237165400056 ER PT S AU Ott, MN Coyle, DB Canham, JS Leidecker, HW AF Ott, Melanie N. Coyle, D. Barry Canham, John S. Leidecker, Henning W. BE Hoffman, HJ Shori, RK TI Qualification and issues with space flight laser systems and components - art. no. 61001V SO Solid State Lasers XV: Technology and Devices SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Solid State Lasers XV CY JAN 23-26, 2006 CL San Jose, CA DE Nd : YAG; laser diode array; flight qualified laser; lifetime; contamination; radiation; reliability ID ND-YAG LASER; ALTIMETER AB The art of flight quality solid-state laser development is still relatively young, and much is still unknown regarding the best procedures, components, and packaging required for achieving the maximum possible lifetime and reliability when deployed in the harsh space environment. One of the most important issues is the limited and unstable supply of quality, high power diode arrays with significant technological heritage and market lifetime. Since Spectra Diode Labs Inc. ended their involvement in the pulsed array business in the late 1990's, there has been a flurry of activity from other manufacturers, but little effort focused on flight quality production. This forces NASA, inevitably, to examine the use of commercial parts to enable space flight laser designs. System-level issues such as power cycling, operational derating, duty cycle, and contamination risks to other laser components are some of the more significant unknown, if unquantifiable, parameters that directly effect transmitter reliability. Designs and processes can be formulated for the system and the components (including thorough modeling) to mitigate risk based on the known failures modes as well as lessons learned that GSFC has collected over the past ten years of space flight operation of lasers. In addition, knowledge of the potential failure modes related to the system and the components themselves can allow the qualification testing to be done in an efficient yet, effective manner. Careful test plan development coupled with physics of failure knowledge will enable cost effect qualification of commercial technology. Presented here will be lessons learned from space flight experience, brief synopsis of known potential failure modes, mitigation techniques, and options for testing from the system level to the component level. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Ott, MN (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 28 TC 0 Z9 0 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 0-8194-6142-3 J9 P SOC PHOTO-OPT INS PY 2006 VL 6100 BP V1001 EP V1001 AR 61001V DI 10.1117/12.674042 PG 15 WC Optics SC Optics GA BEF92 UT WOS:000237165400057 ER PT S AU Su, CH Lehoczky, SL Li, C Raghothamachar, B Dudley, M Szoke, J Barczy, P AF Su, CH Lehoczky, SL Li, C Raghothamachar, B Dudley, M Szoke, J Barczy, P BE Roosz, R Rettenmayr, M Gacsi, Z TI Crystal growth of CdTe by gradient freeze in universal multizone crystallizator (UMC) SO SOLIDIFICATION AND GRAVITY IV SE Materials Science Forum LA English DT Article; Proceedings Paper CT 4th International Conference on Solidification and Gravity CY SEP 06-09, 2004 CL Miskolc Lillafured, HUNGARY SP Univ Miskolc, Mat & Met Engn Fac, Phys Met & Metalforming Dept, Hungarian Acad Sci, Res Grp Mat Sci, NASA MSFC, HAS, Mickolc Comm, Hungarian Space Off, Assoc Hungarian Foundries DE cadmium telluride (CdTe); gradient freeze; Universal Multizone Crystallizator (UMC) ID BRIDGMAN GROWTH; MELT; ZNSE; QUALITY AB In this study, crystals of CdTe were grown from melts, which have undergone different thermal history, by the unseeded gradient freeze method using the Universal Multizone Crystallizator (UMC). The effects of melt conditions on the quality of grown crystal were studied by various characterization techniques, including Synchrotron White Beam X-ray Topography (SWBXT), atomic force microscopy (AFM), electrical conductivity and Hall measurements. C1 NASA, George C Marshall Space Flight Ctr, Micrograv Sci & Applicat Dept SD46, Sci Directorate, Huntsville, AL 35812 USA. Univ Alabama, NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. SUNY Stony Brook, Dept Mat Sci & Engn, Stony Brook, NY 11794 USA. Univ Miskolc, Inst Mat Sci, H-3515 Miskolc, Hungary. RP Su, CH (reprint author), NASA, George C Marshall Space Flight Ctr, Micrograv Sci & Applicat Dept SD46, Sci Directorate, Huntsville, AL 35812 USA. EM ching.h.su@nasa.gov; sandor.l.lehoczky@nasa.gov; chao.li@msfc.nasa.gov; braghoth@ic.sunysb.edu; mdudley@notes.cc.sunysb.edu; janos.szoke@admatis.com; pal.barczy@admatis.com RI Raghothamachar, Balaji/B-1094-2008 NR 16 TC 2 Z9 2 U1 0 U2 1 PU TRANS TECH PUBLICATIONS LTD PI STAFA-ZURICH PA LAUBLSRUTISTR 24, CH-8717 STAFA-ZURICH, SWITZERLAND SN 0255-5476 BN 0-87849-991-1 J9 MATER SCI FORUM PY 2006 VL 508 BP 117 EP 123 PG 7 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Materials Science; Metallurgy & Metallurgical Engineering GA BEA69 UT WOS:000236480800018 ER PT S AU Matney, M Christiansen, E AF Matney, Mark Christiansen, Eric BE Bendisch, J TI A minimalist empirical orbital debris/meteoroid hazard model for the space shuttle SO Space Debris and Space Traffic Management Symposium 2005 SE SCIENCE AND TECHNOLOGY SERIES LA English DT Proceedings Paper CT International-Academy-of-Astronautics-Space-Debris-and-Space-Traffic-Man agement Symposium held Inconjunction with 56th International Astronautical Congress CY OCT 17-21, 2005 CL Fukuoka, JAPAN SP Int Acad Astronaut Space Debris & Space Traffic Management AB Impact hazards due to orbital debris and meteoroids for the US Space Shuttle and other spacecraft have been studied for many years. To date, many sophisticated environment models (such as NASA's ORDEM2000) and collision hazard models (such as NASA's BUMPER) have been developed to accurately assess the overall risk to orbiting vehicles. However, as models get progressively more complex, it is sometimes useful to assess the results at a "back-of-the-envelope" scale. This technique is necessary for those outside a narrow technical specialty to understand and critically examine the assumptions and computations of the models. In an effort to address this challenge, we present in this paper an empirical model of the US Space Shuttle orbital debris/meteoroid hazard based on empirical data and a minimum of model assumptions. Data from non-critical damage on returned Shuttle surfaces (radiators, windows, etc.) is used to quantify the probability of critical damage in a simple calculation of the relative probability that the same impact could have occurred on certain other areas of the Shuttle where the impact would have caused critical damage. These empirical results will then be compared with the results of the more sophisticated models. C1 NASA, Lyndon B Johnson Space Ctr, Orbital Debris Program Off, Houston, TX 77058 USA. RP Matney, M (reprint author), NASA, Lyndon B Johnson Space Ctr, Orbital Debris Program Off, Houston, TX 77058 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 0278-4017 BN 978-0-87703-534-3 J9 SCI TECH PY 2006 VL 112 BP 109 EP 117 PG 9 WC Engineering, Aerospace SC Engineering GA BFT95 UT WOS:000244564000010 ER PT S AU Johnson, NL AF Johnson, Nicholas L. BE Bendisch, J TI The historical effectiveness of space debris mitigation measures SO Space Debris and Space Traffic Management Symposium 2005 SE SCIENCE AND TECHNOLOGY SERIES LA English DT Proceedings Paper CT International-Academy-of-Astronautics-Space-Debris-and-Space-Traffic-Man agement Symposium held Inconjunction with 56th International Astronautical Congress CY OCT 17-21, 2005 CL Fukuoka, JAPAN SP Int Acad Astronaut Space Debris & Space Traffic Management AB Nearly a quarter century has passed since a new emphasis on space debris mitigation began, following two, nearly simultaneous seminal events: the publication of "Space Debris: An AIAA Position Paper" and the realization that numerous, intense Delta second stage fragmentations had been induced by residual propellants. Since that time the major space-faring nations of the world have adopted a wide range of debris mitigation practices which have arguably reduced the rate of growth of the debris population in Earth orbit. A study has been undertaken to quantify the likely historical effects of these debris mitigation measures on the current satellite population based upon vehicle-specific launch rates. The mitigation measures addressed in the study include those associated with mission-related debris, satellite breakups, and the disposal of satellites. Mitigation measures have been classified according to their near-term and far-term consequences and to the degree of their implementation by the international aerospace community. The history of the application of space debris mitigation measures can be used in conjunction with long-term satellite evolutionary models to provide a more realistic expectation of the future environment. C1 NASA, Lyndon B Johnson Space Ctr, Orbital Debris Program Off, Houston, TX 77058 USA. RP Johnson, NL (reprint author), NASA, Lyndon B Johnson Space Ctr, Orbital Debris Program Off, Houston, TX 77058 USA. NR 11 TC 0 Z9 0 U1 2 U2 3 PU UNIVELT INC PI SAN DIEGO PA PO BOX 28130, SAN DIEGO, CA 92128 USA SN 0278-4017 BN 978-0-87703-534-3 J9 SCI TECH PY 2006 VL 112 BP 273 EP 281 PG 9 WC Engineering, Aerospace SC Engineering GA BFT95 UT WOS:000244564000022 ER PT S 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. BE Bruce, LL Dournon, C TI Effect of simulated microgravity on oxidation-sensitive gene expression in PC12 cells SO SPACE LIFE SCIENCES 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 rotating wall vessel; simulated microgravity; gene expression; microarray ID FALSE DISCOVERY RATE; NERVE GROWTH-FACTOR; MOLECULAR MECHANISMS; MICROARRAY ANALYSIS; CDNA; HYPOXIA; CULTURE; WALL; 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, (PC12)] under simulated micro-g conditions. The PC12 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 (RWV) designed at NASA to simulate micro-g. Gene expression in PC12 cells in response to micro-g was analyzed by DNA microarray technology. The microarray analysis of PC12 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] Univ Cincinnati, Ctr Environm Genet, Dept Environm Hlth, Div Biostat & Epidemiol, Cincinnati, OH 45221 USA. [Tomlinson, Craig R.] Univ Cincinnati, Ctr Environm Genet, Dept Environm Hlth, 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, Glenn Res Ctr, Div Micrograv Sci, 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 FU NASA Glenn Research Center [NASA-GSN-6234] FX This study has been partially supported by NASA Glenn Research Center (NASA-GSN-6234). NR 39 TC 0 Z9 0 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 6 BP 1168 EP + DI 10.1016/j.asr.2006.02.059 PG 3 WC Engineering, Aerospace; Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology; Meteorology & Atmospheric Sciences GA BFV99 UT WOS:000245034100022 ER PT S 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. BE Bruce, LL Dournon, C 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 SPACE LIFE SCIENCES 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 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, Winogradsky Inst Microbiol, Pr 60 Letiya Oktyabrya 7-2, Moscow 117312, Russia. [Duxbury, N. S.] CALTECH, JPL, Pasadena, CA 91125 USA. [Bobin, N. E.] St Petersburg Min Inst, St Petersburg 199026, Russia. [Hoover, R. B.] NASA, NSSTC, Dept Space Sci, SD50, Huntsville, AL 35805 USA. [Naganuma, T.] Hiroshima Univ, Sch Biosphere Sci, Hiroshima, Japan. RP Mulyukin, AL (reprint author), Russian Acad Sci, Winogradsky Inst Microbiol, Pr 60 Letiya Oktyabrya 7-2, Moscow 117312, Russia. EM abyzov@inmi.host.ru; nduxbury@jpl.nasa.gov; fukuchi@nipr.ac.jp; Richard.Hoover@msfc.nasa.gov; andylm@rambler.ru; takn@hiroshima-u.ac.jp NR 43 TC 0 Z9 0 U1 2 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 6 BP 1191 EP + DI 10.1016/j.asr.2005.05.034 PG 3 WC Engineering, Aerospace; Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology; Meteorology & Atmospheric Sciences GA BFV99 UT WOS:000245034100025 ER PT S AU Coleman, M Rodgers, D Jones, J AF Coleman, Max Rodgers, David Jones, Jack BE Bruce, LL Dournon, C TI A buoyant life investigating mobile platform (BLIMP) SO SPACE LIFE SCIENCES 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 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] CALTECH, Jet Prop Lab, MS 180-604,4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Rodgers, D (reprint author), CALTECH, 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 OI Coleman, Max/0000-0002-5514-1826 NR 37 TC 0 Z9 0 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 6 BP 1198 EP + DI 10.1016/j.asr.2005.05.058 PG 3 WC Engineering, Aerospace; Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology; Meteorology & Atmospheric Sciences GA BFV99 UT WOS:000245034100026 ER PT S AU Wilson, JW Cucinotta, FA Golightly, M Nealy, JE Qualls, GD Badavi, FF De Angelis, G Anderson, BM Clowdsley, MS Luetke, N Zapp, N Shavers, MR Semones, E Hunter, A AF Wilson, J. W. Cucinotta, F. A. Golightly, M. J. Nealy, J. E. Qualls, G. D. Badavi, F. F. De Angelis, G. Anderson, B. M. Clowdsley, M. S. Luetke, N. Zapp, N. Shavers, M. R. Semones, E. Hunter, A. BE Heilbronn, L DeAngels, G TI International space station: A testbed for experimental and computational dosimetry SO SPACE LIFE SCIENCES: FLIGHT MEASUREMENTS, CALIBRATION OF DETECTORS AND ENVIRONMENTAL MODELS FOR RADIATION ANALYSIS 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 ISS dosimetry; model validation ID RADIATION ENVIRONMENT; TRAPPED PROTONS; SHUTTLE; SPECTRA; STS-57; BOARD; FIELD; FLUX AB The ISS and the prior station Mir provided the proving ground for future human long-duration space activity. A recent European Space Agency study recommended "Measurement campaigns on the ISS form the ideal tool for experimental validation of radiation environment models, of transport code algorithms and reaction cross sections". Indeed, prior measurements on Shuttle have provided vital information impacting both transport code and environmental model development. Recent studies using the ISS 7A configuration with TLD area monitors demonstrated that computational dosimetry requires environmental models with accurate anisotropic and dynamic behavior, detailed information on rack loading, and an accurate 6 degree-of-freedom description of the ISS trajectory. The ISS model is now configured for I I A and uses an anisotropic and dynamic geomagnetic transmission and trapped proton models. The ISS 11A is instrumented with both passive and active dosimetric devices. Time resolved measurements have the advantage of isolating trapped proton and galactic cosmic ray components as was essential to transport code validation in Shuttle data analysis. ISS I I A model validation will begin with passive dosimetry as was used with ISS 7A. Directional dependent active measurements will play an important role in the validation of environmental model anisotropies. (c) 2006 Published by Elsevier Ltd on behalf of COSPAR. C1 NASA, Langley Res Ctr, Hampton, VA 23665 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Old Dominion Univ, Norfolk, VA USA. Christopher Newport Univ, Newport News, VA 23606 USA. Swales Aerosp, Hampton, VA USA. Lockheed Martin, Houston, TX USA. Wyle Labs, Houston, TX USA. Univ Utah, Dept Mech Engn, Salt Lake City, UT 84112 USA. RP Wilson, JW (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA. EM john.w.wilson@nasa.gov NR 31 TC 22 Z9 22 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 9 BP 1656 EP 1663 DI 10.1016/j.asr.2005.02.038 PG 8 WC Engineering, Aerospace; Astronomy & Astrophysics; Biophysics; Geosciences, Multidisciplinary; Instruments & Instrumentation; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Biophysics; Geology; Instruments & Instrumentation; Meteorology & Atmospheric Sciences GA BER53 UT WOS:000239085700001 ER PT S AU Dachev, T Atwell, W Semones, E Tomov, B Reddell, B AF Dachev, Tsvetan Atwell, William Semones, Edward Tomov, Borislav Reddell, Brandon BE Heilbronn, L DeAngels, G TI Observations of the SAA radiation distribution by Liulin-E094 instrument on ISS SO SPACE LIFE SCIENCES: FLIGHT MEASUREMENTS, CALIBRATION OF DETECTORS AND ENVIRONMENTAL MODELS FOR RADIATION ANALYSIS 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 space radiation dosimetry; International Space Station; spectrometry AB Space radiation measurements were made on the International Space Station (ISS) with the Bulgarian Liulin-E094 instrument, which contains 4 Mobile Dosimetry Units (MDU), and the NASA Tissue Equivalent Proportional Counter (TEPC) during the time period May 11-July 26, 2001. In the time span 11-27 May 2001 four MDUs were placed at fixed locations: one unit (MDU #1) in the ISS "Unity" Node-1 and three (MDU #2-#4) units were located in the US Laboratory module. The MDU #2 and the TEPC were located in the US Laboratory module Human Research Facility (rack #1, port side). In this paper we discuss the flight observed asymmetries in different detectors on the ascending and descending parts of the ISS orbits. The differences are described by the shielding differences generated by different geometry between the predominating eastward drifting protons and the orientation and placement of the MDUs within the ISS. Shielding distributions were generated for the combined ISS and detector shielding models. The AP8MAX and AE8MAX trapped radiation models were used to compute the daily absorbed dose for the five detectors and are compared with the flight measurements. In addition, the trapped proton incident spectra inside of ISS were calculated using calibration curve of MDU obtained during the tests with protons at the Louvain-la-Neuve cyclotron facility. The energy of incident spectra maximums were analyzed against L value for the individual passes through the South Atlantic Anomaly. (c) 2006 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Bulgarian Acad Sci, BU-113 Sofia, Bulgaria. NASA, Boeing Co, Houston, TX 77059 USA. Lockheed Martin Engn Serv, Houston, TX 77058 USA. RP Dachev, T (reprint author), Bulgarian Acad Sci, BU-113 Sofia, Bulgaria. EM tdachev@bas.bg NR 11 TC 23 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 PY 2006 VL 37 IS 9 BP 1672 EP 1677 DI 10.1016/j.asr.2006.01.001 PG 6 WC Engineering, Aerospace; Astronomy & Astrophysics; Biophysics; Geosciences, Multidisciplinary; Instruments & Instrumentation; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Biophysics; Geology; Instruments & Instrumentation; Meteorology & Atmospheric Sciences GA BER53 UT WOS:000239085700004 ER PT S AU Johnson, AS Golightly, MJ Lin, T Semones, EJ Shelfer, T Weyland, MD Zapp, EN AF Johnson, A. S. Golightly, M. J. Lin, T. Semones, E. J. Shelfer, T. Weyland, M. D. Zapp, E. N. BE Heilbronn, L DeAngels, G TI A comparison of measurements and predictions for the April 15 and April 18, 2001 solar proton events SO SPACE LIFE SCIENCES: FLIGHT MEASUREMENTS, CALIBRATION OF DETECTORS AND ENVIRONMENTAL MODELS FOR RADIATION ANALYSIS 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 solar particle event; SPE; space station; radiation; astronaut; April 2001 ID MODEL AB Two energetic solar particle events (SPE) occurred during the week of April 15, 2001 resulting in exposure to the crew aboard the International Space Station (ISS). The radiation environment on the ISS is monitored with a tissue equivalent proportional counter (TEPC) which measures a time-resolved record of the accumulated dose and dose rate during the course of the event. In addition to TEPC measurements, the flight control radiological support team uses an in-house developed solar particle event - real time (SPERT) code to estimate the progress of crew exposures during an SPE. The TEPC measurements during these two events and corresponding calculated results from the SPERT code are compared. The timing of high dose rate intervals from SPERT is in excellent agreement with measured TEPC data. The accumulated dose and peak dose rate per pass are more difficult to assess due to uncertainties in shield distributions and directionality of the source term. However, using a standard shield file, the total accumulated exposure projected using SPERT was approximately two thirds of the total dose measured by the TEPC (900 mu G) for the April 15, 2001 and April 18, 2001 events. (c) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 NASA, Space Radiat Anal Grp, Houston, TX 77058 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Johnson, AS (reprint author), NASA, Space Radiat Anal Grp, 2400 NASA Pkwy,Mail Stop C23, Houston, TX 77058 USA. EM asjohnso@emsjsc.nasa.gov NR 12 TC 1 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 9 BP 1678 EP 1684 DI 10.1016/j.asr.2005.04.083 PG 7 WC Engineering, Aerospace; Astronomy & Astrophysics; Biophysics; Geosciences, Multidisciplinary; Instruments & Instrumentation; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Biophysics; Geology; Instruments & Instrumentation; Meteorology & Atmospheric Sciences GA BER53 UT WOS:000239085700005 ER PT S AU O'Neill, PM AF O'Neill, P. M. BE Heilbronn, L DeAngels, G TI Badhwar-O'Neill galactic cosmic ray model update based on advanced composition explorer (ACE) energy spectra from 1997 to present SO SPACE LIFE SCIENCES: FLIGHT MEASUREMENTS, CALIBRATION OF DETECTORS AND ENVIRONMENTAL MODELS FOR RADIATION ANALYSIS 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 galactic cosmic rays; solar modulation; advanced composition explorer; radiation protection; local interstellar spectra; heliosphere ID SPACE EXPLORATION; RADIATION; MODULATION AB Accurate knowledge of the interplanetary Galactic Cosmic Ray (GCR) environment is critical to planning and operating manned space flight to the moon and beyond. In the early 1990s, Badhwar and O'Neill developed a GCR model based on balloon and satellite data from 1954 to 1992. Since August 1997 the Advanced Composition Explorer (ACE) has provided significantly more accurate GCR energy spectra due to its much larger collection power. The original Badhwar-O'Neill Model, updated with the new ACE data, should provide interplanetary mission planners with highly accurate GCR environment data for radiation protection for astronauts and radiation hardness assurance for electronic equipment. Published by Elsevier Ltd on behalf of COSPAR. C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP O'Neill, PM (reprint author), NASA, Lyndon B Johnson Space Ctr, EV5,NASA Rd 1, Houston, TX 77058 USA. EM patrick.m.oneill@nasa.gov NR 16 TC 57 Z9 60 U1 1 U2 8 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 9 BP 1727 EP 1733 DI 10.1016/j.asr.2005.02.001 PG 7 WC Engineering, Aerospace; Astronomy & Astrophysics; Biophysics; Geosciences, Multidisciplinary; Instruments & Instrumentation; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Biophysics; Geology; Instruments & Instrumentation; Meteorology & Atmospheric Sciences GA BER53 UT WOS:000239085700013 ER PT S AU Kim, MY Wilson, JW Cucinotta, FA AF Kim, M. Y. Wilson, J. W. Cucinotta, F. A. BE Heilbronn, L DeAngels, G TI A solar cycle statistical model for the projection of space radiation environment SO SPACE LIFE SCIENCES: FLIGHT MEASUREMENTS, CALIBRATION OF DETECTORS AND ENVIRONMENTAL MODELS FOR RADIATION ANALYSIS 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 solar cycle; space radiation; radiation protection; statistical model; space radiation environment ID MAGNETIC-FIELD; FORECAST AB The interplanetary plasma and radiation fields are affected by the degree of disturbance in the solar surface. Sunspot number is well correlated with many observable space quantities and is used herein to represent variations in the space radiation environment. A solar cycle statistical model is developed based on the accumulating cycle sunspot data in order to estimate future levels of cycle activity. In developing the model, the odd and even cycles are treated as two independent populations. Furthermore, the rising and declining phases of each cycle are treated separately due to the randomization through the remainder of the cycle. It is shown that all the historical sunspot cycles are reasonably consistent with each respective activity level, as the cycle progresses from its solar minimum/solar maximum. The ranges of mean percentile groups containing up-to-date cycle data are calculated in order to estimate future levels of cycle activity. The resultant projection of sunspot numbers will be used to estimate future space-related quantities of interest in radiation protection. (c) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Wyle Labs, Houston, TX 77058 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Kim, MY (reprint author), Wyle Labs, HAC 37A,NASA Rd 1, Houston, TX 77058 USA. EM myung-hee.y.kim1@jsc.nasa.gov; john.w.wilson@nasa.gov; francis.a.cucinotta@nasa.gov OI Kim, Myung-Hee/0000-0001-5575-6858 NR 18 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 9 BP 1741 EP 1748 DI 10.1016/j.asr.2004.11.036 PG 8 WC Engineering, Aerospace; Astronomy & Astrophysics; Biophysics; Geosciences, Multidisciplinary; Instruments & Instrumentation; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Biophysics; Geology; Instruments & Instrumentation; Meteorology & Atmospheric Sciences GA BER53 UT WOS:000239085700015 ER PT S AU Tripathi, RK Wilson, JW Badavi, FF De Angelis, G AF Tripathi, R. K. Wilson, J. W. Badavi, F. F. De Angelis, G. BE Heilbronn, L DeAngels, G TI A characterization of the moon radiation environment for radiation analysis SO SPACE LIFE SCIENCES: FLIGHT MEASUREMENTS, CALIBRATION OF DETECTORS AND ENVIRONMENTAL MODELS FOR RADIATION ANALYSIS 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 moon radiation environment; lunar mission scenarios; galactic cosmic rays; solar particle events; HZETRN deterministic space radiation transport code ID GALACTIC COSMIC-RAYS; INTERPLANETARY SPACE AB The radiation environment found on the surface of the Moon is shown and applied to different possible lunar mission scenarios. Models for the primary particle environment to be found on the Moon due to galactic cosmic rays (GCR) and solar particle events (SPE) have been used, with solar modulation and surface backscattering patterns taken into account. The surface itself has been modeled as regolith and bedrock. Particle transport has been performed with both deterministic and Monte Carlo approaches. A good agreement is found between the two methods. (c) 2006 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. Christopher Newport Univ, Newport News, VA 23606 USA. Old Dominion Univ, Norfolk, VA 23508 USA. RP Tripathi, RK (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM r.k.tripathi@larc.nasa.gov NR 29 TC 10 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-SERIES PY 2006 VL 37 IS 9 BP 1749 EP 1758 DI 10.1016/j.asr.2006.03.016 PG 10 WC Engineering, Aerospace; Astronomy & Astrophysics; Biophysics; Geosciences, Multidisciplinary; Instruments & Instrumentation; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Biophysics; Geology; Instruments & Instrumentation; Meteorology & Atmospheric Sciences GA BER53 UT WOS:000239085700016 ER PT S AU Zhou, D O'Sullivan, D Semones, E Heinrich, W AF Zhou, D. O'Sullivan, D. Semones, E. Heinrich, W. BE Heilbronn, L DeAngels, G TI Radiation field of cosmic rays measured in low Earth orbit by CR-39 detectors SO SPACE LIFE SCIENCES: FLIGHT MEASUREMENTS, CALIBRATION OF DETECTORS AND ENVIRONMENTAL MODELS FOR RADIATION ANALYSIS 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 radiation; cosmic rays; low Earth orbit; CR-39 detectors; LET spectra; charge spectra AB In low Earth orbit astronauts are exposed to a radiation field composed of galactic cosmic rays, solar particles, particles in the Earth's radiation belts and albedo neutrons and protons from the Earth's atmosphere. Linear Energy Transfer (LET) spectra have been measured for the STS-108, STS-112 and ISS-7S missions. Measurement of the radiation fields is based on accurate measurements of recoils and fragments produced in CR-39 detectors by cosmic ray primary and secondary protons and heavier nuclei and by secondary neutrons. The measured LET spectra were used to determine the corresponding absorbed dose and dose equivalent. Total flux of Z >= 2 was estimated and a charge spectrum was measured for STS-108 and STS-112 missions. Comparisons are made with the predictions of cosmic ray transport models. (c) 2004 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 Dublin Inst Adv Studies, Dublin 2, Ireland. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Univ Siegen, Dept Phys, D-57068 Siegen, Germany. RP Zhou, D (reprint author), Dublin Inst Adv Studies, 5 Meerrion Sq, Dublin 2, Ireland. EM dz@cp.dias.ie NR 10 TC 19 Z9 19 U1 2 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 9 BP 1764 EP 1769 DI 10.1016/j.asr.2004.08.009 PG 6 WC Engineering, Aerospace; Astronomy & Astrophysics; Biophysics; Geosciences, Multidisciplinary; Instruments & Instrumentation; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Biophysics; Geology; Instruments & Instrumentation; Meteorology & Atmospheric Sciences GA BER53 UT WOS:000239085700018 ER PT S AU Kim, MHY George, KA Cucinotta, FA AF Kim, Myung-Hee Y. George, Kerry A. Cucinotta, Francis A. BE Heilbronn, L DeAngels, G TI Evaluation of skin cancer risk for lunar and Mars missions SO SPACE LIFE SCIENCES: FLIGHT MEASUREMENTS, CALIBRATION OF DETECTORS AND ENVIRONMENTAL MODELS FOR RADIATION ANALYSIS 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 space radiation; cancer risk; individual radiation sensitivity; space exploration ID RADIATION; RINGWORM; EVENTS; SCALP AB Methods used to estimate the probability of excess incidence of skin cancer from space radiation exposure must take into consideration the variability of dose to different areas of the body and the individual factors that may contribute to increased risk, including skin pigment and synergistic effects from combined ionizing and UV exposure. We have estimated the skin cancer risk for future lunar and Mars missions using: (1) the multiplicative risk model for transferring the Japanese survivor data to the US population, (2) epidemiological data for the increased risk for skin locations exposed to combined UV and ionizing radiation, and (3) models of space radiation environments, transport, and anatomical shielding for 5260 skin loci. We have estimated that the probability for increased skin cancer risk from solar particle events varies more than 10-fold depending on the individual and area of skin exposed. We show that a skin cancer risk greater than 1% could occur for astronauts with light skin and hair color following exposure to medium or large class solar particle events during future lunar base operations, or from exposure to galactic cosmic rays during Mars missions. (c) 2006 COSPAR. Published by Elsevier Ltd. All rights reserved. C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Wyle Labs, Houston, TX 77058 USA. RP Cucinotta, FA (reprint author), NASA, Lyndon B Johnson Space Ctr, SK NASA Rd 1, Houston, TX 77058 USA. EM myung-hee.y.kim@nasa.gov; kerry.a.george@nasa.gov; francis.a.cucinotta@nasa.gov RI Heilbronn, Lawrence/J-6998-2013; OI Heilbronn, Lawrence/0000-0002-8226-1057; Kim, Myung-Hee/0000-0001-5575-6858 NR 17 TC 10 Z9 11 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 9 BP 1798 EP 1803 DI 10.1016/j.asr.2006.03.032 PG 6 WC Engineering, Aerospace; Astronomy & Astrophysics; Biophysics; Geosciences, Multidisciplinary; Instruments & Instrumentation; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Biophysics; Geology; Instruments & Instrumentation; Meteorology & Atmospheric Sciences GA BER53 UT WOS:000239085700023 ER PT J AU Gardner, JP Mather, JC Clampin, M Doyon, R Greenhouse, MA Hammel, HB Hutchings, JB Jakobsen, P Lilly, SJ Long, KS Lunine, JI McCaughrean, MJ Mountain, M Nella, J Rieke, GH Rieke, MJ Rix, HW Smith, EP Sonneborn, G Stiavelli, M Stockman, HS Windhorst, RA Wright, GS AF Gardner, Jonathan P. Mather, John C. Clampin, Mark Doyon, Rene Greenhouse, Matthew A. Hammel, Heidi B. Hutchings, John B. Jakobsen, Peter Lilly, Simon J. Long, Knox S. Lunine, Jonathan I. McCaughrean, Mark J. Mountain, Matt Nella, John Rieke, George H. Rieke, Marcia J. Rix, Hans-Walter Smith, Eric P. Sonneborn, George Stiavelli, Massimo Stockman, H. S. Windhorst, Rogier A. Wright, Gillian S. TI The James Webb Space Telescope SO SPACE SCIENCE REVIEWS LA English DT Review DE galaxies : formation; infrared : general; planetary systems; space vehicles : instruments; stars : formation ID EXTRASOLAR GIANT PLANETS; INITIAL MASS FUNCTION; DIGITAL SKY SURVEY; YOUNG STELLAR OBJECTS; STAR-FORMING GALAXIES; LY-ALPHA EMITTERS; HUBBLE-DEEP-FIELD; MICROWAVE BACKGROUND POLARIZATION; INFRARED SPECTROGRAPH IRS; PROBE WMAP OBSERVATIONS AB The James Webb Space Telescope (JWST) is a large (6.6 m), cold (<50 K), infrared (IR)-optimized space observatory that will be launched early in the next decade into orbit around the second Earth-Sun Lagrange point. The observatory will have four instruments: a near-IR camera, a near-IR multiobject spectrograph, and a tunable filter imager will cover the wavelength range, 0.6 < lambda < 5.0 mu m, while the mid-IR instrument will do both imaging and spectroscopy from 5.0 < lambda < 29 mu m. The JWST science goals are divided into four themes. The key objective of The End of the Dark Ages: First Light and Reionization theme is to identify the first luminous sources to form and to determine the ionization history of the early universe. The key objective of The Assembly of Galaxies theme is to determine how galaxies and the dark matter, gas, stars, metals, morphological structures, and active nuclei within them evolved from the epoch of reionization to the present day. The key objective of The Birth of Stars and Protoplanetary Systems theme is to unravel the birth and early evolution of stars, from infall on to dust-enshrouded protostars to the genesis of planetary systems. The key objective of the Planetary Systems and the Origins of Life theme is to determine the physical and chemical properties of planetary systems including our own, and investigate the potential for the origins of life in those systems. Within these themes and objectives, we have derived representative astronomical observations. To enable these observations, JWST consists of a telescope, an instrument package, a spacecraft, and a sunshield. The telescope consists of 18 beryllium segments, some of which are deployed. The segments will be brought into optical alignment on-orbit through a process of periodic wavefront sensing and control. The instrument package contains the four science instruments and a fine guidance sensor. The spacecraft provides pointing, orbit maintenance, and communications. The sunshield provides passive thermal control. The JWST operations plan is based on that used for previous space observatories, and the majority of JWST observing time will be allocated to the international astronomical community through annual peer-reviewed proposal opportunities. C1 NASA, Goddard Space Flight Ctr, Lab Observ Cosmol, Greenbelt, MD 20771 USA. NASA, Goddard Space Flight Ctr, Lab Exoplanet & Stellar Astrophys, Greenbelt, MD 20771 USA. Univ Montreal, Dept Phys, Montreal, PQ H3C 3J7, Canada. Space Sci Inst, Boulder, CO 80301 USA. Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. European Space Agcy, Div Astrophys, RSSD, NL-2200 AG Noordwijk, Netherlands. ETH Honggerberg, Swiss Fed Inst Technol ETH Zurich, Dept Phys, CH-8093 Zurich, Switzerland. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. Astrophys Inst Potsdam, D-14482 Potsdam, Germany. Univ Exeter, Sch Phys, Exeter EX4 4QL, Devon, England. Northrop Grumman Space Technol, Redondo Beach, CA 90278 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Max Planck Inst Astron, D-69117 Heidelberg, Germany. NASA Headquarters, Washington, DC 20546 USA. Arizona State Univ, Dept Phys & Astron, Tempe, AZ 85287 USA. Royal Observ, Astron Technol Ctr, Edinburgh EH9 3HJ, Midlothian, Scotland. RP Gardner, JP (reprint author), NASA, Goddard Space Flight Ctr, Lab Observ Cosmol, Code 665, Greenbelt, MD 20771 USA. EM jonathan.p.gardner@nasa.gov RI Sonneborn, George/D-5255-2012; Clampin, mark/D-2738-2012 NR 314 TC 372 Z9 373 U1 10 U2 49 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0038-6308 EI 1572-9672 J9 SPACE SCI REV JI Space Sci. Rev. PY 2006 VL 123 IS 4 BP 485 EP 606 DI 10.1007/s11214-006-8315-7 PG 122 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 121ZB UT WOS:000243194400001 ER PT S AU Dever, JA Deshpande, MS Jaworske, DA Cerbus, CA AF Dever, JA Deshpande, MS Jaworske, DA Cerbus, CA BE ElGenk, MS TI Issues and advancements in space durable multi-functional thermal control coatings SO Space Technology and Applications International Forum - STAIF 2006 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE thermal control; spacecraft; coatings; space environment; radiation effects on materials AB Passive spacecraft thermal control coatings are required to possess properties of low solar absorptance, high thermal emittance, and stability to survive the space environment for the mission duration. The white paint coatings Z-93, YB-71 and S13G/LO, originally developed in the 1960s, have been successfully used for satellite thermal control and have served as standards for spacecraft white thermal control paints. Since their original development, these coatings have gone through re-formulations as original raw materials became unavailable; however, their replacement products continue to serve as standards for spaceflight thermal control. Unique conditions of space exploration and space science missions have required that additional functionalities be incorporated into spacecraft thermal control coatings. Coating development efforts have addressed needs for long-life stability, surface conductivity, and the ability to clean coating surfaces. Advancements in development of lightweight composite structures for spacecraft have led to the need for thermal control coatings that are adherent and compatible with these composite substrates, whereas the original formulations of white paints were developed for application to aluminum substrates. The pursuit of nuclear reactor powered spacecraft for future missions requires coating/substrate systems which are not only compatible with harsh space radiation environmental exposures, but must also perform at higher temperatures than have been previously required. Future missions to the lunar and Martian surfaces will additionally require thermal control coatings for which dust accumulation can be mitigated. Although advancements continue in the area of thermal control materials technologies, thermal control coatings are not currently commercially available to meet all of these advanced requirements. This paper presents some of the unique challenges for thermal control material systems for future space missions and some current approaches to meeting these challenges. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Dever, JA (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd,MS 309-2, Cleveland, OH 44135 USA. NR 13 TC 1 Z9 1 U1 0 U2 4 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 3 EP 10 PG 8 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600001 ER PT S AU Jaworske, DA AF Jaworske, DA BE ElGenk, MS TI Electron beam exposure of thermal control paints on carbon-carbon and carbon-polyimide composites SO Space Technology and Applications International Forum - STAIF 2006 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE solar absorptance; infrared emittance AB Carbon-carbon and carbon-polyimide composites are being considered for use as radiator face sheets or fins for space radiator applications. Several traditional white thermal control paints are being considered for the surface of the composite face sheets or fins. One threat to radiator performance is high energy electrons. The durability of the thermal control paints applied to the carbon-carbon and carbon-polyimide composites was evaluated after extended exposure to 4.5 MeV electrons. Electron exposure was conducted under argon utilizing a Mylar (TM) bag enclosure. Solar absorptance and infrared emittance was evaluated before and after exposure to identify optical properties degradation. Adhesion of the paints to the carbon-carbon and carbon-polyimide composite substrates was also of interest. Adhesion was evaluated on pristine and electron beam exposed coupons using a variation of the ASTM D-3359 tape test. Results of the optical properties evaluation and the adhesion tape tests are summarized. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Jaworske, DA (reprint author), NASA, Glenn Res Ctr, 21000 Brookpk Rd, Cleveland, OH 44135 USA. NR 4 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 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 50 EP 55 PG 6 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600007 ER PT S AU Vaughn, J Schneider, T AF Vaughn, J Schneider, T BE ElGenk, MS TI Surface power radiative cooling tests SO Space Technology and Applications International Forum - STAIF 2006 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE heat transfer; surface power radiator materials; solar energy AB Terrestrial nuclear power plants typically maintain their temperature through convective cooling, such as water and forced air. However, the space environment is a vacuum environment, typically 10(-8) Torr pressure, therefore in proposed missions to the lunar surface, power plants would have to rely on radiative cooling to remove waste heat. Also, the Martian surface has a very tenuous atmosphere (e.g. similar to 5 Torr CO2), therefore, the main heat transfer method on the Martian surface is also radiative. Because of the lack of atmosphere on the Moon and the tenuous atmosphere on Mars, surface power systems on both the Lunar and Martian surface must rely heavily on radiative heat transfer. Because of the large temperature swings on both the lunar and the Martian surfaces, trying to radiate heat is inefficient. In order to increase power system efficiency, an effort is underway to test various combinations of materials with high emissivities to demonstrate their ability to survive these degrading atmospheres to maintain a constant radiator temperature improving surface power plant efficiency. An important part of this effort is the development of a unique capability that would allow the determination of a materials emissivity at high temperatures. A description of the test capability as well as initial data is presented. C1 NASA, Marshall Space Flight Ctr, Environm Effects Branch, Huntsville, AL 35812 USA. RP Vaughn, J (reprint author), NASA, Marshall Space Flight Ctr, Environm Effects Branch, EM50, Huntsville, AL 35812 USA. NR 7 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 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 74 EP 80 PG 7 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600010 ER PT S AU Hull, PV Tinker, M SanSoucie, M Kittredge, K AF Hull, PV Tinker, M SanSoucie, M Kittredge, K BE ElGenk, MS TI Thermal analysis and shape optimization of an in-space radiator using genetic algorithms SO Space Technology and Applications International Forum - STAIF 2006 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE optimization; radiator; genetic algorithms; heat rejection ID DESIGN AB Future space exploration missions will require the development of more advanced in-space radiators. These radiators should be highly efficient and lightweight, deployable heat rejection systems. Typical radiators for in-space heat mitigation commonly comprise a substantial portion of the total vehicle mass. A small mass savings of even 5-10% can greatly improve vehicle performance. The objective of this paper is to present the development of detailed tools for the analysis and design of in-space radiators using evolutionary computation techniques. The optimality criterion is defined as a two-dimensional radiator with a shape demonstrating the smallest mass for the greatest overall heat transfer, thus the end result is a set of highly functional radiator designs. This cross-disciplinary work combines shape optimization and thermal analysis design by means of a genetic algorithm. The proposed design tool consists of the following steps; design parameterization based on the exterior boundary of the radiator, objective function definition (mass minimization and heat loss maximization), objective function evaluation via finite element analysis (thermal radiation analysis) and optimization based on evolutionary algorithms. The radiator design problem is defined as follows: the input force is a driving temperature and the output reaction is heat loss. Appropriate modeling of the space environment is added to capture its effect on the radiator. The design parameters chosen for this radiator shape optimization problem fall into two classes, variable height along the width of the radiator and a spline curve defining the material boundary of the radiator. The implementation of multiple design parameter schemes allows the user to have more confidence in the radiator optimization tool upon demonstration of convergence between the two design parameter schemes. This tool easily allows the user to manipulate the driving temperature regions thus permitting detailed design of in-space radiators for unique situations. Preliminary results indicate an optimized shape following that of the temperature distribution regions in the "cooler" portions of the radiator. The results closely follow the expected radiator shape. C1 NASA, Marshall Space Flight Ctr, Syst Anal & Integrat, Huntsville, AL 35812 USA. RP Hull, PV (reprint author), NASA, Marshall Space Flight Ctr, Syst Anal & Integrat, Huntsville, AL 35812 USA. NR 12 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 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 81 EP 90 PG 10 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600011 ER PT S AU Martin, JJ Reid, RS AF Martin, JJ Reid, RS BE ElGenk, MS TI Life test approach for refractory metal/sodium heat pipes SO Space Technology and Applications International Forum - STAIF 2006 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE nuclear; reactor cooling; heat pipe; refractory metal; alkali metal; sodium; corrosion; life test AB Heat pipe life tests described in the literature have seldom been conducted on a systematic basis. Typically one or more heat pipes are built and tested for an extended period at a single temperature with simple condenser loading. The objective of this work was to establish an approach to generate carefully controlled data that can conclusively establish heat pipe operating life with material-fluid combinations capable of extended operation. Approximately 10 years of operational life might be compressed into 3 years of laboratory testing through a combination of increased temperature and mass fluence. To accomplish this goal test series have been identified, based on American Society for Testing and Materials (ASTM) specifications, to investigate long term corrosion rates. The heat pipes selected for demonstration purposes are fabricated from a Molybdenum-44.5%Rhenium refractory metal alloy and include an internal crescent annular wick design formed by hot isostatic pressing. A processing methodology has been devised that incorporates vacuum distillation filling with an integrated purity sampling technique for the sodium working fluid. Energy is supplied by radio frequency induction coils coupled to the heat pipe evaporator with an input range of I to 5 kW per unit while a static gas gap coupled water calorimeter provides condenser cooling for heat pipe temperatures ranging from 1123 to 1323 K. The test chamber's atmosphere would require active purification to maintain low oxygen concentrations at an operating pressure of approximately 75 toff. The test is designed to operate round-the-clock with 6-month non-destructive inspection intervals to identify the onset and level of corrosion. At longer intervals specific heat pipes are destructively evaluated to verify the non-destructive observations. Accomplishments prior to project cancellation included successful demonstration of the heat pipe wick fabrication technique, establishment of all engineering designs, baselined operational test requirements and procurement/assembly of supporting test hardware systems. C1 NASA, MSFC, Huntsville, AL 35812 USA. RP Martin, JJ (reprint author), NASA, MSFC, ER11, Huntsville, AL 35812 USA. NR 11 TC 1 Z9 1 U1 1 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 108 EP 116 PG 9 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600014 ER PT S AU Rowden, BL Selvam, RP Silk, EA AF Rowden, BL Selvam, RP Silk, EA BE ElGenk, MS TI Spray cooling development effort for microgravity environments SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM - STAIF 2006 SE AIP Conference Proceedings LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE spray cooling; high heat fluxes; microgravity environments ID BOILING HEAT-TRANSFER AB Spray cooling is a high heat flux removal technique considered for systems such as advanced lasers and high power density electronics. Several experiments have been conducted using spray cooling in recent years and various designs of spray cooling devices are continually emerging. At this time, one of NASA's missions is to enhance future space science capabilities through the application of power lasers and electronics. However, the usage of systems having high heat fluxes can only be achieved with the corresponding development of high power thermal control systems. For the reliable performance of these high-heat-flux systems, proper thermal management is imperative. The study presented reviews the fabrication of a spray cooling system aimed at addressing issues pertinent to space applications. These issues include heat flux capability, orientation, and volumetric packaging. Computer modeling of spray cooling under microgravity conditions as well as comparison to the analogous 1-g condition was also performed to gain insight into microgravity behavior. C1 Power Elect Leveling Solut, 700 W Res Ctr Blvd, Fayetteville, AR 72701 USA. Univ Arkansas, BELL 4190, Fayetteville, AR 72701 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Power Elect Leveling Solut, 700 W Res Ctr Blvd, Fayetteville, AR 72701 USA. EM klrbee@cox.net RI selvam, Rathinam/H-7849-2013 NR 14 TC 4 Z9 4 U1 1 U2 2 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 134 EP + PG 2 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600017 ER PT S AU Abelson, RD Spilker, TR Shirley, JH AF Abelson, RD Spilker, TR Shirley, JH BE ElGenk, MS TI A Saturn Ring Observer mission using multi-mission radioisotope power systems SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM - STAIF 2006 SE AIP Conference Proceedings LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE RPS; radioisotope power system; MMRTG; SRG; Saturn; rings; orbiter; SRO AB Saturn remains one of the most fascinating planets within the solar system. To better understand the complex ring structure of this planet, a conceptual Saturn Ring Observer (SRO) mission is presented that would spend one year in close proximity to Saturn's A and B rings, and perform detailed observations and measurements of the ring particles and electric and magnetic fields. The primary objective of the mission would be to understand ring dynamics, including the microphysics of individual particles and small scale (meters to a few kilometers) phenomena such as particle agglomeration behavior. This would be accomplished by multispectral imaging of the rings at multiple key locations within the A and B rings, and by ring-particle imaging at an unprecedented resolution of 0.5 cm/pixel. The SRO spacecraft would use a Venus-Earth-Earth-Jupiter Gravity Assist (VEEJGA) and be aerocaptured into Saturn orbit using an advanced aeroshell design to minimize propellant mass. Once in orbit, the SRO would stand off from the ring plane 1 to 1.4 km using chemical thrusters to provide short propulsive maneuvers four times per revolution, effectively causing the SRO vehicle to "hop" above the ring plane. The conceptual SRO spacecraft would be enabled by the use of a new generation of multi-mission Radioisotope Power Systems (RPSs) currently being developed by NASA and DOE. These RPSs include the Multi-Mission Radioisotope Thermoelectric Generator (MMRTG) and Stirling Radioisotope Generator (SRG). The RPSs would generate all necessary electrical power ( 330 W, at beginning of life) during the 10-year cruise and 1-year science mission (similar to 11 years total). The RPS heat would be used to maintain the vehicle's operating and survival temperatures, minimizing the need for electrical heaters. Such a mission could potentially launch in the 2015-2020 timeframe, with operations at Saturn commencing in approximately 2030. C1 CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 301-455W, Pasadena, CA 91109 USA. RP CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 301-455W, Pasadena, CA 91109 USA. EM Robert.D.Ahelson@jpl.nasa.gov 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 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 155 EP + PG 2 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600019 ER PT S AU Chowdhury, BH Hossain, SA Lawrence, JT Barave, S AF Chowdhury, BH Hossain, SA Lawrence, JT Barave, S BE ElGenk, MS TI AC/DC power systems with applications in future human habitat on Lunar and Mars bases SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM - STAIF 2006 SE AIP Conference Proceedings LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE crew exploration vehicle; high frequency power generation; permanent magnet synchronous machine. ID PERMANENT-MAGNET MACHINES; FLUX AB As NASA readies itself for new space exploration initiatives starting with a human return to the Moon by the year 2020 eventually leading to human exploration of Mars, the requirements for a safe, efficient and comprehensive power system to support the exploration missions as well human habitat will become important issues to consider. Certain issues dealing with electric power generation and distribution on board Mars-bound vehicles and those on Lunar and Martian surfaces are described. The requirements for lightweight power generation dictates the use of a high frequency ac machine. Preliminary results of investigating the design of a permanent magnet synchronous machine is presented. C1 Univ Missouri, Dept Elect & Comp Engn, Rolla, MO 65409 USA. NASA, Johnson Space Ctr, Div Energy Syst EP5, ISS Elect Power Syst Team, Houston, TX 77058 USA. RP Univ Missouri, Dept Elect & Comp Engn, Rolla, MO 65409 USA. EM bchow@umr.edu FU NASA Johnson Space Center and the American Society of Engineering Education FX This work was supported in part by the NASA Johnson Space Center and the American Society of Engineering Education. NR 14 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 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 193 EP + PG 2 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600023 ER PT S AU Gilland, J McGuire, M Corle, T Clem, M AF Gilland, J McGuire, M Corle, T Clem, M BE ElGenk, MS TI Mission performance of high-power electromagnetic thruster systems SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM - STAIF 2006 SE AIP Conference Proceedings LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE electric propulsion; MPD; PIT; plasma propulsion; Nuclear Electric Propulsion; NEP AB Electromagnetic thrusters such as the Magnetoplasmadynamic (MPD) thruster and Pulsed Inductive Thruster provide the relatively unique capability to process megawatts (MW) of power compactly at specific impulses (I-sp) of 2,000 to 10,000 seconds. This capability is well suited to demanding future missions such as cargo and piloted missions to Mars, in which large payload masses or short trip times require MW power levels. These two thrusters have been modeled at both the performance and system mass level, addressing thruster efficiency, I-sp, voltage and current, and the mass of thrusters as well as their corresponding heat rejection and power processing subsystems. The resulting data have been assessed for representative Mars exploration missions using detailed low thrust trajectory codes in conjunction with the thruster system models. Analyses indicate that the thruster type and technology levels have less impact on overall mission performance than the total power level. For the 2.5 and 5 MW cases considered, the lower power delivered 50% more payload. C1 Ohio Aerosp Inst, 22800 Cedar Point Rd, Brookpark, OH 44142 USA. NASA, Glenn Res Ctr, Cleveland, OH USA. RP Ohio Aerosp Inst, 22800 Cedar Point Rd, Brookpark, OH 44142 USA. EM james.h.gilland@nasa.gov NR 7 TC 0 Z9 0 U1 1 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 201 EP + PG 2 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600024 ER PT S AU Luo, N Mileyl, GH Mather, J Burton, R Hawkins, G Gimlin, R Rusek, J Valdez, TI Narayanan, SR AF Luo, N Mileyl, GH Mather, J Burton, R Hawkins, G Gimlin, R Rusek, J Valdez, TI Narayanan, SR BE ElGenk, MS TI NaBH4/H2O2 fuel cells for Lunar and Mars exploration SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM - STAIF 2006 SE AIP Conference Proceedings LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE fuel cell; hydrogen peroxide; sodium borohydride; proton exchange membrane; Lunar rover; Mars AB The properties of direct hydrogen peroxide (H2O2) fuel cells are studied in this research. Different catalysts and diffusion electrodes are tested to optimize the cell performance. Initial results indicate: 1) conversion efficiency over 60% at a practical current density of 250 mA/cm(2); 2) power density over 0.6 W/cm(2), at room temperature and ambient pressure, better than that of any traditional fuel cell. Further, the unique combination of NaBH4 and H2O2, both of which are in an aqueous form, paves the way for a convenient unitized regeneration, which is inherently compact compared to other cells that use gas phase reactants, such as the conventional H-2 and O-2. These excellent properties make the NaBH4/H2O2 fuel cell a very promising candidate for future space power systems. A conceptual design to power Lunar and Mars missions is discussed. C1 Univ Illinois, Dept Nucl Plasma & Radiol Engn, Urbana, IL 61801 USA. Univ Illinois, Dept Mech Engn, Urbana, IL 61801 USA. Univ Illinois, Dept Aerosp Engn, Urbana, IL 61801 USA. Swift Enterprises Ltd, W Lafayette, IN 47906 USA. Jet Prop Lab, Pasadena, CA 91109 USA. RP Univ Illinois, Dept Nucl Plasma & Radiol Engn, Urbana, IL 61801 USA. EM nluo@uiuc.edu NR 15 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 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 209 EP + PG 2 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600025 ER PT S AU McGuire, ML Martini, MC Packard, TW Weglian, JE Gilland, JH AF McGuire, ML Martini, MC Packard, TW Weglian, JE Gilland, JH BE ElGenk, MS TI Use of high-power Brayton nuclear electric propulsion (NEP) for a 2003 Mras round-trip mission SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM - STAIF 2006 SE AIP Conference Proceedings LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE NEP; MPD; Mars; RASC; NASA; magnetoplasmadynamic; Brayton ID CALLISTO AB The Revolutionary Aerospace Systems Concepts (RASC) team, led by the NASA Langley Research Center, is tasked with exploring revolutionary new approaches to enabling NASA to achieve its strategic goals and objectives in future missions. This paper provides the details from the 2004-2005 RASC study of a point-design that uses a high-power nuclear electric propulsion (NEP) based space transportation architecture to support a manned mission to Mars. The study assumes a high-temperature liquid-metal cooled fission reactor with a Brayton power conversion system to generate the electrical power required by magnetoplasmadynamic (MPD) thrusters. The architecture includes a cargo vehicle with an NEP system providing 5 MW of electrical power and a crewed vehicle with an NEP system with two reactors providing a combined total of 10 MW of electrical power. Both vehicles use a low-thrust, high-efficiency (5000 see specific impulse) MPD system to conduct a spiral-out of the Earth gravity well, a low-thrust heliocentric trajectory, and a spiral-in at Mars with arrival late in 2033. The cargo vehicle carries two moon landers to Mars and arrives shortly before the crewed vehicle. The crewed vehicle and cargo vehicle rendezvous in Mars orbit and, over the course of the 60-day stay, the crew conducts nine-day excursions to Phobos and Deimos with the landers. The crewed vehicle then spirals out of Martian orbit and returns via a low-thrust trajectory to conduct an Earth flyby. The crew separates from the vehicle prior to Earth flyby and aerobrakes for a direct-entry landing. C1 NASA, Glenn Res Ctr, Space Propuls & Miss Anal Off, Code PMB,MS 500-103,21000 Brookpk Rd, Cleveland, OH 44135 USA. Analex Corp, Brookpark, OH 44142 USA. Ohio Aerosp Inst, Brookpark, OH 44142 USA. RP NASA, Glenn Res Ctr, Space Propuls & Miss Anal Off, Code PMB,MS 500-103,21000 Brookpk Rd, Cleveland, OH 44135 USA. EM Melissa.L.Mcguire@nasa.gov NR 7 TC 0 Z9 0 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 222 EP + PG 2 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600026 ER PT S AU Houts, MG Schmidt, GR Bragg-Sitton, S Hickman, R Hissam, A Houston, V Martin, J Mireles, O Poston, D Reid, B Schneider, T Stewart, E Turpin, J Van Dyke, M Vaughn, J Wagner, D AF Houts, MG Schmidt, GR Bragg-Sitton, S Hickman, R Hissam, A Houston, V Martin, J Mireles, O Poston, D Reid, B Schneider, T Stewart, E Turpin, J Van Dyke, M Vaughn, J Wagner, D BE ElGenk, MS TI Integration and utilization of nuclear systems on the moon and Mars SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM - STAIF 2006 SE AIP Conference Proceedings LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE space; nuclear; fission; planetary; surface AB Over the past five decades numerous studies have identified nuclear energy as an enhancing or enabling technology for planetary surface exploration missions. This includes both radioisotope and fission sources for providing both heat and electricity. Nuclear energy sources were used to provide electricity on Apollo missions 12, 14, 15, 16, and 17, and on the Mars Viking landers. Very small nuclear energy sources were used to provide heat on the Mars Pathfinder, Spirit, and Opportunity rovers. Research has been performed at NASA MSFC to help assess potential issues associated with surface nuclear energy sources, and to generate data that could be useful to a future program. Research areas include System Integration, use of Regolith as Radiation Shielding, Waste Heat Rejection, Surface Environmental Effects on the Integrated System, Thermal Simulators, Surface System Integration/Interface/Interaction Testing, End-to-End Breadboard Development, Advanced Materials Development, Surface Energy Source Coolants, and Planetary Surface System Thermal Management and Control. This paper provides a status update on several of these research areas. C1 NASA, Marshall Space Flight Ctr, Nucl Syst Off, NP50, Huntsville, AL 35812 USA. RP NASA, Marshall Space Flight Ctr, Nucl Syst Off, NP50, Huntsville, AL 35812 USA. EM michael.g.houts@nasa.gov NR 9 TC 3 Z9 3 U1 2 U2 2 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 262 EP + PG 2 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600030 ER PT S AU Mason, LS AF Mason, LS BE ElGenk, MS TI A comparison of fission power system options for lunar and Mars surface applications SO Space Technology and Applications International Forum - STAIF 2006 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE fission power; lunar and Mars surface power; space reactors; Brayton; Stirling; thermoelectric AB This paper presents a comparison of reactor and power conversion design options for 50 kWe class lunar and Mars surface power applications with scaling from 25 to 200 kWe. Design concepts and integration approaches are provided for three reactor-converter combinations: gas-cooled Brayton, liquid-metal Stirling, and liquid-metal thermoelectric. The study examines the mass and performance of low temperature, stainless steel based reactors and higher temperature refractory reactors. The preferred system implementation approach uses crew-assisted assembly and in-situ radiation shielding via installation of the reactor in an excavated hole. As an alternative, self-deployable system concepts that use earth-delivered, on-board radiation shielding are evaluated. The analyses indicate that among the 50 kWe stainless steel reactor options, the liquid-metal Stirling system provides the lowest mass at about 5300 kg followed by the gas-cooled Brayton at 5700 kg and the liquid-metal thermoelectric at 8400 kg. The use of a higher temperature, refractory reactor favors the gas-cooled Brayton option with a system mass of about 4200 kg as compared to the Stirling and thermoelectric options at 4700 kg and 5600 kg, respectively. The self-deployed concepts with on-board shielding result in a factor of two system mass increase as compared to the in-situ shielded concepts. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Mason, LS (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. NR 15 TC 6 Z9 6 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 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 270 EP 280 PG 11 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600031 ER PT S AU Balint, TS Emis, ND AF Balint, TS Emis, ND BE ElGenk, MS TI validation database based thermal analysis of an advanced rps. SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM - STAIF 2006 SE AIP Conference Proceedings LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE RPS; ARPS; ARTG; small RPS; thermal analysis; numerical model; validation AB Advanced RPS concepts can be conceived, designed and performance of these models, but verification tools. These predictions may provide an initial insight into the potential and validation are necessary and required steps to gain confidence in the numerical analysis results. This paper discusses the findings from a numerical validation exercise for a small advanced RPS concept, based on a thermal analysis methodology developed at JPL and on a validation database obtained from experiments performed at Oregon State University. Both the numerical and experimental configurations utilized a single GPHS module enabled design, resembling a Mod-RTG concept. The analysis focused on operating and environmental conditions during the storage phase only. This validation exercise helped to refine key thermal analysis and modeling parameters, such as heat transfer coefficients, and conductivity and radiation heat transfer values. Improved understanding of the Mod-RTG concept through validation of the thermal model allows for future improvements to this power system concept. 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 tibor.balint@jpl.nasa.gov 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 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 327 EP + PG 2 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600037 ER PT S AU Schmidt, GR Houts, MG AF Schmidt, GR Houts, MG BE ElGenk, MS TI Radioisotope-based nuclear power strategy for exploration systems development SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM - STAIF 2006 SE AIP Conference Proceedings LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE radioisotope; reactor; space nuclear power; space exploration AB Nuclear power will play an important role in future exploration efforts. Its benefits pertain to practically all the different timeframes associated with the Exploration Vision, from robotic investigation of potential lunar landing sites to long-duration crewed missions on the lunar surface. However, the implementation of nuclear technology must follow a logical progression in capability that meets but does not overwhelm the power requirements for the missions in each exploration timeframe. It is likely that the surface power infrastructure, particularly for early missions, will be distributed in nature. Thus, nuclear sources will have to operate in concert with other types of power and energy storage systems, and must mesh well with the power architectures envisioned for each mission phase. Most importantly, they must demonstrate a clear advantage over other non-nuclear options (e.g., solar power, fuel cells) for their particular function. This paper describes a strategy that does this in the form of three sequential system developments. It begins with use of radioisotope generators currently under development, and applies the power conversion technology developed for these units to the design of a simple, robust reactor power system. The products from these development efforts would eventually serve as the foundation for application of nuclear power systems for exploration of Mars and beyond. C1 NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. EM George.Schmidt@nasa.gov NR 4 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 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 334 EP + PG 2 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600038 ER PT S AU Wong, WA Anderson, DJ Tuttle, KL Tew, RC AF Wong, WA Anderson, DJ Tuttle, KL Tew, RC BE ElGenk, MS TI Status of NASA's advanced radioisotope power conversion technology research and development SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM - STAIF 2006 SE AIP Conference Proceedings LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE radioisotope; power; RPS; energy conversion; Stirling; thermoelectric; regenerator ID GENERATORS AB NASA's Advanced Radioisotope Power Systems (RPS) development program is funding the advancement of next generation power conversion technologies that will enable future missions that have requirements that can not be met by either the ubiquitous photovoltaic systems or by current Radioisotope Power Systems (RPS). Requirements of advanced radioisotope power systems include high efficiency and high specific power (watts/kilogram) in order to meet mission requirements with less radioisotope fuel and lower mass. Other Advanced RPS development goals include long-life, reliability, and scalability so that these systems can meet requirements for a variety of future space applications including continual operation surface missions, outer-planetary missions, and solar probe. This paper provides an update on the Radioisotope Power Conversion Technology Project which awarded ten Phase I contracts for research and development of a variety of power conversion technologies consisting of Brayton, Stirling, thermoelectrics, and thermophotovoltaics. Three of the contracts continue during the current Phase II in the areas of thermoelectric and Stirling power conversion. The accomplishments to date of the contractors, project plans, and status will be summarized. C1 NASA, Glenn Res Ctr, Thermal Energy Convers Branch, 21000 Brookpk Rd, Cleveland, OH 44135 USA. NASA, Glenn Res Ctr, Div Sci, Cleveland, OH 44135 USA. RP NASA, Glenn Res Ctr, Thermal Energy Convers Branch, 21000 Brookpk Rd, Cleveland, OH 44135 USA. EM Wayne.A.Wong@nasa.gov FU National Aeronautics and Space Administration (NASA) under the Radioisotope Power Conversion Technology NASA Research Announcement [NRA 02-OSS-01] FX The results and findings presented here are based on work funded by the National Aeronautics and Space Administration (NASA) under the Radioisotope Power Conversion Technology NASA Research Announcement NRA 02-OSS-01 issued through the Science Mission Directorate. The authors acknowledge the technical achievements by the respective contractor teams, and the contributions of the NASA contract and technical monitors. Any opinions expressed are those of the authors and do not necessarily reflect the views of NASA. NR 11 TC 6 Z9 6 U1 1 U2 3 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 340 EP + PG 2 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600039 ER PT S AU Woods, BG Arnold, LC Balint, TS AF Woods, BG Arnold, LC Balint, TS BE ElGenk, MS TI Thermal analysis and testing of a small radioisotope power system concept SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM - STAIF 2006 SE AIP Conference Proceedings LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE radioisotope thermoelectric; static energy conversion; thermal radiation AB Oregon State University (OSU) is conducting an experimental study into the thermal behavior of a GPHS based small RPS concept. The subject RPS configuration is applicable for a number of Mars surface missions, such as using them to power small rovers and small static landers. Each module will use a single GPHS module to generate about 20-25W of electric power. Initial designs for similar RPS concepts have been completed and initial numerical analysis models have been developed by NASA's JPL. The primary purpose of this research project is to develop an experimental model of the GPHS module based small RPS concept and generate operational data that can be used to validate the thermal analysis codes and methodologies. The validation of codes and methodologies is to be completed by JPL. Five mission phases have been identified for the subject RPS concept. This experimental program focuses on one of these mission phases, earth storage. This paper addresses model design, construction, and testing. C1 Oregon State Univ, Dept Nucl Engn & Radiat Hlth Phys, Corvallis, OR 97330 USA. CALTECH, Jet Prop Lab, Deep Space Mission Architecture, Pasadena, CA 91109 USA. RP Oregon State Univ, Dept Nucl Engn & Radiat Hlth Phys, Corvallis, OR 97330 USA. EM woodsb@ne.orst.edu NR 4 TC 0 Z9 0 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 348 EP + PG 2 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600040 ER PT S AU Abelson, RD Spilker, TR Shirley, JH AF Abelson, RD Spilker, TR Shirley, JH BE ElGenk, MS TI A conceptual Titan orbiter with probe mission using advanced radioisotope power systems SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM - STAIF 2006 SE AIP Conference Proceedings LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE RPS; radioisotope power system; Titan; orbiter; RTG; Stirling; Brayton; TPV AB With the remarkable success of the Cassini-Huygens mission, considerable new knowledge has been obtained regarding the surface topography, composition and atmospheric characteristics of Titan. However, Cassini-Huygens represents only a bold beginning for the exploration of Titan, as high resolution mapping will have been performed for only a small fraction of the surface of Titan by the end of the nominal mission. Large gaps in knowledge will remain in key scientific areas including global surface topography, atmospheric and surface composition, precipitation rates, and the density, thickness, and formation processes of clouds. This study details a conceptual follow-on Titan orbiter mission that would provide full global topographic coverage, surface imaging, and meteorological characterization of the atmosphere over a nominal 2-year science mission duration. The reference power requirement is similar to 1 kW(e) at EOM and is driven by a high power radar instrument that would provide 3-dimensional measurements of atmospheric clouds, precipitation, and surface topography. While this power level is moderately higher than that of the Cassini spacecraft, higher efficiency advanced RPSs could potentially reduce the plutonium usage to less than 1/3 of that used on the Cassini spacecraft. The Titan Orbiter mission is assumed to launch in 2015. It would utilize advanced RPSs to provide all on-board power, and would employ an aeroshell to aerocapture into Titan orbit. A conceptual advanced Stirling RPS was selected due to its high specific power and conversion efficiency which enabled the ability to include a 500 kg "black box" deployed entry probe. C1 CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 301-445W, Pasadena, CA 91109 USA. RP CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,Mail Stop 301-445W, Pasadena, CA 91109 USA. EM Robert.D.Abelson@jpl.nasa.gov FU National Aeronautics and Space Administration FX The work described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. The authors wish to acknowledge the effotts and contributions of JPL Team-A, Eastwood Im, Stephen Durden, and Bill Nesmith. NR 6 TC 1 Z9 1 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 356 EP + PG 2 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600041 ER PT S AU Balint, TS Schriener, TM Shirley, JH AF Balint, TS Schriener, TM Shirley, JH BE ElGenk, MS TI Advanced radioisotope power system enabled Titan rover concept with inflatable wheels SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM - STAIF 2006 SE AIP Conference Proceedings LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE RPS; ARPS; ARTG; advanced-Stirling; TPV; Brayton; rover; inflatable wheel AB The Decadal Survey identified Titan as one of the top priority science destinations in the large moons category, while NASA's proposed Design Reference Mission Set ranked a Titan in-situ explorer second, after a recommended Europa Geophysical Explorer mission. This paper discusses a Titan rover concept, enabled by a single advanced Radioisotope Power System that could provide about 110 We (BOL). The concept targets the smaller Flagship or potentially the New Frontiers mission class. This MSL class rover would traverse on four 1.5 in diameter inflatable wheels during its 3 years mission duration and would use as much design and flight heritage as possible to reduce mission cost. Direct to Earth communication would remove the need for a relay orbiter. Details on the strawman instrument payload, and rover subsystems are given for this science driven mission concept. In addition, power system trades between Advanced RTG, TPV, and Advanced-Stirling and Brayton RPSs are outlined. While many possible approaches exist for Titan in-situ exploration, the Titan rover concept presented here could provide a scientifically interesting and programmatically affordable solution. C1 CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. Oregon State Univ, Corvallis, OR USA. RP CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM tibor.balint@jpl.nasa.gov FU JPL's Nuclear Systems and Technology Office FX The authors of this paper wish to thank members of Team P under JPL's Team of Teams for their contribution to this study. The design team included Wayne Zimmerman, Bob Kinsey, Vince Randolph, Mike Henry, Jay Whitacre, Gerhard Klose, Andy Etters, Tracy Leavens, Bob Miyake, David Morabito and Kyle Smith. The study was funded by JPL's Nuclear Systems and Technology Office, managed by Jacklyn Green. Further details on this and other advanced RPS enabled studies can be found in (Abelson et al, 2005). The work was performed at the Jet Propulsion Laboratory, California Institute of Technology. The opinions expressed in the paper are those of the authors of this paper alone and do not reflect official NASA policy NR 7 TC 0 Z9 0 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 364 EP + PG 2 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600042 ER PT S AU Evans, M Shirley, JH Abelson, RD AF Evans, M Shirley, JH Abelson, RD BE ElGenk, MS TI A conceptual Venus rover mission using advanced radioisotope power systems SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM - STAIF 2006 SE AIP Conference Proceedings LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE Venus; rover; TASHE; Stirling; thermoacoustic; radioisotope power; RPS AB This concept study demonstrates that a long lived Venus rover mission could be enabled by a novel application of advanced RPS technology. General Purpose Heat Source (GPHS) modules would be employed to drive an advanced thermoacoustic Stirling engine, pulse tube cooler and linear alternator that provides electric power and cooling for the rover. The Thermoacoustic Stirling Heat Engine (TASHE) is a system for converting high-temperature heat into acoustic power which then drives linear alternators and a pulse tube cooler to provide both electric power and cooling for the rover. A small design team examined this mission concept focusing on the feasibility of using the TASHE system in this hostile environment. A rover design is described that would provide a mobile platform for science measurements on the Venus surface for 60 days, with the potential of operating well beyond that. A suite of science instruments is described that collects data on atmospheric and surface composition, surface stratigraphy, and subsurface structure. An Earth-Venus-Venus trajectory would be used to deliver the rover to a low entry angle allowing an inflated ballute to provide a low deceleration and low heat descent to the surface. All rover systems would be housed in a pressure vessel in vacuum with the internal temperature maintained by the TASHE at under 50 degrees C. C1 CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 301-260, Pasadena, CA 91109 USA. RP CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,M-S 301-260, Pasadena, CA 91109 USA. EM michael.evans@jpl.nasa.gov NR 5 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 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 376 EP + PG 2 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600043 ER PT S AU Determan, W Frye, P Mondt, J Fleurial, JP Johnson, K Stapfer, G Brooks, M Heshmatpour, B AF Determan, W Frye, P Mondt, J Fleurial, JP Johnson, K Stapfer, G Brooks, M Heshmatpour, B BE ElGenk, MS TI Lunar base thermoelectric power station study SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM - STAIF 2006 SE AIP Conference Proceedings LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE lunar; surface; power; thermoelectric; reactor AB Under NASA's Project Prometheus, the Nuclear Space Power Systems Program, the Jet Propulsion Laboratory, Pratt & Whitney Rocketdyne, and Teledyne Energy Systems have teamed with a number of universities, under the Segmented Thermoelectric Multicouple Converter (STMC) Task, to develop the next generation of advanced thermoelectric converters for space reactor power systems. Work on the STMC converter assembly has progressed to the point where the lower temperature stage of the segmented multicouple converter assembly is ready for laboratory testing, and promising candidates for the upper stage materials have been identified and their properties are being characterized. One aspect of the program involves mission application studies to help define the potential benefits from the use of these STMC technologies for designated NASA missions such as a lunar base power station where kilowatts of power would be required to maintain a permanent manned presence on the surface of the moon. A modular 50 kWe thermoelectric power station concept was developed to address a specific set of requirements developed for this particular mission concept. Previous lunar lander concepts had proposed the use of lunar regolith as in-situ radiation shielding material for a reactor power station with a one kilometer exclusion zone radius to minimize astronaut radiation dose rate levels. In the present concept, we will examine the benefits and requirements for a hermetically-sealed reactor thermoelectric power station module suspended within a man-made lunar surface cavity. The concept appears to maximize the shielding capabilities of the lunar regolith while minimizing its handling requirements. Both thermal and nuclear radiation levels from operation of the station, at its 100-m exclusion zone radius, were evaluated and found to be acceptable. Site preparation activities are reviewed as well as transport issues for this concept. The goal of the study was to review the entire life cycle of the unit to assess its technical problems and technology needs in all areas to support the development, deployment, operation and disposal of the unit. C1 CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. Pratt & Whitney Rocketdyne Inc, Canoga Pk, CA 91309 USA. Teledyne Energy Syst Inc, Hunt Valley, MD 21031 USA. RP CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM william.r.determan@boeing.com NR 5 TC 1 Z9 1 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 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 384 EP + PG 2 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600044 ER PT S AU Bragg-Sitton, SM Morton, TJ AF Bragg-Sitton, SM Morton, TJ BE ElGenk, MS TI Dynamic response testing in an electrically heated reactor test facility SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM - STAIF 2006 SE AIP Conference Proceedings LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE non-nuclear testing; reactivity feedback; dynamic simulation ID GAS-COOLED REACTOR; PROPULSION; SUPPORT; SYSTEM; DESIGN AB Non-nuclear testing can be a valuable tool in the development of a space nuclear power or propulsion system. In a non-nuclear test bed, electric heaters are used to simulate the heat from nuclear fuel. Standard testing allows one to fully assess thermal, heat transfer, and stress related attributes of a given system, but fails to demonstrate the dynamic response that would be present in an integrated, fueled reactor system. The integration of thermal hydraulic hardware tests with simulated neutronic response provides a bridge between electrically heated testing and fueled nuclear testing. By implementing a neutronic response model to simulate the dynamic response that would be expected in a fueled reactor system, one can better understand system integration issues, characterize integrated system response times and response characteristics, and assess potential design improvements at a relatively small fiscal investment. Initial system dynamic response testing was demonstrated on the integrated SAFE-100a heat pipe (HP) cooled, electrically heated reactor and heat exchanger hardware, utilizing a one-group solution to the point kinetics equations to simulate the expected neutronic response of the system. Reactivity feedback calculations were then based on a bulk reactivity feedback coefficient and measured average core temperature. This paper presents preliminary results from similar dynamic testing of a direct drive gas cooled reactor system (DDG), demonstrating the applicability of the testing methodology to any reactor type and demonstrating the variation in system response characteristics in different reactor concepts. Although the HP and DDG designs both utilize a fast spectrum reactor, the method of cooling the reactor differs significantly, leading to a variable system response that can be demonstrated and assessed in a non-nuclear test facility. Planned system upgrades to allow implementation of higher fidelity dynamic testing are also discussed. Proposed DDG testing will utilize a higher fidelity point kinetics model to control core power transients, and reactivity feedback will be based on localized feedback coefficients and several independent temperature measurements taken within the core block. This paper presents preliminary test results and discusses the methodology that will be implemented in follow-on DDG testing and the additional instrumentation required to implement high fidelity dynamic testing. C1 NASA, George C Marshall Space Flight Ctr, Nucl & Adv Prop Branch, MSFC, ER-11, Huntsville, AL 35812 USA. Univ New Mexico, Dept Chem & Nucl Engn, Albuquerque, NM 87131 USA. RP NASA, George C Marshall Space Flight Ctr, Nucl & Adv Prop Branch, MSFC, ER-11, Huntsville, AL 35812 USA. EM Shannon.M.Bragg-Sitton@nasa.gov FU NASA's FX NASAs Project Prometheus supported the work described within this paper, in whole or part, as part of the programs technology development and evaluation activities. Any opinions expressed are those of the author and do not necessarily reflect the views of Project Prometheus. NR 16 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 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 396 EP + PG 2 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600045 ER PT S AU Godfroy, T Garber, A Martin, J AF Godfroy, T Garber, A Martin, J BE ElGenk, MS TI Lithium circuit test section design and fabrication SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM - STAIF 2006 SE AIP Conference Proceedings LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE lithium; EFF-TF; liquid metal; pumped circuit AB The Early Flight Fission - Test Facilities (EFF-TF) team has designed and built an actively pumped lithium flow circuit. Modifications were made to a circuit originally designed for NaK to enable the use of lithium that included application specific instrumentation and hardware. Component scale freeze/thaw tests were conducted to both gain experience with handling and behavior of lithium in solid and liquid form and to supply anchor data for a Generalized Fluid System Simulation Program (GFSSP) model that was modified to include the physics for freeze/thaw transitions. Void formation was investigated. The basic circuit components include: reactor segment, lithium to gas heat exchanger, electromagnetic (EM) liquid metal pump, load/drain reservoir, expansion reservoir, instrumentation, and trace heaters. This paper discusses the overall system design and build and the component testing findings. C1 NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. EM Thomas.Godfroy@nasa.gov 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 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 408 EP + PG 2 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600046 ER PT S AU Fensin, ML Elliott, JO Lipinski, RJ Poston, DI AF Fensin, ML Elliott, JO Lipinski, RJ Poston, DI BE ElGenk, MS TI Radiation shielding design and orientation considerations for a 1 kWe heat pipe cooled reactor utilized to bore through the ice caps of Mars SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM - STAIF 2006 SE AIP Conference Proceedings LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE cryobot; Mars; surface power; uranium nitride; heat pipe AB The goal in designing any space power system is to develop a system able to meet the mission requirements for success while minimizing the overall costs. The mission requirements for the this study was to develop a reactor (with Stirling engine power conversion) and shielding configuration able to fit, along with all the other necessary science equipment, in a Cryobot 3 in high with similar to 0.5 in diameter hull, produce 1 kWe for 5yrs, and not adversely affect the mission science by keeping the total integrated dose to the science equipment below 150 krad. Since in most space power missions the overall system mass dictates the mission cost, the shielding designs in this study incorporated Martian water extracted at the startup site in order to minimize the tungsten and LiH mass loading at launch. Different reliability and mass minimization concerns led to three design configuration evolutions. With the help of implementing Martian water and configuring the reactor as far from the science equipment as possible, the needed tungsten and LiH shield mass was minimized. This study further characterizes the startup dose and the necessary mission requirements in order to ensure integrity of the surface equipment during reactor startup phase. C1 Univ Florida, Dept Nucl & Radiol Engn, Gainesville, FL 32611 USA. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Sandia Natl Labs, Albuquerque, NM 87185 USA. RP Univ Florida, Dept Nucl & Radiol Engn, Gainesville, FL 32611 USA. EM mfensin@lanl.gov NR 7 TC 0 Z9 0 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 448 EP + PG 2 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600050 ER PT S AU Chavers, DG Dobson, C Jones, J Lee, M Martin, A Gregory, J Cecil, J Bengtson, RD Breizman, B Arefiev, A Chang-Diaz, F Squire, J Glover, T McCaskill, G Cassibry, J Li, ZM AF Chavers, DG Dobson, C Jones, J Lee, M Martin, A Gregory, J Cecil, J Bengtson, RD Breizman, B Arefiev, A Chang-Diaz, F Squire, J Glover, T McCaskill, G Cassibry, J Li, ZM BE ElGenk, MS TI Status of magnetic nozzle and plasma detachment experiment SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM - STAIF 2006 SE AIP Conference Proceedings LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE magnetic nozzle; plasma detachment; magnetized plasma; magnetohydrodynamics ID INSTRUMENT; FLUX AB High power plasma propulsion can move large payloads for orbit transfer, lunar missions, and beyond with large savings in fuel consumption owing to the high specific impulse. At high power, lifetime of the thruster becomes an issue. Electrodeless devices with magnetically guided plasma offer the advantage of long life since magnetic fields confine the plasma radially and keep it from impacting the material surfaces. For decades, concerns have been raised about the plasma remaining attached to the magnetic field and returning to the vehicle along the closed magnetic field lines. Recent analysis suggests that this may not be an issue if the magnetic field is properly shaped in the nozzle region and the plasma has sufficient energy density to stretch the magnetic field downstream. An experiment is being performed to test the theory regarding the MHD detachment scenario. The status of that experiment will be discussed in this paper. C1 NASA, George C Marshall Space Flight Ctr, Prop Res Ctr, Huntsville, AL 35812 USA. Univ Texas Austin, Dept Phys, Austin, TX 78712 USA. Univ Texas Austin, Inst Fus Studies, Austin, TX 78712 USA. Ad Astra Rocket Co, Houston, TX 77058 USA. Univ Alabama, Huntsville, AL 35899 USA. RP NASA, George C Marshall Space Flight Ctr, Prop Res Ctr, Huntsville, AL 35812 USA. EM greg.chavers@nasa.gov RI Arefiev, Alexey/A-8550-2016 OI Arefiev, Alexey/0000-0002-0597-0976 NR 11 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 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 465 EP + PG 2 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600052 ER PT S AU Eskridge, RH Fimognari, PJ Martin, AK Lee, MH AF Eskridge, RH Fimognari, PJ Martin, AK Lee, MH BE ElGenk, MS TI Design and construction of the PT-1 prototype plasmoid thruster SO Space Technology and Applications International Forum - STAIF 2006 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE plasmoid thruster; field reversed configuration; spheromak; compact toroid; propulsion; theta pinch; electric propulsion; electrode-less; inductive; accelerator AB The design and construction of a plasmoid thruster prototype is described. This thruster operates by expelling pre-detached plasmoids at high velocities. These plasmoids are field reversed configuration plasmas which are formed by reversing a magnetic flux frozen in an ionized gas inside a theta-pinch coil. The pinch coil is a unique multi-turn, multi-lead design chosen for optimization of inductance and field uniformity. The coil is wound around an alumina ceramic core and the operation of the thruster is completely electrode-less. The design of this thruster follows a series of experiments at NASA MSFC based on a single turn theta-pinch coil called the "Plasmoid Thruster Experiment." Key issues are addressed which affect the efficiency of the PT-1. Testing of this device will begin in FY06 at the NASA MSFC Propulsion Research Center. C1 NASA, George C Marshall Space Flight Ctr, Propuls Res Ctr, Huntsville, AL 35812 USA. RP Eskridge, RH (reprint author), NASA, George C Marshall Space Flight Ctr, Propuls Res Ctr, Huntsville, AL 35812 USA. NR 7 TC 3 Z9 3 U1 0 U2 4 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 474 EP 483 PG 10 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600053 ER PT S AU Ballard, RO AF Ballard, RO BE ElGenk, MS TI REIMR- A process for utilizing liquid rocket propulsion-oriented 'lessons learned' to mitigate development risk in nuclear thermal propulsion SO Space Technology and Applications International Forum - STAIF 2006 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE nuclear thermal propulsion; NTP; lessons learned; fundamental root cause; risk mitigation AB This paper is a summary overview of a study conducted at the NASA Marshall Space Flight Center (NASA-MSFC) during the initial phases of the Space Launch Initiative (SLI) program to evaluate a large number of technical problems associated with the design, development, test, evaluation and operation of several major liquid propellant rocket engine systems (i.e., SSME, Fastrac, J-2, F-1). One of the primary results of this study was the identification of the "Fundamental Root Causes" that enabled the technical problems to manifest, and practices that can be implemented to prevent them from recurring in future propulsion system development efforts, such as that which is currently envisioned in the field of nuclear thermal propulsion (NTP). This paper will discus the Fundamental Root Causes, cite some examples of how the technical problems arose from them, and provide a discussion of how they can be mitigated or avoided in the development of an NTP system. C1 NASA, George C Marshall Space Flight Ctr, Nucl & Adv Propuls Syst Engn Branch, Huntsville, AL 35812 USA. RP Ballard, RO (reprint author), NASA, George C Marshall Space Flight Ctr, Nucl & Adv Propuls Syst Engn Branch, Huntsville, AL 35812 USA. NR 4 TC 0 Z9 0 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 514 EP 521 PG 8 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600057 ER PT S AU Chen, SS Veres, JP Fittje, JE AF Chen, SS Veres, JP Fittje, JE BE ElGenk, MS TI Turbopump design and analysis approach for nuclear thermal rockets SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM - STAIF 2006 SE AIP Conference Proceedings LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE turbopump; nuclear thermal rocket engine; conceptual design; system analysis AB A rocket propulsion system, whether it is a chemical rocket or a nuclear thermal rocket, is fairly complex in detail but rather simple in principle. Among all the interacting parts, three components stand out: they are pumps & turbines (turbopumps), and the thrust chamber. To obtain an understanding of the overall rocket propulsion system characteristics, one starts from analyzing the interactions among these three components. It is therefore of utmost importance to be able to satisfactorily characterize the turbopump, level by level, at all phases of a vehicle design cycle. Here at the NASA Glenn Research Center, as the starting phase of a rocket engine design, specifically a Nuclear Thermal Rocket Engine design, we adopted the approach of using a high level system cycle analysis code (NESS) to obtain an initial analysis of the operational characteristics of a turbopump required in the propulsion system. A set of turbopump design codes (PumpDes and TurbDes) were then executed to obtain sizing and performance parameters of the turbopump that were consistent with the mission requirements. A set of turbopump analyses codes (PUMPA and TURBA) were applied to obtain the full performance map for each of the turbopump components; a two dimensional layout of the turbopump based on these mean line analyses was also generated. Adequacy of the turbopump conceptual design will later be determined by further analyses and evaluation. In this paper, descriptions and discussions of the aforementioned approach are provided and future outlooks are discussed. C1 NASA, Lewis Res Ctr, Cleveland, OH 44135 USA. RP NASA, Lewis Res Ctr, Cleveland, OH 44135 USA. EM shu-cheng.s.chen@nasa.gov NR 13 TC 0 Z9 0 U1 0 U2 2 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 522 EP + PG 2 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600058 ER PT S AU Emrich, WJ AF Emrich, WJ BE ElGenk, MS TI Non nuclear NTR environmental simulator SO Space Technology and Applications International Forum - STAIF 2006 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE nuclear thermal rocket; fuel element; testing AB Nuclear Thermal Rockets or NTR's have been suggested as a propulsion system option for vehicles traveling to the moon or Mars. These engines are capable of providing high thrust at specific impulses at least twice that of today's best chemical engines. The performance constraints on these engines are mainly the result of temperature limitations on the fuel coupled with a limited ability to withstand chemical attack by the hot hydrogen propellant. To operate at maximum efficiency, fuel forms are desired which can withstand the extremely hot, hostile environment characteristic of NTR operation for at least several hours. The simulation of such an environment would require an experimental device which could simultaneously approximate the power, flow, and temperature conditions which a nuclear fuel element (or partial element) would encounter during NTR operation. Such a simulation would allow detailed studies of the fuel behavior and hydrogen flow characteristics under reactor like conditions to be performed. The goal of these simulations would be directed toward expanding the performance envelope of NTR engines over that which was demonstrated during the Rover and NERVA nuclear rocket programs of the 1970's. Current planning calls for such a simulator to be constructed at the Marshall Space Flight Center over the coming year, and it is anticipated that it will be used in the future to evaluate a wide variety of fuel element designs and the materials of which they are constructed. This present work addresses the initial experimental objectives of the NTR simulator with regard to reproducing the fuel degradation patterns previously observed during the NERVA testing. C1 NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Emrich, WJ (reprint author), NASA, George C Marshall Space Flight Ctr, MS XD21, Huntsville, AL 35812 USA. NR 5 TC 4 Z9 4 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 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 531 EP 536 PG 6 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600059 ER PT S AU Wang, TS Foote, J Litchford, R AF Wang, TS Foote, J Litchford, R BE ElGenk, MS TI Multiphysics thermal-fluid design analysis of a non-nuclear tester for hot-hydrogen materials and component development SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM - STAIF 2006 SE AIP Conference Proceedings LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE multiphysics; computational fluid dynamics; nuclear thermal engine AB The objective of this effort is to perform design analyses for a non-nuclear hot-hydrogen materials tester, as a first step towards developing efficient and accurate multiphysics, thermo-fluid computational methodology to predict environments for hypothetical solid-core, nuclear thermal engine thrust chamber design and analysis. The computational methodology is based on a multidimensional, finite-volume, turbulent, chemically reacting, thermally radiating, unstructured-grid, and pressure-based formulation. The multiphysics invoked in this study include hydrogen dissociation kinetics and thermodynamics, turbulent flow, convective, and thermal radiative heat transfers. The goals of the design analyses are to maintain maximum hot-hydrogen jet impingement energy and to minimize chamber wall heating. The results of analyses on three test fixture configurations and the rationale for final selection are presented. The interrogation of physics revealed that reactions of hydrogen dissociation and recombination are highly correlated with local temperature and are necessary for accurate prediction of the hot-hydrogen jet temperature. C1 NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. EM Ten-See.Wang-1@nasa.gov FU Nuclear Systems Office; MSFC Internal Research and Development FX This study was partially supported by a Nuclear Systems Office task entitled Multiphysics Thrust Chamber Modeling and by a MSFC Internal Research and Development focus area task entitled Hot Hydrogen Materials and Component Development. 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 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 537 EP + PG 2 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600060 ER PT S AU Krause, DL Kantzos, PT AF Krause, DL Kantzos, PT BE ElGenk, MS TI Accelerated life structural benchmark testing for a Stirling convertor heater head SO Space Technology and Applications International Forum - STAIF 2006 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE stirling creep deformation life techniques temperature Inconel 718 superalloy precipitate grain microscopy AB For proposed long-duration NASA Space Science missions, the Department of Energy, Lockheed Martin, Infinia Corporation, and NASA Glenn Research Center are developing a high-efficiency, 110-watt Stirling Radioisotope Generator (SRG 110). A structurally significant limit state for the SRG 110 heater head component is creep deformation induced at high material temperature and low stress level. Conventional investigations of creep behavior adequately rely on experimental results from uniaxial creep specimens, and a wealth of creep data is available for the Inconel 718 material of construction. However, the specified atypical thin heater head material is fine-grained with a heat treatment that limits precipitate growth, and little creep property data for this microstructure is available in the literature. In addition, the geometry and loading conditions apply a multiaxial stress state on the component, far from the conditions of uniaxial testing. For these reasons, an extensive experimental investigation is ongoing to aid in accurately assessing the durability of the SRG 110 heater head. This investigation supplements uniaxial creep testing with pneumatic testing of heater head-like pressure vessels at design temperature with stress levels ranging from approximately the design stress to several times that. This paper presents experimental results, post-test microstructural analyses, and conclusions for four higher-stress, accelerated life tests. Analysts are using these results to calibrate deterministic and probabilistic analytical creep models of the SRG 110 heater head. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Krause, DL (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. NR 7 TC 1 Z9 1 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 623 EP 630 PG 8 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600071 ER PT S AU DellaCorte, C Radi, KC Bruckner, RJ Bauman, SW Puleo, BJ Howard, SA AF DellaCorte, C Radi, KC Bruckner, RJ Bauman, SW Puleo, BJ Howard, SA BE ElGenk, MS TI Rotor support technology developments for long life Closed Brayton Cycle turbines SO Space Technology and Applications International Forum - STAIF 2006 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE nuclear power; Brayton; turbine; foil gas bearings AB Power conversion systems based upon the Closed Brayton Cycle (CBC) turbine are under consideration for space power generation applications. Using this approach, inert gas, heated with a nuclear reactor or other means, is used to drive a turbine-generator in a recirculating flow path. As a closed system, contamination of the working fluid, for instance with bearing lubricating oil, cannot be tolerated. To prevent this possibility, compliant surface gas film bearings are employed that use the working fluid as their lubricant. Foil gas bearings are in widespread use in turbocompressors and microturbines in aeronatuics and terrestrial applications. To successfully implement them for space power CBC systems, research is underway at NASA's Glenn Research Center to assess foil bearing start-up torque requirements, bearing thermal management and the effects of high ambient pressures in inert gases on performance. This paper introduces foil gas bearing rotor support technologies and provides an update on bearing performance testing and evaluations being conducted to integrate foil bearings in future CBC turbine systems. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP DellaCorte, C (reprint author), NASA, Glenn Res Ctr, Mail Stop 23-2,21000 Brookpark Rd, Cleveland, OH 44135 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 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 653 EP 661 PG 9 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600074 ER PT S AU Johnson, PK Hervol, DS AF Johnson, PK Hervol, DS BE ElGenk, MS TI Experimental validation of a Closed Brayton Cycle system transient simulation SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM - STAIF 2006 SE AIP Conference Proceedings LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE Brayton power conversion; thermal transient modeling AB The Brayton Power Conversion Unit (BPCU) located at NASA Glenn Research Center (GRC) in Cleveland, OH was used to validate the results of a computational code known as Closed Cycle System Simulation (CCSS). Conversion system thermal transient behavior was the focus of this validation. The BPCU was operated at various steady state points and then subjected to transient changes involving shaft rotational speed and thermal energy input. These conditions were then duplicated in CCSS. Validation of the CCSS BPCU model provides confidence in developing future Brayton power system performance predictions, and helps to guide high power Brayton technology development. C1 Analex Corp, Mech Syst Branch, Glenn Engn & Sci Support Or, NASA Glenn Res Ctr, MS 301-2,21000 Brookpk Rd, Cleveland, OH USA. RP Analex Corp, Mech Syst Branch, Glenn Engn & Sci Support Or, NASA Glenn Res Ctr, MS 301-2,21000 Brookpk Rd, Cleveland, OH USA. EM Paul.K.Johnson@grc.nasa.gov NR 14 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 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 673 EP + PG 2 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600076 ER PT S AU Green, NW Frederickson, AR AF Green, NW Frederickson, AR BE ElGenk, MS TI A study of spacecraft charging due to exposure to interplanetary protons SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM - STAIF 2006 SE AIP Conference Proceedings LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE spacecraft charging; proton; dielectric discharge; IESD ID FLUENCE MODEL; CONDUCTIVITY; INSULATORS; STORAGE AB The interplanetary space environment is composed mostly of low energy (E < 100 keV) plasma from the solar wind and high energy (E > 1 MeV) protons from solar energetic particle events. Satellites orbiting Earth are shielded to some degree from these events by the Earth's magnetic field but spacecraft traveling between planets and space nuclear systems on the lunar or Martian surface are exposed to these solar protons directly. A major concern for spacecraft is bulk dielectric charging, a form of spacecraft charging that can lead to dielectric discharges, a form of internal electrostatic discharge (IESD) that can damage sensitive electronics. The majority of research regarding IESD has been concerned with the electrons in the space environment around the Earth and at Jupiter; little research has been done on the charging of spacecraft in interplanetary space due to solar event protons. This paper provides a review of the literature regarding IESD due to protons and presents the results of recent laboratory experiments. Topics for further research are also suggested. 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 Nelson.W.Green@jpl.nasa.gov FU National Aeronautics and Space Administration FX The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. The authors gratefully acknowledge the following colleagues for their contributions of data and expertise: C. Benson, A. Shapiro, P. Willis, and H. Garret. In memory of Dr. A. Robb Frederickson who passed away April 5, 2004 while this paper was been researched and written. NR 22 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 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 694 EP + PG 3 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600078 ER PT S AU Kang, S Lipinski, R McAlpine, W AF Kang, S Lipinski, R McAlpine, W BE ElGenk, MS TI Lunar surface reactor shielding study SO Space Technology and Applications International Forum - STAIF 2006 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE nuclear reactor; shield; MCNPX AB A nuclear reactor system could provide power to support long term human exploration of the moon. Such a system would require shielding to protect astronauts from its emitted radiations. Shielding studies have been performed for a Gas Cooled Reactor system because it is considered to be the most suitable nuclear reactor system available for lunar exploration, based on its tolerance of oxidizing lunar regolith and its good conversion efficiency. The goals of the shielding studies were to determine a material shielding configuration that reduces the dose (rem) to the required level in order to protect astronauts, and to estimate the mass of regolith that would provide an equivalent protective effect if it were used as the shielding material. All calculations were performed using MCNPX, a Monte Carlo transport code. Lithium hydride must be kept between 600 K and 700 K to prevent excessive swelling from large amounts of gamma or neutron irradiation. The issue is that radiation damage causes separation of the lithium and the hydrogen, resulting in lithium metal and hydrogen gas. The proposed design uses a layer of B4C to reduce the combined neutron and gamma dose to below 0.5Grads before the LiH is introduced. Below 0.5Grads the swelling in LiH is small (less than about 1%) for all temperatures. This approach causes the shield to be heavier than if the B4C were replaced by LiH, but it makes the shield much more robust and reliable. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Sandia Natl Labs, Albuquerque, NM 87185 USA. RP Kang, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 5 TC 13 Z9 14 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 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 707 EP 715 PG 9 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600080 ER PT S AU Gould, JE Ritzert, FJ Loewenthal, WS AF Gould, JE Ritzert, FJ Loewenthal, WS BE ElGenk, MS TI Preliminary investigations of joining technologies for attaching refractory metals to Ni-based superalloys SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM - STAIF 2006 SE AIP Conference Proceedings LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE dissimilar materials joining; refractory metals; superalloys; inertia welding; electro-spark deposition; magnetic pulse welding ID ALUMINUM AB In this study, a range of joining technologies has been investigated for creating attachments between refractory metal and Ni-based superalloys. Refractory materials of interest include Mo-47%Re, T-111, and Ta-10%W. The Ni-based superalloys include Hastelloy X and MarM 247. During joining with conventional processes, these materials have potential for a range of solidification and intermetallic formation-related defects. For this study, three non-conventional joining technologies were evaluated. These included inertia welding, electro-spark deposition (ESD) welding, and magnetic pulse welding (MPW). The developed inertia welding practice closely paralleled that typically used for the refractory metals alloys. Metallographic investigations showed that forging during inertia welding occurred predominantly on the refractory metal side. It was also noted that at least some degree of forging on the Ni-based superalloy side of the joint was necessary to achieve consistent bonding. Both refractory metals were readily weldable to the Hastelloy X material. When bonding to the MarM 247, results were inconsistent. This was related to the higher forging temperatures of the MarM 247, and subsequent reduced deformation on that material during welding. ESD trials using a Hastelloy X filler were successful for all material combinations. ESD places down very thin (5- to 10-mu m) layers per pass, and interactions between the substrates and the fill were limited (at most) to that layer. For the refractory metals, the fill only appeared to wet the surface, with minimal dilution effects. Microstructures of the deposits showed high weld metal integrity with maximum porosity on the order of a few percent. Some limited success was also obtained with MPW. In these trials, only the T-111 tubes were used. Joints were possible for the T-111 tube to the Hastelloy X bar stock, but the stiffness of the tube (resisting collapse) necessitated the use of very high power levels. These power levels resulted in damage to the equipment (concentrator) during welding. It is of note that the joint made showed the typical wavy bond microstructure associated with magnetic pulse/explosion bond joints. Joints were not possible between the T-111 tube and the MarM 247 bar stock. In this case, the MarM 247 shattered before sufficient impact forces could be developed for bonding. C1 Edison Welding Inst, 1250 Arthur E Adams Dr, Columbus, OH 43221 USA. NASA Glenn Res Ctr, Cleveland, OH 44135 USA. Ohio Aerosp Inst, Cleveland, OH 44135 USA. RP Edison Welding Inst, 1250 Arthur E Adams Dr, Columbus, OH 43221 USA. EM jerry_gould@ewi.org NR 18 TC 2 Z9 2 U1 1 U2 6 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 757 EP + PG 3 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600085 ER PT S AU Martin, AK Eskridge, RH Fimognari, PJ Lee, MH AF Martin, AK Eskridge, RH Fimognari, PJ Lee, MH BE ElGenk, MS TI FIREBALL: Fusion ignition rocket engine with ballistic ablative lithium liner SO Space Technology and Applications International Forum - STAIF 2006 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE spacecraft Propulsion; FRC; MTF; thermo-nuclear fusion ID NUCLEAR PULSE PROPULSION AB Thermo-nuclear fusion may be the key to a high Isp, high specific power propulsion system. In a fusion system energy is liberated within, and imparted directly to, the propellant. In principle, this can overcome the performance limitations inherent in systems that require thermal power transfer across a material boundary, and/or multiple power conversion stages (NTR, NEP). A thermo-nuclear propulsion system, which attempts to overcome some of the problems inherent in the Orion concept, is described. A dense FRC plasmoid is accelerated to high velocity (in excess of 500 km/s) and is compressed into a detached liner (pulse unit). The kinetic energy of the FRC is converted into thermal and magnetic-field energy, igniting a fusion bum in the magnetically confined plasma. The fusion reaction serves as an ignition source for the liner, which is made out of detonable materials. The energy liberated in this process is converted to thrust by a pusher-plate, as in the classic Orion concept. However with this concept, the vehicle does not carry a magazine of autonomous pulse-units. By accelerating a second, heavier FRC, which acts as a piston, right behind the first one, the velocity required to initiate the fusion bum is greatly reduced. C1 NASA, George C Marshall Space Flight Ctr, Prop Res Ctr, Huntsville, AL 35812 USA. RP Martin, AK (reprint author), NASA, George C Marshall Space Flight Ctr, Prop Res Ctr, XD22, Huntsville, AL 35812 USA. NR 18 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 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 783 EP 794 PG 12 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600088 ER PT S AU Myers, DE Kosareo, DN AF Myers, DE Kosareo, DN BE ElGenk, MS TI Structural analyses of the support trusses for the Nuclear Thermal Rocket engines and drop tanks SO Space Technology and Applications International Forum - STAIF 2006 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE Nuclear Thermal Rocket; NTR; structures; structural analysis; buckling AB Finite element structural analyses were performed on the support trusses of the Nuclear Thermal Rocket (NTR) engines and drop tanks to verify that the proper amount of mass was allocated for these components in the vehicle sizing model. The verification included a static stress analysis, a modal analysis, and a buckling analysis using the MSC/NASTRAN (TM) structural analysis software package. In addition, a crippling stress analysis was performed on the truss beams using a handbook equation. Two truss configurations were examined as possible candidates for the drop tanks truss while a baseline was examined for the engine support thrust structure. For the drop tanks trusses, results showed that both truss configurations produced similar results although one performed slightly better in buckling. In addition, it was shown that the mass allocated in the vehicle sizing model was adequate although the engine thrust structure may need to be modified slightly to increase its lateral natural frequency above the minimum requirement of 8 Hz that is specified in the Delta IV Payload Planners Guide. C1 NASA, Glenn Res Ctr, Appl Struct Mech Branch, Cleveland, OH 44135 USA. RP Myers, DE (reprint author), NASA, Glenn Res Ctr, Appl Struct Mech Branch, 21000 Brookpark Rd MS 86-10, Cleveland, OH 44135 USA. NR 7 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 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 837 EP 846 PG 10 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600094 ER PT S AU Bulman, MJ Poth, G Borowski, S AF Bulman, MJ Poth, G Borowski, S BE ElGenk, MS TI LANTR engine optimization for Lunar missions SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM - STAIF 2006 SE AIP Conference Proceedings LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE nuclear propulsion; Lunar missions AB Propulsion requirements for sustainable Lunar missions are very demanding. The high Delta V for short transit times and/or reusable vehicles are best served with the High Isp of Nuclear Propulsion. High thrust is needed to reduce gravity losses during earth departure. The LOX-Augmented Nuclear Thermal Rocket (LANTR) is a concept whereby thrust from a nuclear thermal rocket can be doubled, or even quadrupled, by the injection and combustion of gaseous oxygen downstream of the throat. This has many advantages for the mission including a reduction in the size of the reactor(s) and propellant tank volume for a given payload delivered to Low Lunar Orbit. In this paper, we conduct mission studies to define the optimum basic (Unaugmented) engine thrust, Lox augmentation level and Lox loading for minimum initial mass in low earth orbit. 35% mass savings are seen for NTR powered LTVs with over twice the propellant Volume. The LANTR powered LTV has a similar mass savings with minimal volume penalties. C1 Aerojet, POB 13222, Sacramento, CA 95813 USA. NASA, Lewis Res Ctr, Cleveland, OH 44135 USA. RP Aerojet, POB 13222, Sacramento, CA 95813 USA. EM mel.bulman@Aerojet.com NR 6 TC 1 Z9 1 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 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 847 EP + PG 2 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600095 ER PT S AU Stewart, MEM Krivanek, TM Hemminger, JA Bulman, MJ AF Stewart, MEM Krivanek, TM Hemminger, JA Bulman, MJ BE ElGenk, MS TI 3D reacting flow analysis of LANTR nozzles SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM - STAIF 2006 SE AIP Conference Proceedings LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE nuclear propulsion AB This paper presents performance predictions for LANTR nozzles and the system implications for their use in a manned Mars mission. The LANTR concept is rocket thrust augmentation by injecting Oxygen into the nozzle to combust the Hydrogen exhaust of a Nuclear Thermal Rocket. The performance predictions are based on three-dimensional reacting flow simulations using VULCAN. These simulations explore a range Of O-2/H-2 mixture ratios, injector configurations, and concepts. These performance predictions are used for a trade analysis within a system study for a manned Mars mission. Results indicate that the greatest benefit of LANTR will occur with In-Situ Resource Utilization (ISRU). However, Hydrogen propellant volume reductions may allow greater margins for fitting tanks within the launch vehicle where packaging issues occur. C1 NASA, Glenn Res Ctr, QSS Grp Inc, 21000 Brookpark Rd,MS 142-4, Cleveland, OH 44135 USA. RP NASA, Glenn Res Ctr, QSS Grp Inc, 21000 Brookpark Rd,MS 142-4, Cleveland, OH 44135 USA. EM Mark.E.Stewart@grc.nasa.gov FU NASA Computing and Information Communications Technology (CICT) [NAS3-00145]; NASA Glenn Research Center FX This work was supported by the NASA Computing and Information Communications Technology (CICT) program (contract NAS3-00145) at NASA Glenn Research Center. The authors would like to thank, Stanley K. Borowski, for suggesting this problem, Ambady Suresh, Louis A. Povinelli, Charles J. Trefny, for valuable discussions, and Jeff White and Robert A. Baurle, NASA Langley Research Center, for help with VULCAN. NR 24 TC 0 Z9 0 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 858 EP + PG 2 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600096 ER PT S AU Elliott, JO Schriener, TM Coste, K AF Elliott, JO Schriener, TM Coste, K BE ElGenk, MS TI Concept for a radioisotope powered dual mode lunar rover SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM - STAIF 2006 SE AIP Conference Proceedings LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE lunar rover; human exploration; radioisotope power system AB Over three decades ago, the Apollo missions manifestly demonstrated the value of a lunar rover to expand the exploration activities of lunar astronauts. The stated plan of the new Vision for Space Exploration to establish a permanent presence on the moon in the next decades gives new impetus to providing long range roving and exploration capability in support of the siting, construction, and maintenance of future human bases. The incorporation of radioisotope power systems and telerobotic capability in the design has the potential to significantly expand the capability of such a rover, allowing continuous operation during the full lunar day/night cycle, as well as enabling exploration in permanently shadowed regions that may be of interest to humans for the resources they may hold. This paper describes a concept that builds on earlier studies originated in the Apollo program for a Dual Mode (crewed and telerobotic) Lunar Roving Vehicle (DMLRV). The goal of this vehicle would be to provide a multipurpose infrastructure element and remote science platform for the exploration of the moon. The DMLRV would be essential for extending the productivity of human exploration crews, and would provide a unique capability for diverse long-range, long-duration science exploration between human visits. With minimal reconfiguration this vehicle could also provide the basic platform to support a range of site survey and preparation activities in anticipation of the establishment of a permanent human presence on the moon. A conceptual design is presented for the DMLRV, including discussion of mission architecture, vehicle performance, representative science payload accommodation, and equipment and crew radiation considerations. C1 CALTECH, Jet Prop Lab, Syst Engn Sect, Pasadena, CA 91109 USA. RP CALTECH, Jet Prop Lab, Syst Engn Sect, Pasadena, CA 91109 USA. EM jelliott@jpl.nasa.gov 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 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 898 EP + PG 2 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600100 ER PT S AU Elliott, JO Reh, K MacPherson, D AF Elliott, JO Reh, K MacPherson, D BE ElGenk, MS TI Lunar fission surface power system design and implementation concept SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM - STAIF 2006 SE AIP Conference Proceedings LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE Prometheus Project; Fission Power; Lunar Base AB At the request of NASA's Exploration Systems Mission Directorate (ESMD) in May of 2005, a team was assembled within the Prometheus Project to investigate lunar surface nuclear power architectures and provide design and implementation concept inputs to NASA's Exploration Systems Architecture 60-day Study (ESAS) team. System engineering tasks were undertaken to investigate the design and implementation of a Fission Surface Power System (FSPS) that could be launched as early as 2019 as part of a possible initial Lunar Base architecture. As a result of this activity, the Prometheus team evaluated a number of design and implementation concepts as well as a significant number of trades associated with lunar surface power, all culminating in a recommended approach. This paper presents the results of that study, including a recommended FSPS design and implementation concept. C1 CALTECH, Jet Prop Lab, Syst Engn Sect, Pasadena, CA 91109 USA. RP CALTECH, Jet Prop Lab, Syst Engn Sect, Pasadena, CA 91109 USA. EM jelliott@jpl.nasa.gov NR 1 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 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 942 EP + PG 2 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600104 ER PT S AU Dorsey, JT Collins, TJ Moe, RV Doggett, WR AF Dorsey, JT Collins, TJ Moe, RV Doggett, WR BE ElGenk, MS TI Framework for defining and assessing benefits of a modular assembly design approach for exploration systems SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM - STAIF 2006 SE AIP Conference Proceedings LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE modular assembly; in-space assembly; servicing; repair; evaluation criteria; metrics; interfaces AB A comprehensive modular assembly system model has been proposed that extends the art from modular hardware, to include in-space assembly, servicing and repair and it's critical components of infrastructure, agents and assembly operations. Benefits of modular assembly have been identified and a set of metrics defined that extends the art beyond the traditional measures of performance, with emphasis on criteria that allow life-cycle mission costs to be used as a figure of merit (and include all substantive terms that have an impact on the evaluation). The modular assembly approach was used as a basis for developing a Solar Electric Transfer Vehicle (SETV) concept and three modular assembly scenarios were developed. The modular assembly approach also allows the SETV to be entered into service much earlier than competing conventional configurations and results in a great deal of versatility in accommodating different launch vehicle payload capabilities, allowing for modules to be pre-assembled before launch or assembled on orbit, without changing the space vehicle design. C1 NASA, Langley Res Ctr, Met & Thermal Struct Branch, MS 396, Hampton, VA 23681 USA. RP NASA, Langley Res Ctr, Met & Thermal Struct Branch, MS 396, Hampton, VA 23681 USA. EM john.t.dorsey@nasa.gov NR 9 TC 0 Z9 0 U1 0 U2 2 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 969 EP + PG 2 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600106 ER PT S AU Diftler, MA Doggett, WR Mehling, JS King, BD AF Diftler, MA Doggett, WR Mehling, JS King, BD BE ElGenk, MS TI Reconfiguration of EVA modular truss assemblies using an anthropomorphic robot SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM - STAIF 2006 SE AIP Conference Proceedings LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE space construction; infrastructure; modularity; assembly; dexterous robot; shared control ID DESIGN CONSIDERATIONS; SPACE; ROBONAUT AB NASA relies heavily on astronauts to perform Extra-Vehicular Activities (EVA) as part of space construction and maintenance operations. Astronauts provide an unmatched capability and flexibility. In the future, this capability will be in even greater demand as space platforms become more modular making on-orbit servicing, repair and reconfiguration routine. To assist crew, NASA is developing Robonaut, an anthropomorphic robot with human sized arms and hands that can work with many of the same interfaces designed for the space suited astronaut. Recently Robonaut has been used to investigate techniques for automated assembly, disassembly, and repair of space platforms. The current work focuses on techniques to reconfigure a modular truss system representative of the tasks necessary to convert a space solar power tug to a lunar orbiting solar power station in support of lunar exploration missions. An overview of these activities is given, detailing the assembly sequence and the infrastructure used by Robonaut to perform the reconfiguration operations. Advances in Robonaut's capabilities are described and include: a grip surface augmentation to Robonaut's gloves that provides a close approximation to the latest astronaut gloves, ensuring a secure grasp during truss coupler manipulation, and a shared control strategy that divides the Cartesian control of Robonaut's hands between the teleoperator and the robot's on-board controller to minimize human workload during constrained tasks. To support truss reconfiguration experiments, infrastructure is required to stabilize and register the structure during reconfiguration. Details on the design and operation of the infrastructure, a small fixture, are given. C1 NASA, Lyndon B Johnson Space Ctr, Automat Robot & Simulat Div, Houston, TX 77058 USA. NASA Langley Res Ctr, Dynam Syst & Control Branch, Hampton, VA 23681 USA. Lockheed Martin, Hampton, VA 23681 USA. RP NASA, Lyndon B Johnson Space Ctr, Automat Robot & Simulat Div, Houston, TX 77058 USA. EM myron.a.diftler@nasa.gov FU NASA's Exploration Systems and Missions Directorate FX This work was partially supported by NASA's Exploration Systems and Missions Directorate through the "Advanced Materials and Structures for the Modular Assembly of Large Space Platforms" Project. NR 18 TC 0 Z9 0 U1 1 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 992 EP + PG 2 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600108 ER PT S AU Mikulas, MM Collins, TJ Doggett, W Dorsey, J Watson, J AF Mikulas, MM Collins, TJ Doggett, W Dorsey, J Watson, J BE ElGenk, MS TI Truss performance and packaging metrics SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM - STAIF 2006 SE AIP Conference Proceedings LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE truss; structures; deployable; inflatable; erectable; packaging; efficiency; metrics; modular; in-space fabrication AB In the present paper a set of performance metrics are derived from first principals to assess the efficiency of competing space truss structural concepts in terms of mass, stiffness, and strength, for designs that are constrained by packaging. The use of these performance metrics provides unique insight into the primary drivers for lowering structural mass and packaging volume as well as enabling quantitative concept performance evaluation and comparison. To demonstrate the use of these performance metrics, data for existing structural concepts are plotted and discussed. Structural performance data is presented for various mechanical deployable concepts, for erectable structures, and for rigidizable structures. C1 Natl Inst Aerosp, Hampton, VA USA. NASA, Langley Res Ctr, Hampton, VA USA. RP Natl Inst Aerosp, Hampton, VA USA. EM Mikulasmmm@aol.com FU NASA; DARPA FX The authors would like to thank NASA and DARPA for providing the funds that enabled this research. NR 10 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 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 1000 EP + PG 3 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600109 ER PT S AU Smitherman, DV Dayal, V Dunn, DJ AF Smitherman, DV Dayal, V Dunn, DJ BE ElGenk, MS TI Architecture for a mobile lunar base using lunar materials SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM - STAIF 2006 SE AIP Conference Proceedings LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE mobile habitat; Hab-Bot; habot; robotic walkers; walking machines; propellant depots; lunar shelters; space vehicles AB During the summers of 2004, and 2005, several studies were conducted in the Future Concepts Office at the NASA Marshall Space Flight Center (MSFC) with assistance from summer faculty and student program participants to develop concepts and architectures for mobile lunar habitats. This work included conceptual designs for a launch architecture derived from existing expendable launch systems; a lunar walker based on existing technology for the robotics; compatible hardware from the International Space Station (ISS) program for pressurized modules; and lunar resources utilization for environmental shielding. This paper provides a brief summary of some of the key findings from these studies, and identifies areas for future work that could lead to more robust lunar exploration architectures in the future. In conclusion, it is recommended that future exploration missions consider reusable depot/transfer vehicles, robotic walking technology for lunar exploration, and lunar resources utilization for environmental shielding of surface habitats. C1 NASA, George C Marshall Space Flight Ctr, Adv Projects Off, Huntsville, AL 35812 USA. Iowa State Univ Sci & Technol, Dept Aerosp Engn, Ames, IA 50011 USA. NASA Marshall Space Flight Ctr, Res Program, Huntsville, AL 35812 USA. RP NASA, George C Marshall Space Flight Ctr, Adv Projects Off, Huntsville, AL 35812 USA. EM David.Smitherman@nasa.gov FU NASA Summer Faculty Research Opportunities Program; NASA Undergraduate Student Research Program (USRP); NASA MSFC FX This research was conducted in summer of 2005 in the Future Concepts Office (SP20) of the Space Systems Programs and Projects Office at the NASA Marshall Space Flight Center (MSFC), in Huntsville, Alabama. The NASA Summer Faculty Research Opportunities Program, the NASA Undergraduate Student Research Program (USRP), and the NASA MSFC provided funding support. Participants included David Smitherman (SP20) for overall mission architecture and study leadership, Dr. Vinay Dayal, Iowa State University for detailed design and analysis of the lunar shelters, and Daniel Dunn (USRP) for module and walker designs and animations. Figures were provided as follows: 1-3, Daniel Dunn and David Smitherman; 4-5 & 7, Daniel Dunn; 8 and Table 1, Vinay Dayal. NR 5 TC 0 Z9 1 U1 0 U2 2 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 1022 EP + PG 2 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600111 ER PT S AU Gavert, RB AF Gavert, RB BE ElGenk, MS TI Lunar colonization and NASA's exploration changes SO Space Technology and Applications International Forum - STAIF 2006 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE lunar colonization; tourism; exploration AB Space colonization is not part of NASA's mission planning. NASA's exploration vision, mission goals and program implementations, however, can have an important affect on private lunar programs leading towards colonization. NASA's exploration program has been described as a journey not a race. It is not like the Apollo mission having tight schedules and relatively unchanging direction. NASA of this era has competing demands from the areas of aeronautics, space science, earth science, space operations and, there are competing demands within the exploration program itself. Under the journey not a race conditions, an entrepreneur thinking about building a hotel on the Moon, with a road to an exploration site, might have difficulty determining where and when NASA might be at a particular place on the Moon. Lunar colonization advocates cannot depend on NASA or other nations with space programs to lead the way to colonization. They must set their own visions, mission goals and schedules. In implementing their colonization programs they will be resource limited. They would be like "hitchhikers" following the programs of spacefaring nations identifying programs that might have a fit with their vision and be ready to switch to other programs that may take them in the colonization direction. At times they will have to muster their own limited resources and do things themselves where necessary. The purpose of this paper is to examine current changes within NASA, as a lunar colonization advocate might do, in order to see where there might be areas for fitting into a lunar colonization strategy. The approach will help understand how the "hitchhiking" technique might be better utilized. C1 NASA, Innovat Partnering Program, Washington, DC 20546 USA. RP Gavert, RB (reprint author), NASA, Innovat Partnering Program, Washington, DC 20546 USA. NR 9 TC 0 Z9 0 U1 0 U2 2 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 1033 EP 1040 PG 8 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600112 ER PT S AU Khan, Z Vranis, A Zavoico, A Freid, S Manners, B AF Khan, Z Vranis, A Zavoico, A Freid, S Manners, B BE ElGenk, MS TI Power system concepts for the lunar outpost: A review of the power generation, energy storage, power management and distribution (PMAD) system requirements and potential technologies for development of the lunar outpost SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM - STAIF 2006 SE AIP Conference Proceedings LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE lunar base; power systems; photovoltaic AB This paper will review potential power system concepts for the development of the lunar outpost including power generation, energy storage and power management and distribution (PMAD). In particular, the requirements of the initial robotic missions will be discussed and the technologies considered will include cryogenics and regenerative fuel cells (RFC), AC and DC transmission line technology, high voltage and low voltage power transmission, conductor materials of construction and power beaming concepts for transmitting power to difficult to access locations such as at the bottom of craters. Operating conditions, component characteristics, reliability, maintainability, constructability, system safety, technology gaps/risk and adaptability for future lunar missions will be discussed for the technologies considered. C1 Bechtel Power, 5275 Westview Dr, Frederick, MD 21703 USA. Bechtel Nevada, Las Vegas, NV 89193 USA. NASA Glenn Res Ctr, Cleveland, OH 44135 USA. RP Bechtel Power, 5275 Westview Dr, Frederick, MD 21703 USA. EM zakhan@bechtel.com FU Bechtel Power [DOE/NV/11718-1118]; Bechtel Nevada [DE-AC08-96NV11718]; U.S. Department of Energy FX Zahid A. Khan thanks Jeffrey Hojnicki (NASA Glenn Research Center) and Thomas Kerslake (NASA Glenn Research Center) for their editorial comments and review. Thanks to Paul Nastick (Bechtel Power) and Ram Narula (Bechtel Power) for their support of this paper. DOE/NV/11718-1118. This manuscript has been authored by Bechtel Nevada under Contract No. DE-AC08-96NV11718 with the U.S. Department of Energy. The United States Government retains and the publisher, by accepting the article for publication, acknowledges that the United States Government retains a non-exclusive, paidup, irrevocable, world-wide license to publish or reproduce the published form of this manuscript, or allow others to do so, for United States Government purposes. NR 9 TC 1 Z9 1 U1 1 U2 2 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 1083 EP + PG 2 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600117 ER PT S AU Nayagam, V Sacksteder, KR AF Nayagam, V Sacksteder, KR BE ElGenk, MS TI A vibrofluidized reactor for resource extraction from lunar regolith SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM - STAIF 2006 SE AIP Conference Proceedings LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE ISRU; vibrofluidized reactor; lunar regolith; granular flow ID SHALLOW VIBRATED BEDS; GRANULAR CONVECTION; VERTICAL VIBRATION; HEAT-TRANSFER; DYNAMICS; BEHAVIORS; CONTAINER; PHYSICS; GASES; FLOWS AB The extraction of oxygen and water from the lunar regolith for use as propulsion and life support consumables is an essential feature of any extended-duration missions on the Moon and in preparations for Mars. Most methods for extracting these resources involve heating lunar regolith to significant temperatures under the constraint of a limited power supply. This paper will discuss an innovative method for uniformly heating regolith using a vibrofluidized reactor. Various flow regimes encountered during vibrofluidization and preliminary heat transfer results using a standard Lunar regolith simulant, JSC-1, are presented for a range of acceleration levels and vibration frequencies. The results show that regolith compaction, segregation, or convective mixing can be accomplished depending on the acceleration levels chosen. Granular convection is shown to produce uniform temperature within the heated vibrofluidized reactor. Scaling laws that link performance in normal Earth gravity and Lunar gravity is also discussed. C1 NASA, Glenn Res Ctr, Natl Ctr Space Explorat Res, Cleveland, OH 44135 USA. NASA Glenn Res Ctr, Cleveland, OH 44135 USA. RP NASA, Glenn Res Ctr, Natl Ctr Space Explorat Res, Cleveland, OH 44135 USA. EM v.nayagam@grc.nasa.gov FU NASA Headquarters Exploration Systems Mission Directorate FX This work was part of the RESOLVE project for demonstrating ground truth about hydrogen at the lunar poles; and was supported by the NASA Headquarters Exploration Systems Mission Directorate. The authors are grateful to the RESOLVE Team Members for many helpful discussions. Lindsay Miller, Richard Chapek and John Easton of the NASA Glenn Research Center helped with the experiments. NR 25 TC 2 Z9 2 U1 0 U2 2 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 1101 EP + PG 3 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600119 ER PT S AU Brooks, K Rassat, S Hu, J Stenkamp, S Schlahta, S Bontha, J Holladay, J Simon, T Romig, K Howard, C AF Brooks, K Rassat, S Hu, J Stenkamp, S Schlahta, S Bontha, J Holladay, J Simon, T Romig, K Howard, C BE ElGenk, MS TI Development of a microchannel in situ propellant production system SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM - STAIF 2006 SE AIP Conference Proceedings LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE microchannel; microtechnology; in-situ propellant production; in-situ resource utilization; adsorption; Sabatier; reverse water gas shift; Mars AB A microchannel-based system is being developed for NASA to produce propellants from atmospheric CO2 on Mars. This system will provide a means of reducing the earth-based launch mass for both sample return and human exploration missions. The atmospheric CO2 will be collected, separated, and compressed with a microchannel thermal swing adsorption system. It will be reacted with hydrogen that has either been electrolyzed from the available subsurface water or brought from earth. Methane and water will be produced by using microchannel Sabatier and Reverse Water Gas Shift reactors, respectively. The water will then separated with a microchannel condenser/phase separator and electrolyzed to produce oxygen and hydrogen. Feed gases will be separated from the products and recycled. The system design requirements will be presented in this paper. The design and fabrication methods of the microchannel CO2 sorption pump, reactors, and phase separators will be described, and the advantages of microchannel architecture will be delineated for each component. Estimates of system mass and volume will also be provided in comparison to conventional hardware. The testing and integration proposed during this project to meet NASA's Technology Readiness Level 5 will also be presented. C1 Battelle Mem Inst, Pacific NW Div, Richland, WA 99352 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Battelle Mem Inst, Pacific NW Div, Richland, WA 99352 USA. EM kriston.brooks@pnl.gov FU Advanced Space Technology Program; Office of Exploration Systems FX The authors would like to acknowledge the Advanced Space Technology Program and the Office of Exploration Systems for their financial support and the technical direction provided by Johnson Space Center. NR 21 TC 0 Z9 0 U1 1 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 1111 EP + PG 2 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600120 ER PT S AU England, C Hrubes, JD AF England, C Hrubes, JD BE ElGenk, MS TI Recovering the atmospheric resources of Mars: Updating the MARRS study SO SPACE TECHNOLOGY AND APPLICATIONS INTERNATIONAL FORUM - STAIF 2006 SE AIP Conference Proceedings LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE Mars; atmosphere; oxygen; ISRU; variability; propellant; in-situ resource utilization; MARRS; O-2 AB In 2000 a conceptual design was conducted of a plant that extracts oxygen (O-2) directly from the martian atmosphere, and that makes water and carbon monoxide (CO) as by-products. Updated estimates suggest that the amount of O-2 in the atmosphere is about 2.3 times greater than that used as the basis for the 2000 study. In this paper, estimates for O-2 and by-products, and for energy and mass requirements based on the higher O-2 value are updated. The basis for the design, termed "MARRS" for Mars Atmosphere Resource Recovery System, is the NASA/JSC Mars Reference Mission (MRM) requirement for O-2, estimated at 5.8 kg/hr for about 500 sols. The 2000 study based its design on an atmospheric O-2 content of 0.13%, the then-accepted value. Analysis now places the O-2 content at about 0.3%, reducing the amount of energy and equipment proportionately. The revised estimate of the thermal power to meet MRM requirements for O-2 is an average of about 52 kW, seasonally variable. The new mass estimate is 7898 kg, down from 13650 kg. The new estimate of oxygen content correspondingly reduces the amounts of by-products that can be recovered. CO, a primary fuel and propellant precursor, is produced at about 0.2 kg/kg O-2. Water, possibly available at about 0.04 kg/kg O-2, is believed not recoverable by the MARRS process at this lower level, even seasonally. An equation is provided for the seasonal variation in atmospheric O-2 fraction based on Viking pressure measurements. Oxygen varies seasonally from about 0.25% or 0.34%, the variability affecting plant design. While the higher O-2 fraction means reduced amounts of by-products from the MARRS process, large amounts of nitrogen (liquid and gas), argon gas and liquid carbon dioxide (CO2) remain available as by-products for use as respiratory agents, refrigerants, propellants, propellant precursors and working fluids for emergency or backup power, transportation, and surface operations such as drilling. C1 CALTECH, Jet Prop Lab, Propuls & Mat Engn Sect, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. Raytheon Polar Ser, Amundsen, Antarctica. RP CALTECH, Jet Prop Lab, Propuls & Mat Engn Sect, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM cengland@jpl.nasa.gov NR 10 TC 0 Z9 0 U1 1 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 1138 EP + PG 2 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600123 ER PT S AU Robertson, GA AF Robertson, GA BE ElGenk, MS TI Electromagnetic nonlinearity in the dielectric medium of experimental EM impulse-momentum systems SO Space Technology and Applications International Forum - STAIF 2006 SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Space Technology and Applications International Forum (STAIF 2006) CY FEB 12-16, 2006 CL Albuquerque, NM SP Lockheed Martin, Los Alamos Natl Lab, Oak Ridge Natl Lab, Sandia Natl Lab, Northrop Grumman Space Technol, Idaho Natl Lab, US DOE, AIAA, AIChE, ASME, NASA Natl Space Grant Coll & Fellowship Program, Profess Aerosp Contractors Assoc, Inst Space & Nucl Power Studies DE electromagnetics; impulse; momentum; magnetoelectrics; dielectrics ID INERTIA MANIPULATION; FLUX CAPACITORS; PROPULSION AB In this paper, an empirical correlation among electromagnetic (EM) impulse-momentum experiments performed by Brito (1999, 2003, 2004, and 2005), Woodward (2004a, 2004b, 2005, and 2006) and March (2006) is developed. This empirical correlation assumes that the dielectric medium exhibits non-linear magnetoelectric effects arising from the interplay of piezo-magnetism and piezo-electricity (Rado, 1975). The modification to the generally accepted electromagnetic field (volume) momentum equation (Jackson, 1999) is derived from Fiegel's (2004) thesis that inside a magnetoelectric, the momenta of counter-propagating vacuum modes do not eliminate each other, in contrast to the other materials. Whereby, a time independent vacuum mode component can be subtracted from the impulse-momentum to give a constant force. This vacuum mode component is interpreted as the nonlinearity of the dielectric medium with respect to the applied frequency of the input power. C1 NASA, MSFC, Prop Res Ctr, Huntsville, AL 35812 USA. RP Robertson, GA (reprint author), NASA, MSFC, Prop Res Ctr, Huntsville, AL 35812 USA. NR 21 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 0-7354-0305-8 J9 AIP CONF PROC PY 2006 VL 813 BP 1333 EP 1340 PG 8 WC Engineering, Aerospace; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA BDY47 UT WOS:000236123600146 ER PT S AU Stahl, HP AF Stahl, H. Philip BE Mather, JC MacEwen, HA DeGraauw, MWM TI Mirror technology roadmap for optical/IR/FIR space telescopes - art. no. 626504 SO Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation I - Optical, Infrared and Millimeter CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE mirror technology; space telescopes AB The NASA Advanced Telescope and Observatory (ATO) Capability Roadmap addresses technologies necessary for NASA to enable future space telescopes and observatories operating in all electromagnetic bands, from x-rays to millimeter waves, and including gravity-waves. It lists capability priorities derived from current and developing Space Missions Directorate (SMD) strategic roadmaps. Technology topics include optics; wavefront sensing and control and interferometry; distributed and advanced spacecraft systems; cryogenic and thermal control systems; large precision structure for observatories; and the infrastructure essential to future space telescopes and observatories. This paper summarizes optic technology capability requirements necessary to enable space telescopes from the UV to Far-Infared. C1 NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Stahl, HP (reprint author), NASA, Marshall Space Flight Ctr, Huntsville, AL 35812 USA. NR 8 TC 1 Z9 1 U1 1 U2 1 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6330-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6265 BP 26504 EP 26504 AR 626504 DI 10.1117/12.671958 PN 1-2 PG 9 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX66 UT WOS:000240025400003 ER PT S AU Werner, MW AF Werner, Michael W. BE Mather, JC MacEwen, HA DeGraauw, MWM TI The Spitzer Space Telescope: the first 30 months - art. no. 626507 SO Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation I - Optical, Infrared and Millimeter CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE infrared; Great Observatories; space telescope; cryogenics; infrared arrays ID BROWN DWARF; CIRCUMSTELLAR DISK; PERFORMANCE; GALAXIES; STARS AB We provide an overview of the design of the Spitzer Space Telescope and review scientific highlights from the first 30 months of on-orbit operations. C1 CALTECH, Jet Prop Lab, Astron & Phys Directorate, Pasadena, CA 91109 USA. RP Werner, MW (reprint author), CALTECH, Jet Prop Lab, Astron & Phys Directorate, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 14 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 0-8194-6330-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6265 BP 26507 EP 26507 AR 626507 DI 10.1117/12.671019 PN 1-2 PG 11 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX66 UT WOS:000240025400005 ER PT S AU Dean, BH Aronstein, DL Smith, JS Shiri, R Acton, DS AF Dean, Bruce H. Aronstein, David L. Smith, J. Scott Shiri, Ron Acton, D. Scott BE Mather, JC MacEwen, HA DeGraauw, MWM TI Phase retrieval algorithm for JWST flight and testbed telescope - art. no. 626511 SO Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation I - Optical, Infrared and Millimeter CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE phase; retrieval; JWST; wavefront; sensing; optical; control; segmented; mirror; TRL-6 ID DIFFRACTION PLANE PICTURES; WEBB-SPACE-TELESCOPE; IMAGE-RECONSTRUCTION; ADAPTIVE OPTICS; DIVERSITY; SELECTION; MODULUS; OBJECT; ERROR AB An image-based wavefront sensing and control algorithm for the James Webb Space Telescope (JWST) is presented. The algorithm heritage is discussed in addition to implications for algorithm performance dictated by NASA's Technology Readiness Level (TRL) 6. The algorithm uses feedback through an adaptive diversity function to avoid the need for phase-unwrapping post-processing steps. Algorithm results are demonstrated using JWST Testbed Telescope (TBT) commissioning data and the accuracy is assessed by comparison with interferometer results on a multi-wave phase aberration. Strategies for minimizing aliasing artifacts in the recovered phase are presented and orthogonal basis functions are implemented for representing wavefronts in irregular hexagonal apertures. Algorithm implementation on a parallel cluster of high-speed digital signal processors (DSPs) is also discussed. C1 NASA, Goddard Space Flight Ctr, Wavefront Sensing & Control Grp, Opt Branch, Greenbelt, MD 20771 USA. RP Dean, BH (reprint author), NASA, Goddard Space Flight Ctr, Wavefront Sensing & Control Grp, Opt Branch, Code 551, Greenbelt, MD 20771 USA. NR 69 TC 27 Z9 30 U1 2 U2 6 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6330-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6265 BP 26511 EP 26511 AR 626511 DI 10.1117/12.673569 PN 1-2 PG 17 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX66 UT WOS:000240025400031 ER PT S AU Davila, PS Bolcar, MR Bos, BJ Dean, B Hagopian, JG Howard, JM Unger, BL Wilson, ME AF Davila, Pamela S. Bolcar, Matthew R. Bos, Brent J. Dean, Bruce Hagopian, John G. Howard, Joseph M. Unger, Blair L. Wilson, Mark E. BE Mather, JC MacEwen, HA DeGraauw, MWM TI Focus determination for the James Webb Space Telescope Science Instruments: A Survey of Methods - art. no. 626512 SO Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation I - Optical, Infrared and Millimeter CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE james Webb Space Telescope; telescope; science instruments; focus; astronomy; space optics ID PHASE-RETRIEVAL; IMAGE-RECONSTRUCTION AB The James Webb Space Telescope (JWST) is a segmented deployable telescope that will require on-orbit alignment using the Near Infrared Camera as a wavefront sensor. The telescope will be aligned by adjusting seven degrees of freedom on each of 18 primary mirror segments and five degrees of freedom on the secondary mirror to optimize the performance of the telescope and camera at a wavelength of 2 microns. With the completion of these adjustments, the telescope focus is set and the optical performance of each of the other science instruments should then be optimal. This alignment approach requires confocality of the instruments after integration to the composite metering structure, which will be verified during instrument level testing at Goddard Space Flight Center with a telescope optical simulator. In this paper, we present the results from a study of several analytical approaches to determine the focus for each instrument. C1 Goddard Space Flight Ctr, Opt Branch Code 551, Greenbelt, MD 20771 USA. RP Davila, PS (reprint author), Goddard Space Flight Ctr, Opt Branch Code 551, Greenbelt Rd, Greenbelt, MD 20771 USA. NR 18 TC 1 Z9 1 U1 2 U2 3 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6330-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6265 BP 26512 EP 26512 AR 626512 DI 10.1117/12.673383 PN 1-2 PG 11 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX66 UT WOS:000240025400032 ER PT S AU Greenhouse, MA Boyce, LA Glazer, SD Johnson, EL McCloskey, JC Shears, LB Sullivan, PC Voyton, MF AF Greenhouse, Matthew A. Boyce, Leslye A. Glazer, Stuart D. Johnson, Eric L. McCloskey, John C. Shears, Lisa B. Sullivan, Pamela C. Voyton, Mark F. BE Mather, JC MacEwen, HA DeGraauw, MWM TI The James Webb Space Telescope Integrated Science Instrument Module - art. no. 626513 SO Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation I - Optical, Infrared and Millimeter CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE JWST; instrumentation AB The Integrated Science Instrument Module of the James Webb Space Telescope is described from a systems perspective with emphasis on unique and advanced technology aspects. The major subsystems of this flight element are described including: structure, thermal, command and data handling, and software. C1 Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Greenhouse, MA (reprint author), Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 0 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 0-8194-6330-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6265 BP 26513 EP 26513 AR 626513 DI 10.1117/12.671523 PN 1-2 PG 16 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX66 UT WOS:000240025400033 ER PT S AU Shao, M Levine, BM Wallace, JK Orton, GS Schmidtlin, E Lane, BF Seager, S Tolls, V Lyon, RG Samuele, R Tenerelli, DJ Woodruff, R Ge, J AF Shao, Michael Levine, Bruce Martin Wallace, James Kent Orton, Glenn S. Schmidtlin, Edouard Lane, Benjamin F. Seager, Sara Tolls, Volker Lyon, Richard G. Samuele, Rocco Tenerelli, Domenick J. Woodruff, Robert Ge, Jian BE Mather, JC MacEwen, HA DeGraauw, MWM TI A nulling coronagraph for TPF-C - art. no. 626517 SO Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation I - Optical, Infrared and Millimeter CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE exoplanets; terrestrial planets; nulling interferometry; coronography AB The nulling coronagraph is one of 5 instrument concepts selected by NASA for study for potential use in the TPF-C mission. This concept for extreme starlight suppression has two major components, a nulling interferometer to suppress the starlight to similar to 10(-10) per airy spot within 2 lambda/D of the star, and a calibration interferometer to measure the residual scattered starlight. The ability to work at 2 lambda/D dramatically improves the science throughput of a space based coronagraph like TPF-C. The calibration interferometer is an equally important part of the starlight suppression system. It measures the measures the wavefront of the scattered starlight with very high SNR, to 0.05 nm in less than 5 minutes on a 5mag star. In addition, the post coronagraph wavefront sensor will be used to measure the residual scattered light after the coronagraph and subtract it in post processing to 1 similar to 2x10(-11) to enable detection of an Earthlike planet with a SNR of 5 similar to 10. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Shao, M (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. NR 0 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 0-8194-6330-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6265 BP 26517 EP 26517 AR 626517 DI 10.1117/12.671934 PN 1-2 PG 13 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX66 UT WOS:000240025400035 ER PT S AU Rinehart, SA AF Rinehart, S. A. CA SPECS Mission Study Team BE Mather, JC MacEwen, HA DeGraauw, MWM TI SPECS: The submillimeter probe of the evolution of cosmic structure - art. no. 626520 SO Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation I - Optical, Infrared and Millimeter CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE Michelson interferometry; far-infrared; double-fourier ID INTERFEROMETRY AB The concept for the Submillimeter Probe of the Evolution of Cosmic Structure (SPECS) was investigated through NASA Vision Missions Program. In the course of this study, a compelling need for high spatial-resolution far-infrared/submillimeter observations with high angular resolution (50 milliarcseconds) was identified. In order to achieve these scientific goals, a kilometer-baseline far-infrared/submillimeter Michelson stellar interferometer is required, operating in the 40-640 Micron range with fully cryogenically cooled optics and photon-limited detectors. There are significant technological challenges to developing this mission, including controllable tethered flight, detector development, and large cryogenic mechanisms. We present here a concept for SPECS and discuss some of the relevant technical aspects of the mission. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Rinehart, SA (reprint author), NASA, Goddard Space Flight Ctr, Code 665, Greenbelt, MD 20771 USA. NR 12 TC 1 Z9 1 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6330-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6265 BP 26520 EP 26520 AR 626520 DI 10.1117/12.672038 PN 1-2 PG 12 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX66 UT WOS:000240025400060 ER PT S AU Mainzer, AK Eisenhardt, P Wright, EL Liu, FC Irace, W Heinrichsen, I Cutri, R Duval, V AF Mainzer, Amanda K. Eisenhardt, Peter Wright, Edward L. Liu, Feng-Chuan Irace, William Heinrichsen, Ingolf Cutri, Roc Duval, Valerie BE Mather, JC MacEwen, HA DeGraauw, MWM TI Update on the Wide-Field Infrared Survey Explorer (WISE) - art. no. 626521 SO Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation I - Optical, Infrared and Millimeter CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE infrared - brown dwarfs; ultraluminous galaxies; asteroids AB The Wide-field Infrared Survey Explorer (WISE), a NASA MIDEX mission, will survey the entire sky in four bands from 3.3 to 23 microns with a sensitivity 1000 times greater than the IRAS survey. The WISE survey will extend the Two Micron All Sky Survey into the thermal infrared and will provide an important catalog for the James Webb Space Telescope. Using 1024(2) HgCdTe and Si:As arrays at 3.3, 4.7, 12 and 23 microns, WISE will find the most luminous galaxies in the universe, the closest stars to the Sun, and it will detect most of the main belt asteroids larger than 3 km. The single WISE instrument consists of a 40 cm diamond-turned aluminum afocal telescope, a two-stage solid hydrogen cryostat, a scan mirror mechanism, and reimaging optics giving 5" resolution (full-width-half-maximum). The use of dichroics and beamsplitters allows four color images of a 47'x47' field of view to be taken every 8.8 seconds, synchronized with the orbital motion to provide total sky coverage with overlap between revolutions. WISE will be placed into a Sun-synchronous polar orbit on a Delta 7320-10 launch vehicle. The WISE survey approach is simple and efficient. The three-axis-stabilized spacecraft rotates at a constant rate while the scan mirror freezes the telescope line of sight during each exposure. WISE has completed its mission Preliminary Design Review and its NASA Confirmation Review, and the project is awaiting confirmation from NASA to proceed to the Critical Design phase. Much of the payload hardware is now complete, and assembly of the payload will occur over the next year. WISE is scheduled to launch in late 2009; the project web site can be found at www.wise.ssl.berkeley.edu. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Mainzer, AK (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 9 TC 6 Z9 6 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 0-8194-6330-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6265 BP 26521 EP 26521 AR 626521 DI 10.1117/12.672494 PN 1-2 PG 12 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX66 UT WOS:000240025400061 ER PT S AU Benford, DJ Lauer, TR AF Benford, Dominic J. Lauer, Tod R. BE Mather, JC MacEwen, HA DeGraauw, MWM TI Destiny: A candidate architecture for the joint dark energy mission - art. no. 626528 SO Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation I - Optical, Infrared and Millimeter CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE dark energy; supernova survey; weak lensing; Hubble diagram; near-infrared; grism imaging ID IA SUPERNOVAE AB Destiny is a simple, direct, low cost mission to determine the properties of dark energy by obtaining a cosmologically deep supernova (SN) type Ia Hubble diagram. Its science instrument is a 1.65m space telescope, featuring a grism-fed near-infrared (NIR) (0.85-1.7 mu m) survey camera/spectrometer with a 0.12 square degree field of view (FOV) covered by a mosaic of 16 2kx2k HgCdTe arrays. For maximum operational simplicity and instrument stability, Destiny will be deployed into a halo-orbit about the Second Sun-Earth Lagrange Point. During its two-year primary mission, Destiny will detect, observe, and characterize similar to 3000 SN la events over the redshift interval 0.4 < z < 1.7 within a 3 square degree survey area. In conjunction with ongoing ground-based SN Ia surveys for z < 0.8, Destiny mission data will be used to construct a high-precision Hubble diagram and thereby constrain the dark energy equation of state. The total range of redshift is sufficient to explore the expansion history of the Universe from an early time, when it was strongly matter-dominated, to the present when dark energy dominates. The grism-images will provide a spectral resolution of R equivalent to lambda/Delta lambda=75 spectrophotometry that will simultaneously. provide broad-band photometry, redshifts, and SN classification, as well as time-resolved diagnostic data, which is valuable for investigating additional SN luminosity diagnostics. Destiny will be used in its third year as a high resolution, wide-field imager to conduct a multicolor NIR weak lensing (WL) survey covering 1000 square degrees. The large-scale mass power spectrum derived from weak lensing distortions of field galaxies as a function of redshift will provide independent and complementary constraints on the dark energy equation of state. The combination of SN and WL is much more powerful than either technique on its own. Used together, these surveys will have more than an order of magnitude greater sensitivity (by the Dark Energy Task Force's (DETF) figure of merit) than will be provided by ongoing ground-based projects. The dark energy parameters, w(0) and w(a), will be measured to a precision of 0.05 and 0.2 respectively. C1 NASA, Goddard Space Flight Ctr, Observ Cosmol Lab, Greenbelt, MD 20771 USA. RP Benford, DJ (reprint author), NASA, Goddard Space Flight Ctr, Observ Cosmol Lab, Code 661, Greenbelt, MD 20771 USA. RI Benford, Dominic/D-4760-2012 OI Benford, Dominic/0000-0002-9884-4206 NR 15 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 0-8194-6330-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6265 BP 26528 EP 26528 AR 626528 DI 10.1117/12.672135 PN 1-2 PG 12 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX66 UT WOS:000240025400067 ER PT S AU Quijada, MA Boucarut, R Telfer, R Baggett, S Quijano, JK Allen, G Arsenovic, P AF Quijada, M. A. Boucarut, R. Telfer, R. Baggett, S. Quijano, J. Kim Allen, George Arsenovic, Peter BE Mather, JC MacEwen, HA DeGraauw, MWM TI Spectral and imaging performance of WFC3 interference filters - art. no. 626531 SO Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation I - Optical, Infrared and Millimeter CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE visible/UV; infrared; interference filters; transmittance; ghost images; transmitted wavefront error ID HUBBLE-SPACE-TELESCOPE AB The Wide Field Camera 3 (WFC3) is a panchromatic imager that will be deployed in the Hubble Space Telescope (HST). The mission of the WFC3 is to enhance the imaging capability of HST in the ultraviolet, visible and near-infrared spectral regions. Together with a wavelength coverage spanning 2000 Angstrom to 1.7 mu m, the WFC3 high sensitivity, high spatial resolution, and large field-of-view provide the astronomer with an unprecedented set of tools for exploring all types of exciting astrophysical terrain and for addressing many key questions in astronomy today. The filter complement, which includes broad, medium, and narrow band filters, naturally reflects the diversity of astronomical programs to be targeted with WFC3. The WFC3 holds 61 UVIS filter elements, 15 IR filters, and 3 dispersive elements. During ground testing, the majority of the UVIS filters were found to exhibit excellent performance consistent with or exceeding expectations. However, a subset of filters showed considerable ghost images; some with relative intensity as high as 10-15%. Replacement filters with band-defining coatings that substantially reduce these ghost images were designed and procured. A state-of-the-art characterization setup was developed to measure the intensity of ghost images, focal shift, wedge direction, transmitted uniformity and surface features of the filters. We will report on these filter characterization methods, as well as the spectral performance measurements of the in-band transmittance and blocking. C1 Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Quijada, MA (reprint author), Goddard Space Flight Ctr, Code 551, Greenbelt, MD 20771 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 0-8194-6330-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6265 BP 26531 EP 26531 AR 626531 DI 10.1117/12.672352 PN 1-2 PG 12 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX66 UT WOS:000240025400092 ER PT S AU Rauscher, BJ Boker, T Cabelli, C De Marchi, G Ferruit, P Garnett, J Hill, RJ Loose, M Regan, MW Waczynski, A Wen, YT Wong, S Zandian, M Alexander, D Brambora, CK Derro, R Dunn, C Ellis, T Garrison, MB Howe, B Jakobsen, P Johnson, TE Jurado, M Lee, G Manthripragada, SS Marsh, JM Marshall, C Martineau, RJ Mott, B Nieznanski, J Roher, WD Shakoorzadeh, KB Smith, MT Strada, P Wallis, P Wei, XS York, J AF Rauscher, Bernard J. Boker, Torsten Cabelli, Craig De Marchi, Guido Ferruit, Pierre Garnett, James Hill, Robert J. Loose, Markus Regan, Michael W. Waczynski, Augustyn Wen, Yiting Wong, Selmer Zandian, Majid Alexander, David Brambora, Clifford K. Derro, Rebecca Dunn, Carol Ellis, Timothy Garrison, Matthew B. Howe, Bryan Jakobsen, Peter Johnson, Thomas E. Jurado, Miriam Lee, Ginn Manthripragada, Sridhar S. Marsh, James M. Marshall, Cheryl Martineau, Robert J. Mott, Brent Nieznanski, John Roher, Wayne D. Shakoorzadeh, Kamdin B. Smith, Miles T. Strada, Paolo Wallis, Peter Wei Xia-Serafino York, James BE Mather, JC MacEwen, HA DeGraauw, MWM TI Detectors for the James Webb Space Telescope Near Infrared Spectrograph (NIRSpec) - art. no. 626538 SO Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation I - Optical, Infrared and Millimeter CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE James Webb Space Telescope; JWST; NIRSpec; detector; HAWAII-2RG; SIDECAR AB The Near Infrared Spectrograph (NIRSpec) will be the James Webb Space Telescope's (JWST's) primary near-infrared spectrograph. NIRSpec is a multi-object spectrograph with fixed-slit and integral field modes. EADS/Astrium is building NIRSpec for the European Space Agency (ESA), with NASA is providing the detector subsystem and programmable multi-aperture mask. In this paper, we summarize recent progress on the detector subsystem including tests demonstrating that JWST's Rockwell HAWAII-2RG sensor chip assemblies have achieved Technology Readiness Level 6 (TRL-6). Achieving TRL-6 is an important milestone because TRL-6 is required for flight. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Rauscher, BJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 2 TC 1 Z9 1 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6330-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6265 BP 26538 EP 26538 AR 626538 DI 10.1117/12.668489 PN 1-2 PG 7 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX66 UT WOS:000240025400099 ER PT S AU Leisawitz, D Baker, C Barger, A Benford, D Blain, A Boyle, R Broderick, R Budinoff, J Carpenter, J Caverly, R Chen, P Cooley, S Cottingham, C Crooke, J DiPietro, D DiPirro, M Femiano, M Ferrera, A Fischer, J Gardner, J Hallock, L Harris, K Hartman, K Harwit, M Hillenbrand, L Hyde, T Jones, D Kellogg, J Kogut, A Kuchner, M Lawson, B Lecha, J Lecha, M Mainzer, A Mannion, J Martino, A Mason, P Mather, J McDonald, G Mills, R Mundy, L Ollendorf, S Pellicciotti, J Quinn, D Rhee, K Rinehart, S Sauerwine, T Silverberg, R Smith, T Stacey, G Stahl, HP Staguhn, J Tompkins, S Tveekrem, J Wall, S Wilson, M AF Leisawitz, David Baker, Charles Barger, Amy Benford, Dominic Blain, Andrew Boyle, Rob Broderick, Richard Budinoff, Jason Carpenter, John Caverly, Richard Chen, Phil Cooley, Steve Cottingham, Christine Crooke, Julie DiPietro, Dave DiPirro, Mike Femiano, Michael Ferrera, Art Fischer, Jackie Gardner, Jonathan Hallock, Lou Harris, Kenny Hartman, Kate Harwit, Martin Hillenbrand, Lynne Hyde, Tupper Jones, Drew Kellogg, Jim Kogut, Alan Kuchner, Marc Lawson, Bill Lecha, Javier Lecha, Maria Mainzer, Amy Mannion, Jim Martino, Anthony Mason, Paul Mather, John McDonald, Gibran Mills, Rick Mundy, Lee Ollendorf, Stan Pellicciotti, Joe Quinn, Dave Rhee, Kirk Rinehart, Stephen Sauerwine, Tim Silverberg, Robert Smith, Terry Stacey, Gordon Stahl, H. Philip Staguhn, Johannes Tompkins, Steve Tveekrem, June Wall, Sheila Wilson, Mark BE Mather, JC MacEwen, HA DeGraauw, MWM TI The Space Infrared Interferometric Telescope (SPIRIT): mission study results - art. no. 626540 SO Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation I - Optical, Infrared and Millimeter CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE infrared; submillimeter; interferometry; infrared detectors; cryogenic optics; Origins Probe ID SPECTROSCOPY; GALAXIES; DISKS AB We report results of a recently-completed pre-Formulation Phase study of SPIRIT, a candidate NASA Origins Probe mission. SPIRIT is a spatial and spectral interferometer with an operating wavelength range 25 - 400 mu m. SPIRIT will provide sub-arcsecond resolution images and spectra with resolution R = 3000 in a 1 arcmin field of view to accomplish three primary scientific objectives: (1) Learn how planetary systems form from protostellar disks, and how they acquire their chemical organization; (2) Characterize the family of extrasolar planetary systems by imaging the structure in debris disks to understand how and where planets form, and why some planets are ice giants and others are rocky; and (3) Learn how high-redshift galaxies formed and merged to form the present-day population of galaxies. Observations with SPIRIT will be complementary to those of the James Webb Space Telescope and the ground-based Atacama Large Millimeter Array. All three observatories could be operational contemporaneously. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Leisawitz, D (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RI Benford, Dominic/D-4760-2012; Kuchner, Marc/E-2288-2012 OI Benford, Dominic/0000-0002-9884-4206; NR 28 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 0-8194-6330-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6265 BP 26540 EP 26540 AR 626540 DI 10.1117/12.669820 PN 1-2 PG 18 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX66 UT WOS:000240025400120 ER PT S AU Goldsmith, P Khayatian, B Bradford, M Dragovan, M Hoppe, D Imbriale, W Lee, R Paine, C Turner, P Yorke, H Zmuidzinas, J AF Goldsmith, Paul Khayatian, Behrouz Bradford, Matt Dragovan, Mark Hoppe, Daniel Imbriale, William Lee, Roger Paine, Chris Turner, Philip Yorke, Harold Zmuidzinas, Jonas BE Mather, JC MacEwen, HA DeGraauw, MWM TI Analysis of the optical design for the SAFIR telescope - art. no. 62654A SO Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation I - Optical, Infrared and Millimeter CY MAY 24-31, 2006 CL Orlando, FL SP SPIE AB SAFIR, the Single Aperture Far Infra Red Observatory, is a very powerful space mission that will achieve background-limited sensitivity in the far infrared-submillimeter spectral region. Many processes of enormous interest to astronomers can best be studied in this wavelength range, but require the demanding combination of high sensitivity, good angular resolution, and spectroscopic capability. SAFIR is a 10m class telescope offering good angular resolution, cooled to below 5 K in order to achieve background-limited sensitivity, and equipped with a complement of large-format cameras and broadband spectrometers. Successful operation of such a facility is critically dependent on achieving the level of sensitivity expected, but this is rendered difficult by potential pickup from unwanted sources of radiation. This problem is exacerbated by the fact that the emission from the optical system itself is minimal due to its low temperature, thus emphasizing the importance of minimizing pickup from unwanted astronomical sources of radiation, including the emission from dust in our solar system (analogous to the zodiacal light, hence "zodi"), and the emission from warm dust in the Milky Way (Galactic "cirrus"). The extreme sensitivity of SAFIR to these unwanted sources of radiation makes it essential to understand the relative sensitivity of the telescope/detector system to radiation coming from angles far outside the main beam, and to develop designs which minimize this pickup. In this paper we analyze in some detail the relative telescope sensitivity (referred to as the antenna pattern by microwave engineers) for different designs of SAFIR. These calculations include edge diffraction from the secondary and primary reflector, and also the effect of blockage by the secondary and blockage and scattering by support legs in a symmetric system. By convolving the antenna pattern with the brightness of the sky due to the zodi and cirrus, we can calculate the power received when the antenna is pointed in any specified direction. We can also compare the undesired pickup for different designs, in particular symmetric vs. asymmetric (off-axis or unblocked) antenna configurations. These considerations are vital for achieving the most efficient SAFIR design possible, in terms of achieving maximum sensitivity while being able to observe over a large fraction of the sky. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Goldsmith, P (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 5 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 0-8194-6330-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6265 BP A2654 EP A2654 AR 62654A DI 10.1117/12.670051 PN 1-2 PG 13 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX66 UT WOS:000240025400130 ER PT S AU Clampin, M Melnick, G Lyon, R Kenyon, S Sasselov, D Tolls, V Ford, H Golimowski, D Petro, L Hartig, G Sparks, W Illingworth, G Lin, D Seager, S Weinberger, A Harwit, M Marley, M Schneider, J Shao, M Levine, M Ge, J Woodruff, R AF Clampin, Mark Melnick, Gary Lyon, Richard Kenyon, Scott Sasselov, Dimitar Tolls, Volker Ford, Holland Golimowski, David Petro, Larry Hartig, George Sparks, William Illingworth, Garth Lin, Doug Seager, Sara Weinberger, Alycia Harwit, Martin Marley, Mark Schneider, Jean Shao, Michael Levine, Marty Ge, Jian Woodruff, Robert BE Mather, JC MacEwen, HA DeGraauw, MWM TI Extrasolar Planetary Imaging Coronagraph (EPIC) - art. no. 62651B SO Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation I - Optical, Infrared and Millimeter CY MAY 24-31, 2006 CL Orlando, FL SP SPIE AB The Extrasolar Planetary Imaging Coronagraph (EPIC) is a proposed NASA Discovery mission to image and characterize extrasolar giant planets in orbits with semi-major axes between 2 and 10 AU. EPIC will provide insights into the physical nature of a variety of planets in other solar systems complimenting radial velocity (RV) and astrometric planet searches. It will detect and characterize the atmospheres of planets identified by radial velocity surveys, determine orbital inclinations and masses, characterize the atmospheres around A and F type stars which cannot be found with RV techniques, and observe the inner spatial structure and colors of debris disks. EPIC has a proposed launch date of 2012 to heliocentric Earth trailing drift-away orbit, with a 3 year mission lifetime (5 year goal), and will revisit planets at least three times at intervals of 9 months. The robust mission design is simple and flexible ensuring mission success while minimizing cost and risk. The science payload consists of a heritage optical telescope assembly (OTA), and visible nulling coronagraph (VNC) instrument. The instrument achieves a contrast ratio of 109 over a 4.84 arcsecond field-of-view with an unprecedented inner working angle of 0.14 arcseconds over the spectral range of 440-880 nm, with spectral resolutions from 10-150. The telescope is a 1.5 meter off-axis Cassegrain with an OTA wavefront error of theta/9, which when coupled to the VNC greatly reduces the requirements on the large scale optics, compressing them to stability requirements within the relatively compact VNC optical chain. The VNC features two integrated modular millers, a spatial filter array (SFA), and an E2V-L3 photon counting CCD. Direct null control is accomplished from the science focal mitigating against complex wavefront and amplitude sensing and control strategies. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Clampin, M (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RI Clampin, mark/D-2738-2012; Lyon, Richard/D-5022-2012; Marley, Mark/I-4704-2013; OI Petro, Larry/0000-0001-8879-528X NR 2 TC 5 Z9 5 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6330-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6265 BP B2651 EP B2651 AR 62651B DI 10.1117/12.672849 PN 1-2 PG 7 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX66 UT WOS:000240025400038 ER PT S AU Oegerle, WR Purves, LR Budinoff, JG Moe, RV Carnahan, TM Evans, DC Kim, CK AF Oegerle, W. R. Purves, L. R. Budinoff, J. G. Moe, R. V. Carnahan, T. M. Evans, D. C. Kim, C. K. BE Mather, JC MacEwen, HA DeGraauw, MWM TI Concept for a large scalable space telescope: In-space assembly - art. no. 62652C SO Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation I - Optical, Infrared and Millimeter CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE large space telescopes; robotic assembly; orbital assembly AB We present a conceptual design for a scalable (10-50 meter segmented filled-aperture) space observatory operating at UV-optical-near infrared wavelengths. This telescope is designed for assembly in space by robots, astronauts or a combination of the two, as envisioned in NASA's Vision for Space Exploration. Our operations concept for this-space telescope provides for assembly and check-out in an Earth Moon L2 (EML2) orbit, and transport to a Sun-Earth L2 (SEL2) orbit for science operations and routine servicing, with return to EML2 for major servicing. We have developed and analyzed initial designs for the optical, structural, thermal and attitude control systems for a 30-m aperture space telescope. We further describe how the separate components are packaged for launch by heavy lift vehicle(s) and the approach for the robot assembly of the telescope from these components. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Oegerle, WR (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI Oegerle, William/C-9070-2012 NR 10 TC 3 Z9 3 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 0-8194-6330-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6265 BP C2652 EP C2652 AR 62652C DI 10.1117/12.672244 PN 1-2 PG 12 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX66 UT WOS:000240025400070 ER PT S AU Kegley, J Baker, M Carpenter, J Eng, R Haight, H Hogue, W McCracken, J Russell, K Siler, R Wright, E AF Kegley, Jeff Baker, Mark Carpenter, Jay Eng, Ron Haight, Harlan Hogue, William McCracken, Jeff Russell, Kevin Siler, Richard Wright, Ernie BE Mather, JC MacEwen, HA DeGraauw, MWM TI Improved cryogenic testing capability at Marshall Space Flight Center's X-ray Cryogenic Facility - art. no. 62654E SO Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation I - Optical, Infrared and Millimeter CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE cryogenic; test; XRCF; JWST AB Marshall Space Flight Center's X-ray Cryogenic Facility (XRCF) has been performing optical wavefront testing and thermal structural deformation testing at sub-liquid nitrogen cryogenic temperatures since 1999. Recent modifications have been made to the facility in support of the James Webb Space Telescope (JWST) program. The test article envelope and the chamber's refrigeration capacity have both been increased. A new larger helium-cooled enclosure has been added to the existing enclosure increasing both the cross-sectional area and the length. This new enclosure is capable of supporting six JWST Primary Mirror Segment Assemblies. A second helium refrigeration system has been installed essentially doubling the cooling capacity available at the facility. Modifications have also been made to the optical instrumentation area. Improved access is now available for both the installation and operation of optical instrumentation outside the vacuum chamber. Chamber configuration, specifications, and performance data will be presented. C1 NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Kegley, J (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 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 0-8194-6330-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6265 BP E2654 EP E2654 AR 62654E DI 10.1117/12.672096 PN 1-2 PG 8 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX66 UT WOS:000240025400134 ER PT S AU Dean, BH Smith, JS Budinoff, JG Feinberg, L AF Dean, Bruce H. Smith, Jeff S. Budinoff, Jason G. Feinberg, Lee BE Mather, JC MacEwen, HA DeGraauw, MWM TI Wavefront sensing and control architecture for the spherical primary optical telescope (SPOT) - art. no. 62654F SO Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation I - Optical, Infrared and Millimeter CY MAY 24-31, 2006 CL Orlando, FL SP SPIE AB Testbed results are presented demonstrating high-speed image-based wavefront sensing and control for a spherical primary optical telescope (SPOT). The testbed incorporates a phase retrieval camera coupled to a 3-Mirror Vertex testbed (3MV) at the NASA Goddard Space Flight Center. Actuator calibration based on the Hough transform is discussed as well as several supercomputing architectures for image-based wavefront sensing. Timing results are also presented based on various algorithm implementations using a cluster-of 64 TigerSharc TS101 DSP's (digital-signal processors). C1 NASA, Goddard Space Flight Ctr, Opt Branch, Greenbelt, MD 20771 USA. RP Dean, BH (reprint author), NASA, Goddard Space Flight Ctr, Opt Branch, Code 551, Greenbelt, MD 20771 USA. NR 22 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 0-8194-6330-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6265 BP F2654 EP F2654 AR 62654F DI 10.1117/12.673450 PN 1-2 PG 10 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX66 UT WOS:000240025400135 ER PT S AU Haguenauer, P Serabyn, E Mennesson, B Wallace, JK Gappinger, RO Troy, M Bloemhof, EE Moore, J Koresko, CD AF Haguenauer, Pierre Serabyn, Eugene Mennesson, Bertrand Wallace, James K. Gappinger, Robert O. Troy, Mitchell Bloemhof, Eric E. Moore, Jim Koresko, Chris D. BE Mather, JC MacEwen, HA DeGraauw, MWM TI Astronomical near-neighbor detection with a four-quadrant phase mask (FQPM) coronagraph - art. no. 62651G SO Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation I - Optical, Infrared and Millimeter CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE coronagraphy; phase mask ID STELLAR CORONAGRAPH; APODIZATION; PERFORMANCE; PUPILS AB Direct detection of planets around nearby stars requires the development of high-contrast imaging techniques, because of their very different respective fluxes. We thus investigated the innovative coronagraphic approach based on the use of a four-quadrant phase mask (FQPM). Simulations showed that, combined with high-level wavefront correction on an unobscured off-axis section of a large telescope, this method allows high-contrast imaging very close to stars, with detection capability superior to that of a traditional coronagraph. A FQPM instrument was thus built to test the feasibility of near-neighbor observations with our new off-axis approach on a ground-based telescope. In June 2005, we deployed our instrument to the Palomar 200-inch telescope, using existing facilities as much as possible for rapid implementation. In these initial observations, using data processing techniques specific to FQPM coronagraphs, we reached extinction levels of the order of 200:1. Here we discuss our simulations and on-sky results obtained so far. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Haguenauer, P (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 17 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 0-8194-6330-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6265 BP G2651 EP G2651 AR 62651G DI 10.1117/12.672595 PN 1-2 PG 10 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX66 UT WOS:000240025400043 ER PT S AU Dean, BH Bos, BJ AF Dean, Bruce H. Bos, Brent J. BE Mather, JC MacEwen, HA DeGraauw, MWM TI Wave-optics analysis of pupil imaging - art. no. 62653H SO Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation I - Optical, Infrared and Millimeter CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE wave optics; pupil imaging; diffraction analysis; wave front sensing; JWST AB Pupil imaging performance is analyzed from the perspective of physical optics. A multi-plane diffraction model is constructed by propagating the scalar electromagnetic field, surface by surface, along the optical path comprising the pupil imaging optical system. Modeling results are compared with pupil images collected in the laboratory. The experimental setup, although generic for pupil imaging systems in general, has application to the James Webb Space Telescope (JWST) optical system characterization where the pupil images are used as a constraint to the wavefront sensing and control process. Practical design considerations follow from the diffraction modeling which are discussed in the context of the JWST Observatory. C1 NASA, Goddard Space Flight Ctr, Opt Branch, Greenbelt, MD 20771 USA. RP Dean, BH (reprint author), NASA, Goddard Space Flight Ctr, Opt Branch, Code 551, Greenbelt, MD 20771 USA. NR 16 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 0-8194-6330-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6265 BP H2653 EP H2653 AR 62653H DI 10.1117/12.673572 PN 1-2 PG 11 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX66 UT WOS:000240025400106 ER PT S AU Shaklan, SB Green, JJ Palacios, DM AF Shaklan, Stuart B. Green, Joseph J. Palacios, David M. BE Mather, JC MacEwen, HA DeGraauw, MWM TI The Terrestrial Planet Finder Coronagraph optical surface requirements - art. no. 62651I SO Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation I - Optical, Infrared and Millimeter CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE coronagraph; high-contrast imaging; telescope requirements ID SYSTEMS; PHASE AB We derive the requirements on the surface height uniformity and reflectivity uniformity of the Terrestrial Planet Finder Coronagraph telescope and instrument optics for spatial frequencies within and beyond the spatial control bandwidth of the wave front control system. Three different wave front control systems are considered: a zero-path difference Michelson interferometer with two deformable mirrors at a pupil image; a sequential pair of deformable mirrors with one placed at a pupil image; and the Visible Nuller spatially-filtered controller. We show that the optical bandwidth limits the useful outer working angle. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. RP Shaklan, SB (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. NR 17 TC 9 Z9 9 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 0-8194-6330-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6265 BP I2651 EP I2651 AR 62651I DI 10.1117/12.670124 PN 1-2 PG 12 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX66 UT WOS:000240025400044 ER PT S AU Barry, RK Danch, WC Deming, LD Richardson, LJ Kuchner, MJ Seager, S Frey, BJ Martino, AJ Lee, KA Zuray, M Rajagopal, J Hyde, TT Millan-Gabet, R Monnier, JD Allen, RJ Traub, WA AF Barry, R. K. Danch, W. C. Deming, L. D. Richardson, L. J. Kuchner, M. J. Seager, S. Frey, B. J. Martino, A. J. Lee, K. A. Zuray, M. Rajagopal, J. Hyde, T. T. Millan-Gabet, R. Monnier, J. D. Allen, R. J. Traub, W. A. BE Mather, JC MacEwen, HA DeGraauw, MWM TI The Fourier-Kelvin Stellar Interferometer - A low complexity, low cost space mission for high-resolution astronomy and direct exoplanet detection - art. no. 62651L SO Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation I - Optical, Infrared and Millimeter CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE nulling interferometer; symmetric Mach-Zehnder nuller; extrasolar planets; giant planets; planet formation; debris disk; habitable zone AB The Fourier-Kelvin Stellar Interferometer (FKSI) is a mission concept for a spacecraft-borne nulling interferometer for high-resolution astronomy and the direct detection of exoplanets and assay of their environments and atmospheres. FKSI is a high angular resolution system operating in the near to mid-infrared spectral region and is a scientific and technological pathfinder to the Darwin and Terrestrial Planet Finder (TPF) missions. The instrument is configured with an optical system consisting, depending on configuration, of two 0.5 - 1.0 m telescopes on a 12.5 - 20 m boom feeding a symmetric, dual Mach-Zehnder beam combiner. We report on progress on our nulling testbed including the design of an optical pathlength null-tracking control system and development of a testing regime for hollow-core fiber waveguides proposed for use in wavefront cleanup. We also report results of integrated simulation studies of the planet detection performance of FKSI and results from an in-depth control system and residual optical pathlength jitter analysis. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Barry, RK (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI Kuchner, Marc/E-2288-2012 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 0-8194-6330-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6265 BP L2651 EP L2651 AR 62651L DI 10.1117/12.672437 PN 1-2 PG 12 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX66 UT WOS:000240025400046 ER PT S AU Sidick, E Shi, F Basinger, S Moody, D Lowman, AE Kuhnert, AC Tauger, JT AF Sidick, Erkin Shi, Fang Basinger, Scott Moody, Dwight Lowman, Andrew E. Kuhnert, Andreas C. Tauger, John T. BE Mather, JC MacEwen, HA DeGraauw, MWM TI Performance of TPF's high-contrast imaging testbed: Modeling and simulations - art. no. 62653L SO Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation I - Optical, Infrared and Millimeter CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE TPF; integrated modeling; speckle-nulling; high-contrast coronagraph ID PLANET FINDER CORONAGRAPH AB The performance of the high-contrast imaging testbed (HCIT) at JPL is investigated through optical modeling and simulations. The analytical tool is an optical simulation algorithm developed by combining the HCIT's optical model with a speckle-nulling algorithm that operates directly on coronagraphic images, an algorithm identical to the one currently being used on the HCIT to actively suppress scattered light via a deformable mirror. It is capable of performing full three-dimensional end-to-end near-field diffraction analysis on the HCIT's optical system. By conducting extensive speckle-nulling optimization, we clarify the HCIT's capability and limitations in terms of its contrast performance under various realistic conditions. Considered cases include non-ideal occulting masks, such as a mask with parasitic phase-delay errors (i.e., a not band-limited occulting mask) and one with damped ripples in its transmittance profiles, as well as the phase errors of all optics. Most of the information gathered on the HCIT's optical components through measurement and characterization over the last several years at JPL has been used in this analysis to make the predictions as accurate as possible. Our simulations predict that the contrast values obtainable on the HCIT with narrow-band (monochromatic) illumination at 785nm wavelength are C-m=1.58x10(-11) (mean) and C-4=5.11x10(-11) (at 4 lambda/D), in contrast to the measured results of C-m similar to 6x10(-10) and C-4 similar to 8x10(-10), respectively. In this paper we report our findings about the monochromatic light performance of the HCIT. We will describe the results of our investigation about the HCIT's broad-band performance in an upcoming paper. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Sidick, E (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 9 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 0-8194-6330-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6265 BP L2653 EP L2653 AR 62653L DI 10.1117/12.670524 PN 1-2 PG 12 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX66 UT WOS:000240025400108 ER PT S AU Balasubramanian, K Echternach, PM Dickie, MR Muller, RE White, VE Hoppe, DJ Shaklan, SB Belikov, R Kasdin, NJ Vanderbei, RJ Ceperley, D Neureuther, AR AF Balasubramanian, Kunjithapatham Echternach, Pierre M. Dickie, Matthew R. Muller, Richard E. White, Victor E. Hoppe, Daniel J. Shaklan, Stuart B. Belikov, Ruslan Kasdin, N. Jeremy Vanderbei, Robert J. Ceperley, Daniel Neureuther, Andrew R. BE Mather, JC MacEwen, HA DeGraauw, MWM TI Fabrication and characteristics of free standing shaped pupil masks for TPF-Coronagraph - art. no. 62653N SO Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation I - Optical, Infrared and Millimeter CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE Terrestrial Planet Finder; Coronagraph; shaped pupil mask; DRIE AB Direct imaging and characterization of exo-solar terrestrial planets require coronagraphic instruments capable of suppressing star light to 10(-10). Pupil shaping masks have been proposed and designed(1) at Princeton University to accomplish such a goal. Based on Princeton designs, free standing (without a substrate) silicon masks have been fabricated with lithographic and deep etching techniques. In this paper, we discuss the fabrication of such masks and present their physical and optical characteristics in relevance to their performance over the visible to near IR bandwidth. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Balasubramanian, K (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 13 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 0-8194-6330-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6265 BP N2653 EP N2653 AR 62653N DI 10.1117/12.673251 PN 1-2 PG 9 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX66 UT WOS:000240025400110 ER PT S AU Frey, BJ Barry, RK Danchi, WC Hyde, TT Lee, KY Martino, AJ Zuray, MS AF Frey, B. J. Barry, R. K. Danchi, W. C. Hyde, T. T. Lee, K. Y. Martino, A. J. Zuray, M. S. BE Mather, JC MacEwen, HA DeGraauw, MWM TI The Fourier-Kelvin Stellar Interferometer (FKSI) nulling testbed II: closed-loop path length metrology and control subsystem - art. no. 62651N SO Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation I - Optical, Infrared and Millimeter CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE nulling interferometer; symmetric Mach-Zehnder; metrology; closed-loop; extrasolar planets AB The Fourier-Kelvin Stellar Interferometer (FKSI) is a mission concept for an imaging and nulling interferometer in the near to mid-infrared spectral region (3-8 microns), and will be a scientific and technological pathfinder for upcoming missions including TPF-I/DARWIN, SPECS, and SPIRIT. At NASA's Goddard Space Flight Center, we have constructed a symmetric Mach-Zehnder nulling testbed to demonstrate techniques and algorithms that can be used to establish and maintain the 10(4) null depth that will be required for such a mission. Among the challenges inherent in such a system is the ability to acquire and track the null fringe to the desired depth for timescales on the order of hours in a laboratory environment. In addition, it is desirable to achieve this stability without using conventional dithering techniques. We describe recent testbed metrology and control system developments necessary to achieve these goals and present our preliminary results. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Frey, BJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 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 0-8194-6330-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6265 BP N2651 EP N2651 AR 62651N DI 10.1117/12.672467 PN 1-2 PG 8 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX66 UT WOS:000240025400048 ER PT S AU Gardner, JP Mather, JC Clampin, M Doyon, R Greenhouse, MA Hammel, HB Hutchings, JB Jakobsen, P Lilly, SJ Long, KS Lunine, JI McCaughrean, MJ Mountain, M Nella, J Rieke, GH Rieke, MJ Rix, HW Smith, EP Sonneborn, G Stiavelli, M Stockman, HS Windhorst, RA Wright, GS AF Gardner, Jonathan P. Mather, John C. Clampin, Mark Doyon, Rene Greenhouse, Matthew A. Hammel, Heidi B. Hutchings, John B. Jakobsen, Peter Lilly, Simon J. Long, Knox S. Lunine, Jonathan I. McCaughrean, Mark J. Mountain, Matt Nella, John Rieke, George H. Rieke, Marcia J. Rix, Hans-Walter Smith, Eric P. Sonneborn, George Stiavelli, Massimo Stockman, H. S. Windhorst, Rogier A. Wright, Gillian S. BE Mather, JC MacEwen, HA DeGraauw, MWM TI Science with the James Webb Space Telescope - art. no. 62650N SO Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation I - Optical, Infrared and Millimeter CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE JWST; Webb; space telescope; infrared; science; instrumentation ID INITIAL MASS FUNCTION; STAR-FORMATION; MOLECULAR CLOUDS; AMBIPOLAR DIFFUSION; COLLAPSE; FRAGMENTATION; EXTINCTION; SUPERNOVAE; TURBULENT; EVOLUTION AB The scientific capabilities of the James Webb Space Telescope (JWST) fall into four themes. The End of the Dark Ages: First Light and Reionization theme seeks to identify the first luminous sources to form and to determine the ionization history of the universe. The Assembly of Galaxies theme seeks to determine how galaxies and the dark matter, gas, stars, metals, morphological structures, and active nuclei within them evolved from the epoch of reionization to the present. The Birth of Stars and Protoplanetary Systems theme seeks to unravel the birth and early evolution of stars, from infall onto dust-enshrouded protostars, to the genesis of planetary systems. Planetary Systems and the Origins of Life theme seeks to determine the physical and chemical properties of planetary systems around nearby stars and of our own, and investigate the potential for life in those systems. To enable these for science themes, JWST will be a large (6.5m) cold (50K) telescope with four instruments, capable of imaging and spectroscopy from 0.6 to 29 microns wavelength. C1 Goddard Space Flight Ctr, Lab Observ Cosmol, Greenbelt, MD 20771 USA. RP Gardner, JP (reprint author), Goddard Space Flight Ctr, Lab Observ Cosmol, Code 665, Greenbelt, MD 20771 USA. RI Clampin, mark/D-2738-2012 NR 31 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 0-8194-6330-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6265 BP N2650 EP N2650 AR 62650N DI 10.1117/12.670492 PN 1-2 PG 12 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX66 UT WOS:000240025400017 ER PT S AU Bly, VT Nowak, MD Moore, DO AF Bly, Vincent T. Nowak, Maria D. Moore, David O. BE Mather, JC MacEwen, HA DeGraauw, MWM TI Lightweight instrument mirrors from single crystal silicon - art. no. 62652O SO Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation I - Optical, Infrared and Millimeter CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE silicon; single crystal silicon; silicon mirrors; lightweight mirrors; instrument mirrors AB We describe a process for fabricating lightweight mirrors from single crystal silicon. We also report ambient and cryogenic test results on a variety of mirrors made by this process. Each mirror is a monolithic structure from a single crystal of silicon. Masses are typically 1/3rd to 1/4th that of an equal diameter solid quartz mirror. We avoid print through of the supporting structure by lightweighting after the optical surface has been formed. Because of the extraordinary homogeneity of single crystal silicon, distortion of the optical surface by the lightweighting process is negligible for most applications (< 1/40th wave RMS @ 633mn). This homogeneity also accounts for the near zero distortion at cryogenic temperatures. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Bly, VT (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 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 0-8194-6330-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6265 BP O2652 EP O2652 AR 62652O DI 10.1117/12.672210 PN 1-2 PG 10 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX66 UT WOS:000240025400081 ER PT S AU Clampin, M Lyon, R Petro, L Seager, S Marley, M Melnick, G Weinberger, A Woodruff, R Horner, S Ford, H Illingworth, G Kasting, J Lin, D Kuchner, M Shao, M Sparks, W Rauscher, B Tolls, V Carter, R AF Clampin, Mark Lyon, Richard Petro, Larry Seager, Sara Marley, Mark Melnick, Gary Weinberger, Alycia Woodruff, Robert Horner, Scott Ford, Holland Illingworth, Garth Kasting, Jim Lin, Doug Kuchner, Marc Shao, Mike Sparks, William Rauscher, Bernard Tolls, Volker Carter, Ruth BE Mather, JC MacEwen, HA DeGraauw, MWM TI Coronagraphic exploration camera (CorECam) - art. no. 62650O SO Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation I - Optical, Infrared and Millimeter CY MAY 24-31, 2006 CL Orlando, FL SP SPIE AB The CorECam Instrument Concept Study (ICS) addressed the requirements and science program for the Terrestrial Planet Finder Coronagraph's (TPF-C) primary camera. CorECam provides a simple interface to TPF-C's Starlight Suppression System (SSS) which would be provided by the TPF-C Program, and comprises camera modules providing visible, and near-infrared (NIR) camera focal plane imaging. In its primary operating mode, CorECam will conduct the core science program of TPF-C, detecting terrestrial planets at visible wavelengths. CorECam additionally provides the imaging capabilities to characterize terrestrial planets, and conduct an extended science program focused on investigating the nature of the exosolar systems in which terrestrial planets are detected. In order to evaluate the performance of CorECam we developed a comprehensive, end-to-end model using OSCAR which has provided a number of key conclusions on the robustness of the TPF-C baseline design, and allows investigation of alternative techniques for wavefront sensing and control. CorECam recommends photon counting detectors be baselined for imaging with TPF-C since they provide mitigations against the background radiation environment, improved sensitivity and facilitate alternative WFSC approaches. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RP Clampin, M (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD USA. RI Clampin, mark/D-2738-2012; Kuchner, Marc/E-2288-2012; Lyon, Richard/D-5022-2012; Marley, Mark/I-4704-2013; OI Petro, Larry/0000-0001-8879-528X NR 3 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6330-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6265 BP O2650 EP O2650 AR 62650O DI 10.1117/12.672816 PN 1-2 PG 12 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX66 UT WOS:000240025400018 ER PT S AU Krist, J Trauger, J Moody, D AF Krist, John Trauger, John Moody, Dwight BE Mather, JC MacEwen, HA DeGraauw, MWM TI Studying a simple TPF-C - art. no. 62653O SO Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation I - Optical, Infrared and Millimeter CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE Terrestrial Planet Finder; coronagraph; optical modeling ID SPACE AB The NASA Terrestrial Planet Finder Coronagraph (TPF-C) mission envisions using a space telescope with an approximately 8 m by 3 m diameter primary mirror to image and spectroscopically characterize at visible wavelengths Earth-like planets orbiting nearby stars. Such terrestrial planets have intensities of 100 relative to their stars at separations of a fraction of an arcsecond, requiring extremely high-contrast imaging capabilities. A simple optical system with a minimal number of surfaces will likely have the best chance to image a very faint source near a bright star. A proposed version of a TPF-C integrated starlight suppression system and camera called SpeckleCam encompasses such a design. It incorporates two high-density deformable mirrors to control phase and amplitude wavefront errors, a coronagraph to suppress the stellar diffraction pattern, and simultaneous imaging in three passbands. We use the SpeckleCam concept to examine the utility of the PROPER modeling package, a set of IDL routines that simulate wavefront propagation in an optical system. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Krist, J (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 0-8194-6330-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6265 BP O2653 EP O2653 AR 62653O DI 10.1117/12.672386 PN 1-2 PG 11 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX66 UT WOS:000240025400111 ER PT S AU Feinberg, LD Hagopian, JG Diaz, C AF Feinberg, Lee D. Hagopian, John. G. Diaz, Charles BE Mather, JC MacEwen, HA DeGraauw, MWM TI New approach to cryogenic optical testing the James Webb Space Telescope - art. no. 62650P SO Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation I - Optical, Infrared and Millimeter CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE James Webb Space Telescope; JWST; optics; testing AB The James Webb Space Telescope is a 6.5 meter segmented cryogenic telescope scheduled to be launched in 2013. A key development challenge has been the cost and complexity of cryogenic optical testing of the telescope and observatory. A new approach to cryogenic optical testing the telescope and observatory has been developed that eliminates the need for a complex and expensive cryogenic optical test tower and which also allows all critical test equipment to be external to the chamber and accessible during testing. This paper summarizes the motivation for this change, the conceptual design of it, and status of implementing it. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Feinberg, LD (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NR 3 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 0-8194-6330-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6265 BP P2650 EP P2650 AR 62650P DI 10.1117/12.660396 PN 1-2 PG 9 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX66 UT WOS:000240025400019 ER PT S AU Brugarolas, PB Kia, T Li, D Alexander, JW AF Brugarolas, Paul B. Kia, Tooraj Li, Diane Alexander, James W. BE Mather, JC MacEwen, HA DeGraauw, MWM TI Pointing control system for the Eclipse mission - art. no. 62653R SO Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation I - Optical, Infrared and Millimeter CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE pointing; tracking; coronagraph; Eclipse; space observatory AB This paper describes the high precision pointing control system for the Eclipse telescope. Eclipse is a mission under study at the Jet propulsion Laboratory. Eclipse is a space telescope that uses a coronagraph for high-contrast optical astronomy to study planets around nearby stars. Eclipse observations require very precise pointing, 0.01 arcseconds (3a) during the exposure periods that could be as long as 1000 seconds. This study shows a two layer pointing approach for achieving these requirements. In the first layer, the spacecraft ACS stabilizes the line-of-sight to 0.15 arcseconds (3a). In the second layer, a Fine Steering Mirror centers the star in the occulting mask to the 0.01 arcseconds (3-sigma). The knowledge needed to achieve the desired pointing accuracy is provided by a Fine Guidance Camera. In addition, structural and thermal induced jitter is minimized by design, and through the use of reaction wheel isolators and operational constraints. 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 9 TC 3 Z9 3 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6330-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6265 BP R2653 EP R2653 AR 62653R DI 10.1117/12.671068 PN 1-2 PG 12 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX66 UT WOS:000240025400113 ER PT S AU Paine, CG Bradford, CM Dragovan, MC Yorke, HW AF Paine, Christopher G. Bradford, Charles M. Dragovan, Mark C. Yorke, Harold W. BE Mather, JC MacEwen, HA DeGraauw, MWM TI A parametric design tool for Large Space Telescope Sunshields - art. no. 62652R SO Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation I - Optical, Infrared and Millimeter CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE SAFIR; large space telescope; sunshield; V-groove radiator AB We have developed a thermal-optical-mechanical model of a representative sunshield and telescope assembly, appropriate to 10-m class far-infrared large space telescopes such as SAFIR, SPECs, SPIRIT, and CMBPol. The model provides a tool for sensitivity analysis for design parameters, including material properties and structural configuration, provides performance predictions, and has been used to direct technology development for large space telescope structures and materials. The sunshield model incorporates a flight-like design support structure for the five-layer combined sunshield and V-groove radiator, including temperature-dependent thermal, mechanical, and optical properties for the structure and deployed sunshield layers. Heat lift from mechanical cryocoolers is included, in fixed-temperature or power-balance conditions, at arbitrary points on the sunshields and support structure. The model properly accounts the wavelength dependence of radiative transfer between surfaces of widely different temperature, which capacity has not been available from commercial codes for the infrared thermal band (source temperatures 300 K-15 K) until very recently. A simplified model of the zodiacal background to be experienced at the Sun-Earth L2 point is used which, with the wavelength-dependent thermal transfer, improves the fidelity of temperature and heat lift requirements predictions for the coldest sunshield layer and telescope assembly. C1 CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA. RP Paine, CG (reprint author), CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA. NR 9 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 0-8194-6330-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6265 BP R2652 EP R2652 AR 62652R DI 10.1117/12.672151 PN 1-2 PG 8 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX66 UT WOS:000240025400083 ER PT S AU Numata, K Camp, J AF Numata, Kenji Camp, Jordan BE Mather, JC MacEwen, HA DeGraauw, MWM TI Interferometric testbed for sub-nanometer stabilization of environmental motions for testing of advanced space telescopes - art. no. 62652U SO Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation I - Optical, Infrared and Millimeter CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE interferometer; metrology; mechanical stability; gravitational waves; TPF-C; JWST; LISA AB In several future space telescope missions, high long-term relative stability between optics is required for testing on the ground, as well as achieving the sensitivity goal in flight. Typically, thermal and seismic drifts on the ground are on the order of 1 mu m over few hours, orders of magnitude above the testing requirements. To suppress these environmental motions, we developed a control system that is composed of interferometric sensors and PZT-based actuator. The system provides a stable environment to allow ground testing of the mission requirements. Our results show that this kind of system can provide picometer level stability at long timescale and that it should have many applications. C1 NASA, Goddard Space Flight Ctr, Explorat Univ Div, Greenbelt, MD 20771 USA. RP Numata, K (reprint author), NASA, Goddard Space Flight Ctr, Explorat Univ Div, Code 663, Greenbelt, MD 20771 USA. NR 9 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 0-8194-6330-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6265 BP U2652 EP U2652 AR 62652U DI 10.1117/12.672347 PN 1-2 PG 9 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX66 UT WOS:000240025400086 ER PT S AU Shi, F Basinger, SA Redding, DC AF Shi, Fang Basinger, Scott A. Redding, David C. BE Mather, JC MacEwen, HA DeGraauw, MWM TI Performance of dispersed fringe sensor in the presence of segmented mirror aberrations - Modeling and simulation - art. no. 62650Y SO Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation I - Optical, Infrared and Millimeter CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE wavefront sensing and control; dispersed fringe sen sor; segmented mirrors; wavefront aberration; line-of-sight jitter; JWST AB Dispersed Fringe Sensing (DFS) is an efficient and robust method for coarse phasing of a segmented primary mirror such as the James Webb Space Telescope (JWST). In this paper, modeling and simulations are used to study the effect of segmented mirror aberrations on the DFS fringe image, its signals, and the piston detection accuracy. The simulations show that due to the pixilation spatial filter effect from DFS signal extraction the effect of wavefront error is reduced. In addition, the DFS algorithm is more robust against wavefront aberration when the multi-trace DFS approach is used. We have also studied the JWST Dispersed Hartmann Sensor (DHS) performance in presence of wavefront aberrations caused by the gravity sag and we have used the scaled gravity sag to explore the JWST DHS performance relationship with the level of the wavefront aberration. As a special case of aberration we have also included the effect from line-ofsight jitter in the JWST modeling study. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Shi, F (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 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 0-8194-6330-2 J9 P SOC PHOTO-OPT INS PY 2006 VL 6265 BP Y2650 EP Y2650 AR 62650Y DI 10.1117/12.672714 PN 1-2 PG 12 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX66 UT WOS:000240025400028 ER PT S AU Kimble, RA MacKenty, JW O'Connell, RW AF Kimble, Randy A. MacKenty, John W. O'Connell, Robert W. CA WFC3 Team BE Mather, JC MacEwen, HA DeGraauw, MWM TI Status and performance of HST/Wide Field Camera 3 SO SPACE TELESCOPES AND INSTRUMENTATION I: OPTICAL, INFRARED, AND MILLIMETER, PTS 1 AND 2 SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation I - Optical, Infrared and Millimeter CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE space instrumentation; ultraviolet; optical; infrared; Hubble Space Telescope; CCDs; infrared arrays ID HUBBLE-SPACE-TELESCOPE; FIELD AB Wide Field Camera 3 (WFC3) is a powerful UV/visible/near-infrared camera currently in development for installation into the Hubble Space Telescope. WFC3 provides two imaging channels. The UVIS channel features a 4096 x 4096 pixel CCD focal plane covering 200 to 1000 nm wavelengths with a 160 x 160 arcsec field of view. The UVIS channel provides unprecedented sensitivity and field of view in the near ultraviolet for HST. It is particularly well suited for studies of the star formation history of local galaxies and clusters, searches for Lyman alpha dropouts at moderate redshift, and searches for low surface brightness structures against the dark UV sky background. The IR channel features a 1024 x 1024 pixel HgCdTe focal plane covering 800 to 1700 nm with a 139 x 123 arcsec field of view, providing a major advance in IR survey efficiency for HST. IR channel science goals include studies of dark energy, galaxy formation at high redshift, and star formation. The instrument is being prepared for launch as part of HST Servicing Mission 4, tentatively scheduled for late 2007, contingent upon formal approval of shuttle-based servicing after successful shuttle return-to-flight. We report here on the status and performance of WFC3. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Kimble, RA (reprint author), NASA, Goddard Space Flight Ctr, Code 667, Greenbelt, MD 20771 USA. EM randy.a.kimble@nasa.gov 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 0-8194-6330-2 J9 PROC SPIE PY 2006 VL 6265 AR 62650I DI 10.1117/12.671986 PN 1-2 PG 13 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX66 UT WOS:000240025400014 ER PT S AU Levine, BM Aguayo, F Bifano, T Fregoso, SF Green, JJ Lane, BF Liu, DT Mennesson, B Rao, S Samuele, R Shao, M Schmidtlin, E Serabyn, E Stewart, J Wallace, JK AF Levine, B. Martin Aguayo, Francisco Bifano, Thomas Fregoso, S. Felipe Green, Joseph J. Lane, Benjamin F. Liu, Duncan T. Mennesson, Bertrand Rao, Shanti Samuele, Rocco Shao, Michael Schmidtlin, Edouard Serabyn, Eugene Stewart, Jason Wallace, J. Kent BE Mather, JC MacEwen, HA DeGraauw, MWM TI The visible nulling coronagraph - Architecture definition and technology development status SO SPACE TELESCOPES AND INSTRUMENTATION I: OPTICAL, INFRARED, AND MILLIMETER, PTS 1 AND 2 SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation I - Optical, Infrared and Millimeter CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE extra-solar planet detection; high contrast imaging; nulling interferometer; coronagraph; post-suppression wavefront sensing; space instrumentation ID PLANETS; LIGHT; DEEP AB We describe the advantages of a nulling coronagraph instrument behind a single aperture space telescope for detection and spectroscopy of Earth-like extrasolar planets in visible light. Our concept synthesizes a nulling interferometer by shearing the telescope pupil into multiple beams. They are recombined with a pseudo-achromatic pi-phase shift in one arm to produce a deep null on-axis, attenuating the starlight, while simultaneously transmitting the off-axis planet light. Our nulling configuration includes methods to mitigate stellar leakage, such as spatial filtering by a coherent array of single mode fibers, balancing amplitude and phase with a segmented deformable mirror, and post-starlight suppression wavefront sensing and control. With diffraction limited telescope optics and similar quality components in the optical train (lambda/20), suppression of the starlight to 10(-10) is readily achievable. We describe key features of the architecture and analysis, present the status of key experiments to demonstrate wide bandwidth null depth, and present the status of component technology development. C1 NASA, Jet Prop Lab, Pasadena, CA USA. RP Levine, BM (reprint author), NASA, Jet Prop Lab, Pasadena, CA USA. RI Bifano, Thomas/E-6412-2013 OI Bifano, Thomas/0000-0003-4952-2515 NR 24 TC 5 Z9 5 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 0-8194-6330-2 J9 PROC SPIE PY 2006 VL 6265 AR 62651A DI 10.1117/12.672736 PN 1-2 PG 13 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX66 UT WOS:000240025400037 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 Mather, JC MacEwen, HA DeGraauw, MWM TI Direct imaging of Earth-like planets from space (TPF-C) SO SPACE TELESCOPES AND INSTRUMENTATION I: OPTICAL, INFRARED, AND MILLIMETER, PTS 1 AND 2 SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation I - Optical, Infrared and Millimeter CY MAY 24-31, 2006 CL Orlando, FL SP SPIE 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-1). 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-1 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 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 0-8194-6330-2 J9 PROC SPIE PY 2006 VL 6265 AR 626502 DI 10.1117/12.676257 PN 1-2 PG 7 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX66 UT WOS:000240025400002 ER PT S AU Krimm, HA AF Krimm, Hans A. CA Swift Sci Team BE Turner, MJL Hasinger, G TI Swift: Results from the first year of the mission - art. no. 626604 SO Space Telescopes and Instrumentation II: Ultraviolet to Gamma Ray, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation II - Ultraviolet to Gamma Ray CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE gamma-ray bursts; AGN; pulsar; X-ray binaries; CdZnTe; grazing incidence optics; hard X-ray survey ID GAMMA-RAY-BURSTS; 28 FEBRUARY 1997; EMISSION; AFTERGLOW; TELESCOPE; REDSHIFT AB The Swift gamma-ray burst explorer was launched on Nov. 20, 2004 from Cape Canaveral, Florida. The first instrument onboard became fully operational less than a month later. Since that time the Burst Alert Telescope (BAT) on Swift has detected more than one hundred gamma-ray bursts (GRBs), most of which have also been observed within two minutes by the Swift narrow-field instruments: the X-Ray Telescope (XRT) and the Ultra-Violet and Optical Telescope (UVOT). Swift trigger notices are distributed worldwide within seconds of the trigger through the Gamma-ray burst Coordinates Network (GCN) and a substantial fraction of GRBs have been followed up by ground and space-based telescopes, ranging in wavelength from radio to TeV. Results have included the first rapid localization of a short GRB and further validation of the theory that short and long bursts have different origins; detailed observations of the power-law decay of burst afterglows leading to an improved understanding of the fireball and afterglow models; and detection of the most distant GRB ever found. Swift is also a sensitive X-ray observatory with capabilities to monitor galactic and extragalactic transients on a daily basis, carry out the first all-sky hard X-ray survey since HEAO-1, and study in detail the spectra of X-ray transients. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Krimm, HA (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. NR 29 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 0-8194-6331-0 J9 P SOC PHOTO-OPT INS PY 2006 VL 6266 BP 26604 EP 26604 AR 626604 DI 10.1117/12.675946 PN 1-2 PG 12 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX60 UT WOS:000240015400005 ER PT S AU Kilbourne, CA Bandler, SR Brown, AD Chervenak, JA Figueroa-Feliciano, E Finkbeiner, FM Iyomoto, N Kelley, RL Porter, FS Saab, T Sadleir, J White, J AF Kilbourne, Caroline A. Bandler, Simon R. Brown, Ari D. Chervenak, James A. Figueroa-Feliciano, Enectali Finkbeiner, Fred M. Iyomoto, Naoko Kelley, Richard L. Porter, F. Scott Saab, Tarek Sadleir, John White, Jennifer BE Turner, MJL Hasinger, G TI High-density arrays of x-ray microcalorimeters for Constellation-X - art. no. 626621 SO Space Telescopes and Instrumentation II: Ultraviolet to Gamma Ray, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation II - Ultraviolet to Gamma Ray CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE x-ray microcalorimeter; superconducting transition-edge sensor; imaging spectroscopy ID TES MICROCALORIMETERS AB We have been developing x-ray microcalorimeters for the Constellation-X mission. Devices based on superconducting transition-edge sensors (TES) have demonstrated the potential to meet the Constellation-X requirements for spectral resolution, speed, and array scale (> 1000 pixels) in a close-packed geometry. In our part of the GSFC/NIST collaboration on this technology development, we have been concentrating on the fabrication of arrays of pixels suitable for the Constellation-X reference configuration. We have fabricated 8x8 arrays with 0.25-mm pixels arranged with 92% fill factor. The pixels are based on Mo/Au TES and Bi/Cu or Au/Bi absorbers. We have achieved a resolution of 4.0 eV FWHM at 6 keV in such devices, which meets the Constellation-X resolution requirement at 6 keV. Studies of the thermal transport in our Bi/Cu absorbers have shown that, while there is room for improvement, for 0.25mm pixels the standard absorber design is adequate to avoid unacceptable line-broadening from position dependence caused by thermal diffusion. In order to improve reproducibility and to push closer to the 2-eV goal at 6 keV, however, we are refining the design of the TES and the interface to the absorber. Recent efforts to introduce a barrier layer between the Bi and the Mo/Au to avoid variable interface chemistry and thus improve the reproducibility of device characteristics have thus far yielded unsatisfactory results. However, we have developed a new set of absorber designs with contacts to the TES engineered to allow contact only in regions that do not serve as the active thermometer. We have further constrained the design so that a low-resistance absorber will not electrically short the TES. It is with such a design that we have achieved 4.0 eV resolution at 6 keV. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Kilbourne, CA (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI Bandler, Simon/A-6258-2010; Porter, Frederick/D-3501-2012; Kelley, Richard/K-4474-2012 OI Bandler, Simon/0000-0002-5112-8106; Porter, Frederick/0000-0002-6374-1119; NR 8 TC 6 Z9 6 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 0-8194-6331-0 J9 P SOC PHOTO-OPT INS PY 2006 VL 6266 BP 26621 EP 26621 AR 626621 DI 10.1117/12.672419 PN 1-2 PG 9 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX60 UT WOS:000240015400061 ER PT S AU Gubarev, M Ramsey, B Engelhaupt, D Kester, T Speegle, C AF Gubarev, Mikhail Ramsey, Brian Engelhaupt, Darell Kester, Thomas Speegle, Chet BE Turner, MJL Hasinger, G TI Technology development for high-energy x-ray optics - art. no. 62661I SO Space Telescopes and Instrumentation II: Ultraviolet to Gamma Ray, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation II - Ultraviolet to Gamma Ray CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE x-ray optics; x-ray optics metrology; electroform-nickel replication ID LONG TRACE PROFILER; SURFACES; MIRRORS AB We are developing hard-x-ray optics using an electroformed-nickel-replication process off superpolished mandrels. To date, we have fabricated over 100 shells for our HERO balloon payload with typical angular resolutions in the 13-15 arcsec range. This paper discusses the factors currently limiting this resolution and various developments geared towards the production of higher-resolution optics. C1 Univ Space Res Assoc, MSFC, NASA, Huntsville, AL 35812 USA. RP Gubarev, M (reprint author), Univ Space Res Assoc, MSFC, NASA, VP62, Huntsville, AL 35812 USA. NR 10 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 0-8194-6331-0 J9 P SOC PHOTO-OPT INS PY 2006 VL 6266 BP I2661 EP I2661 AR 62661I DI 10.1117/12.671736 PN 1-2 PG 8 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX60 UT WOS:000240015400046 ER PT S AU Zhang, WW Chan, KW Lehan, JP Petre, R AF Zhang, William W. Chan, Kai-Wing Lehan, John P. Petre, Robert BE Turner, MJL Hasinger, G TI Fabricate and assemble: An alignment and integration method for next generation X-ray telescopes - art. no. 62661M SO Space Telescopes and Instrumentation II: Ultraviolet to Gamma Ray, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation II - Ultraviolet to Gamma Ray CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE X-ray optics; lightweight optics; Constellation-X; space optics AB Future X-ray telescopes invariably require much higher angular resolutions and/or much larger effective areas than those already flown, and they will typically be designed and built with mirror segments, in contrast with the typical past X-ray telescope of complete shells. While the segmented approach has many advantages, it has one significant disadvantage: its complexity and difficulty associated with mirror segment alignment and integration. In this paper, we outline an approach, named "Fabricate and Assemble," that directly addresses this disadvantage. We will describe the necessary components, their fabrication, and their integration into a mirror assembly. The salient features of this approach include: (1) it fully realizes the optical performance potential of each mirror segment, (2) it leaves each mirror in a stress-free or minimally stressed state, resulting in a stress-free and therefore stable mirror assembly, (3) it assembles the mirror segment while it is supported so as to minimize or even eliminate the effect of gravity, and (4) it is highly amenable to being implemented as part of a sequential production line. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Zhang, WW (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 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 0-8194-6331-0 J9 P SOC PHOTO-OPT INS PY 2006 VL 6266 BP M2661 EP M2661 AR 62661M DI 10.1117/12.672155 PN 1-2 PG 6 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX60 UT WOS:000240015400049 ER PT S AU Petre, R Lehan, J O'Dell, S Owens, S Reid, PB Saha, T Stewart, J Jones, WD Zhang, W AF Petre, Robert Lehan, John O'Dell, Stephen Owens, Scott Reid, Paul B. Saha, Tirno Stewart, Jeff Jones, William D. Zhang, William BE Turner, MJL Hasinger, G TI The Constellation-X Spectroscopy X-ray Telescope: Recent technology development - art. no. 62661Q SO Space Telescopes and Instrumentation II: Ultraviolet to Gamma Ray, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation II - Ultraviolet to Gamma Ray CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE X-ray mirrors; Constellation-X AB We describe recent progress in the technology development program for the mirror system for the Constellation-X Spectroscopy X-ray Telescope (SXT). Development of this mirror represents a significant technology challenge, as it must provide a combination of large effective area (3 sq. in) and modest angular resolution (15 arc second half power diameter requirement; 5 arc second goal) with a limited mass allocation. The baseline design incorporates over 200 nested Wolter 1 mirrors. Each of these in turn is segmented in order to simplify handling of the mirrors and facilitate mass production. The X-ray reflecting surfaces are fabricated from thin, thermally formed glass sheets. Production improvements have yielded mirror segments that approach the performance requirement without the need for epoxy replication. A mounting and alignment approach incorporating piezoelectric actuators has been shown to manipulate mirror segments with the required precision without introducing significant distortion. Substantial improvements in metrology methodology have provided insights into the mirror segment forming and alignment processes. We describe the technical advances made over the past year and summarize near-term plans. C1 NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. RP Petre, R (reprint author), NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Code 662, Greenbelt, MD 20771 USA. OI O'Dell, Stephen/0000-0002-1868-8056 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 0-8194-6331-0 J9 P SOC PHOTO-OPT INS PY 2006 VL 6266 BP Q2661 EP Q2661 AR 62661Q DI 10.1117/12.671333 PN 1-2 PG 9 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX60 UT WOS:000240015400051 ER PT S AU Zhang, WW Chan, KW Content, DA Lehan, JP Petre, R Saha, TT Gubarev, M Jones, WD O'Dell, SL AF Zhang, William W. Chan, Kai-Wing Content, David A. Lehan, John P. Petre, Robert Saha, Timo T. Gubarev, Mikhail Jones, William D. O'Dell, Stephen L. BE Turner, MJL Hasinger, G TI Development of lightweight X-ray mirrors for the Constellation-X mission - art. no. 62661V SO Space Telescopes and Instrumentation II: Ultraviolet to Gamma Ray, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation II - Ultraviolet to Gamma Ray CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE X-ray optics; lightweight optics; Constellation-X; space optics AB Constellation-X is NASA's next major X-ray observatory. It requires X-ray mirrors with high throughput (3 m(2) effective area at 1 keV), moderate angular resolution (15" half power diameter), and light weight (about an order of magnitude lighter than XMM/Newton's). Over the past few years we have been developing a glass forming technology for making mirrors. This technology by construction meets from the outset two (throughput and weight) of the three requirements. Our development effort has been concentrated on improving the angular resolution. Our progress so far has shown that this technology not only can meet the angular resolution requirement of 15" HPD, but also has the potential to reach Constellation-X's goal of 5" HPD. This paper is a snapshot of our X-ray mirror development effort as of May 2006. It briefly describes the mirror fabrication process, results achieved, and important issues that are being worked on. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Zhang, WW (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. OI O'Dell, Stephen/0000-0002-1868-8056 NR 4 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 0-8194-6331-0 J9 P SOC PHOTO-OPT INS PY 2006 VL 6266 BP V2661 EP V2661 AR 62661V DI 10.1117/12.672138 PN 1-2 PG 9 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX60 UT WOS:000240015400056 ER PT S AU Owens, SM Meagher, T Hadjimichael, T Lehan, JP Content, DA Saha, T Zhang, WW Petre, R Reid, P Jones, WD O'Dell, S AF Owens, Scott M. Meagher, Thomas Hadjimichael, Theo Lehan, John P. Content, David A. Saha, Timo Zhang, William W. Petre, Rob Reid, Paul Jones, William D. O'Dell, Stephen BE Turner, MJL Hasinger, G TI Alignment and test of a Constellation-X SXT mirror segment pair - art. no. 62661W SO Space Telescopes and Instrumentation II: Ultraviolet to Gamma Ray, Pts 1 and 2 SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation II - Ultraviolet to Gamma Ray CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE x-ray optics; x-ray telescope; optical alignment ID IMPLEMENTATION AB A single Constellation-X Spectroscopy X-ray Telescope (SXT) mirror segment pair is being aligned in the Optical Aliginnent Pathfinder 2 (OAP2) platform using a combination of mechanical and optical techniques. Coarse positioning was provided through a contact probe, the alignment was refined in a collimated while-light facility used for the Suzaku (ASTRO-E2) satellite, and then finalized with a combination of a Centroid Detector Assembly (CDA) and an interferometer coupled to a novel conical null lens providing surface map imaging over 60% of the mirror surface at one time. Due to a variety of reasons, the positioning and figure of the mirror segment under examination can shift, and we test how reliably high quality alignment can be reproduced on any given day. Also, the mirror segment's deformation response to deliberate misalignments has been tested, providing a response matrix for these thin glass mirror segments. C1 NASA, Goddard Space Flight Ctr, Washington, DC USA. RP Owens, SM (reprint author), NASA, Goddard Space Flight Ctr, Washington, DC USA. OI O'Dell, Stephen/0000-0002-1868-8056 NR 3 TC 0 Z9 0 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6331-0 J9 P SOC PHOTO-OPT INS PY 2006 VL 6266 BP W2661 EP W2661 AR 62661W DI 10.1117/12.672663 PN 1-2 PG 10 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX60 UT WOS:000240015400057 ER PT S AU Cottam, J Cash, W Flanagan, KA Heilmann, RK Prigozhin, GY Rasmussen, AP Ricker, GR Schattenburg, ML Schindhelm, E AF Cottam, Jean Cash, Webster Flanagan, Kathryn A. Heilmann, Ralf K. Prigozhin, Gregory Y. Rasmussen, Andrew P. Ricker, George R. Schattenburg, Mark L. Schindhelm, Eric BE Turner, MJL Hasinger, G TI ,The Constellation-X reflection grating spectrometer SO SPACE TELESCOPES AND INSTRUMENTATION II: ULTRAVIOLET TO GAMMA RAY, PTS 1 AND 2 SE Proceedings of SPIE-The International Society for Optical Engineering LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation II - Ultraviolet to Gamma Ray CY MAY 24-31, 2006 CL Orlando, FL SP SPIE DE X-ray; spectrometer; grating; CCD; Constellation-X ID OFF-PLANE GRATINGS; NANOIMPRINT LITHOGRAPHY; DIFFRACTION GRATINGS; RAY; FABRICATION; METROLOGY AB The Constellation-X Reflection Grating Spectrometer (RGS) is designed to provide high-throughput, high-resolution spectra in the long wavelength band of 6 to 50 angstrom. in the nominal design an array of reflection gratings is mounted at the exit of the Spectroscopy X-ray Telescope (SXT) mirror module. The gratings intercept and disperse light to a designated array of CCD detectors. To achieve the throughput (A(eff) > 1000 cm(2) below 0.6 keV) and resolution (Delta lambda/lambda > 300 below 0.6 keV) requirements for the instrument we are investigating two possible grating designs. The first design uses inplane gratings in a classical configuration that is very similar to the XMM-Newton RGS. The second design uses off-plane gratings in a conical configuration. The off-plane design has the advantage of providing higher reflectivity and potentially, a higher spectral resolution than the in-plane configuration. In our presentation we will describe the performance requirements and the current status of the technology development. C1 NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. RP Cottam, J (reprint author), NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 USA. RI Heilmann, Ralf/D-4680-2009 NR 20 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 0-8194-6331-0 J9 P SOC PHOTO-OPT INS PY 2006 VL 6266 AR 62661X DI 10.1117/12.672227 PN 1-2 PG 8 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX60 UT WOS:000240015400058 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 Turner, MJL Hasinger, G TI Direct imaging of Earth-like planets from space (TPF-C) SO SPACE TELESCOPES AND INSTRUMENTATION II: ULTRAVIOLET TO GAMMA RAY, PTS 1 AND 2 SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Space Telescopes and Instrumentation II - Ultraviolet to Gamma Ray CY MAY 24-31, 2006 CL Orlando, FL SP SPIE 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 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 0-8194-6331-0 J9 PROC SPIE PY 2006 VL 6266 AR 626502 DI 10.1117/12.676257 PN 1-2 PG 7 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation; Optics SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation; Optics GA BEX60 UT WOS:000240015400002 ER PT S AU Mushotzky, R AF Mushotzky, Richard BE Ghosh, P VandenHeuvel, EPJ TI Ultra-luminous sources in nearby galaxies SO Spectra and Timing of Compact X-Ray Binaries SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Proceedings Paper CT Colloquium on Spectra and Timing of Compact X-ray Binaries CY JAN 17-21, 2005 CL Tata Inst Fundamental Res, Bombay, INDIA SP COSPAR, Indian Space Res Org, CSIR, Govt India, Dept Sci & Technol HO Tata Inst Fundamental Res DE astrophysics; ultra-luminous sources; galactic X-ray sources ID X-RAY SOURCE; MASS BLACK-HOLES; OPTICAL COUNTERPART; HOLMBERG-II; IC-342; X-1; POPULATION; DISCOVERY; EMISSION; NGC-4559 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 on 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 II 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 - 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 Mushotzky, R (reprint author), NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. NR 40 TC 6 Z9 6 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 12 BP 2793 EP 2800 DI 10.1016/j.asr.2006.08.005 PG 8 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BFW10 UT WOS:000245036600029 ER PT S AU Ebisawa, K Kawaguchi, T AF Ebisawa, Ken Kawaguchi, Toshihiro BE Ghosh, P VandenHeuvel, EPJ TI X-ray observations of black-hole accretion disks SO SPECTRA AND TIMING OF COMPACT X-RAY BINARIES SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Proceedings Paper CT Colloquium on Spectra and Timing of Compact X-ray Binaries CY JAN 17-21, 2005 CL Tata Inst Fundamental Res, Bombay, INDIA SP COSPAR, Indian Space Res Org, CSIR, Govt India, Dept Sci & Technol HO Tata Inst Fundamental Res 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, Code 662, 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 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 12 BP 2862 EP + DI 10.1016/j.asr.2006.06.016 PG 3 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BFW10 UT WOS:000245036600044 ER PT S AU Weisskopf, MC AF Weisskopf, Martin C. BE Ghosh, P VandenHeuvel, EPJ TI Observations of compact X-ray binaries with the Chandra X-ray Observatory SO SPECTRA AND TIMING OF COMPACT X-RAY BINARIES SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Proceedings Paper CT Colloquium on Spectra and Timing of Compact X-ray Binaries CY JAN 17-21, 2005 CL Tata Inst Fundamental Res, Bombay, INDIA SP COSPAR, Indian Space Res Org, CSIR, Govt India, Dept Sci & Technol HO Tata Inst Fundamental Res 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, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Weisskopf, MC (reprint author), NASA, George C Marshall Space Flight Ctr, XD 12, Huntsville, AL 35812 USA. EM martin@smoker.msfc.nasa.gov NR 12 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 12 BP 2953 EP 2958 DI 10.1016/j.asr.2006.02.071 PG 6 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BFW10 UT WOS:000245036600064 ER PT S AU Swank, JH AF Swank, J. H. BE Ghosh, P VandenHeuvel, EPJ TI The Rossi X-ray timing explorer: Capabilities, achievements and aims SO SPECTRA AND TIMING OF COMPACT X-RAY BINARIES SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Proceedings Paper CT Colloquium on Spectra and Timing of Compact X-ray Binaries CY JAN 17-21, 2005 CL Tata Inst Fundamental Res, Bombay, INDIA SP COSPAR, Indian Space Res Org, CSIR, Govt India, Dept Sci & Technol HO Tata Inst Fundamental Res DE Rossi X-ray timing explorer; RXTE; astrophysics; black holes; neutron stars; accreting 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 extra galactic), 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 timescale 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 NR 8 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 12 BP 2959 EP 2963 DI 10.1016/j.asr.2006.07.009 PG 5 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BFW10 UT WOS:000245036600065 ER PT S AU Ramsey, BD AF Ramsey, Brian D. BE Ghosh, P VandenHeuvel, EPJ TI The development of focusing optics for the hard-X-ray region SO SPECTRA AND TIMING OF COMPACT X-RAY BINARIES SE ADVANCES IN SPACE RESEARCH-SERIES LA English DT Proceedings Paper CT Colloquium on Spectra and Timing of Compact X-ray Binaries CY JAN 17-21, 2005 CL Tata Inst Fundamental Res, Bombay, INDIA SP COSPAR, Indian Space Res Org, CSIR, Govt India, Dept Sci & Technol HO Tata Inst Fundamental Res 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 14 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 12 BP 2985 EP 2988 DI 10.1016/j.asr.2005.10.059 PG 4 WC Engineering, Aerospace; Astronomy & Astrophysics; Geosciences, Multidisciplinary; Meteorology & Atmospheric Sciences SC Engineering; Astronomy & Astrophysics; Geology; Meteorology & Atmospheric Sciences GA BFW10 UT WOS:000245036600069 ER PT S AU Smith, MAH Brown, LR Toth, RA Devi, VM Benner, DC AF Smith, M. A. H. Brown, L. R. Toth, R. A. Devi, V. Malathy Benner, D. Chris BE Oks, E Pindzola, M TI Line mixing in water vapor and methane SO SPECTRAL LINE SHAPES SE AIP Conference Proceedings LA English DT Proceedings Paper CT 18th International Conferene on Spectral Line Shapes CY JUN 04-09, 2006 CL Auburn, AL SP US DOE, Alabama Space Grant Consortium, Auburn Univ, Coll Sci & Math DE infrared; line mixing; water vapor; methane; line broadening; line shifts ID SHIFTS; BAND AB A multispectrum fitting algorithm has been used to identify line mixing and determine mixing parameters for infrared transitions of H2O and CH4 in the 5-9 mu m region. Line mixing parameters at room temperature were determined for two pairs of transitions in the v(2) fundamental band of (H2O)-O-16, for self-broadening and for broadening by H-2, He, CO2, N-2, O-2 and air. Line mixing parameters have been determined from air-broadened CH4 spectra, recorded at temperatures between 210 K and 314 K, in selected R-branch manifolds of the v(4) band. For both H2O and CH4, the inclusion of line mixing was seen to have a greater effect on the retrieved values of the line shifts than on the retrieved values of other parameters. C1 [Smith, M. A. H.; Brown, L. R.; Toth, R. A.; Devi, V. Malathy; Benner, D. Chris] NASA, Langley Res Ctr, Sci Directorate, Mail Stop 401A, Hampton, VA 23681 USA. RP Smith, MAH (reprint author), NASA, Langley Res Ctr, Sci Directorate, Mail Stop 401A, Hampton, VA 23681 USA. EM Mary.Ann.H.Smith@nasa.qov; dicbenn@wm.edu NR 5 TC 0 Z9 0 U1 0 U2 1 PU AMER INST PHYSICS PI MELVILLE PA 2 HUNTINGTON QUADRANGLE, STE 1NO1, MELVILLE, NY 11747-4501 USA SN 0094-243X BN 978-0-7354-0370-3 J9 AIP CONF PROC PY 2006 VL 874 BP 316 EP + PG 2 WC Astronomy & Astrophysics; Physics, Fluids & Plasmas; Physics, Multidisciplinary SC Astronomy & Astrophysics; Physics GA BFT23 UT WOS:000244484700039 ER PT B AU Werner, M AF Werner, Michael BE Armus, L Reach, WT TI A short and personal history of the Spitzer Space Telescope SO Spitzer Space Telescope: New Views of the Cosmos SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Meeting on Spitzer Space Telescope - New Views of the Cosmos CY NOV 09-12, 2004 CL Pasadena, CA AB The Spitzer Space Telescope, born as the Shuttle Infrared Telescope Facility (SIRTF) and later the Space Infrared Telescope Facility (still SIRTF), was under discussion and development within NASA and the scientific community for more than 30 years prior to its launch in 2003. This brief history chronicles a few of the highlights and the lowlights of those 30 years from the authors personal perspective. A much more comprehensive history of SIRTF/Spitzer has been written by George Rieke (2006). C1 CALTECH, JPL, Pasadena, CA 91125 USA. RP Werner, M (reprint author), CALTECH, JPL, Pasadena, CA 91125 USA. NR 4 TC 2 Z9 2 U1 1 U2 1 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-583812-25-9 J9 ASTR SOC P PY 2006 VL 357 BP 7 EP 18 PG 12 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation GA BGG38 UT WOS:000246656400002 ER PT B AU Cruikshank, DP Stansberry, JA Emery, JP Van Cleve, J Fernandez, YR Werner, MW Reike, GH Trilling, DE AF Cruikshank, D. P. Stansberry, J. A. Emery, J. P. Van Cleve, J. Fernandez, Y. R. Werner, M. W. Reike, G. H. Trilling, D. E. BE Armus, L Reach, WT TI Solar system observations with Spitzer Space Telescope SO Spitzer Space Telescope: New Views of the Cosmos SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Meeting on Spitzer Space Telescope - New Views of the Cosmos CY NOV 09-12, 2004 CL Pasadena, CA ID TROJAN ASTEROIDS; CONSTRAINTS AB The programs of observations of Solar System bodies conducted in the first year of the operation of the Spitzer Space Telescope as part of the Guaranteed Observing Time allocations are described. Initial results include the determination of the albedos of a number of Kuiper Belt objects and Centaurs from observations of their flux densities at 24 and 70 mu m, and the detection of emission bands in the spectra of several distant asteroids (Trojans) around 10 and 25 mu m. The 10 Kuiper Belt objects observed to date have albedos in the range 0.08 - 0.15, significantly higher than the earlier estimated 0.04. An additional KBO [(55565) 2002 AW(197)] has an albedo of 0.17 +/- 0.03. The emission bands in the asteroid spectra are indicative of silicates, but specific minerals have not yet been identified. The Centaur/comet 29P/Schwassmann-Wachmann 1 has a nucleus surface albedo of 0.025 +/- 0.01, and its dust production rate was calculated from the properties of the coma. Several other investigations are in progress as the incoming data are processed and analyzed. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Cruikshank, DP (reprint author), NASA, Ames Res Ctr, MS 245-6, Moffett Field, CA 94035 USA. NR 15 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-583812-25-9 J9 ASTR SOC P PY 2006 VL 357 BP 23 EP 30 PG 8 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation GA BGG38 UT WOS:000246656400003 ER PT B AU Lissauer, JJ AF Lissauer, Jack J. BE Armus, L Reach, WT TI Planet formation, protoplanetary disks and debris disks SO SPITZER SPACE TELESCOPE: NEW VIEWS OF THE COSMOS SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Meeting on Spitzer Space Telescope - New Views of the Cosmos CY NOV 09-12, 2004 CL Pasadena, CA ID GIANT PLANETS; GRAVITATIONAL-INSTABILITY; SOLAR NEBULA; ACCRETION; SYSTEMS; GAS; MIGRATION; MASS; FRAGMENTATION; METALLICITY AB Models of planetary growth are based upon data from our own Solar System as well as observations of extrasolar planets and the circumstellar environments of young stars. Collapse of molecular cloud cores leads to central condensations (protostars) surrounded by higher specific angular momentum circumstellar disks. Planets form within such disks, and play a major role in disk evolution. Terrestrial planets grow via pairwise accretion of solid bodies. Giant planets begin their growth as do terrestrial planets, but they become massive enough to accumulate substantial amounts of gas before the protoplanetary disk dissipates. A potential hazard to planetary systems is radial decay of planetary orbits resulting from interactions between the planets and the disk. Massive planets can sweep up disk material in their vicinity, eject planetesimals and small planets to interstellar space or into their star, and confine disks in radius and azimuth. Small planetary bodies (asteroids and comets) can sequester solid grains for long periods of time and subsequently release them. Spitzer observations of disks around stars of various ages are providing quantitative constraints on the evolution of dust within protoplanetary disks. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Lissauer, JJ (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. NR 53 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-583812-25-9 J9 ASTR SOC P PY 2006 VL 357 BP 31 EP 38 PG 8 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation GA BGG38 UT WOS:000246656400004 ER PT B AU Hollenbach, D Gorti, U AF Hollenbach, David Gorti, Uma BE Armus, L Reach, WT TI Studying gas in young and debris disks using Spitzer SO SPITZER SPACE TELESCOPE: NEW VIEWS OF THE COSMOS SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Meeting on Spitzer Space Telescope - New Views of the Cosmos CY NOV 09-12, 2004 CL Pasadena, CA ID TERRESTRIAL PLANETS; TEMPERATURE; STARS; MODEL AB We present results from models that self-consistently calculate the gas chemistry, gas temperature, dust temperature, and vertical density distribution in circumstellar disks around young stars, and that predict the emergent infrared spectra. A parameter study of optically thin disks shows that fine structure lines such as [SI] 25 mu m are generally stronger than the H-2 rotational lines. Spitzer can detect lines from disks less than or similar to 100 pc with gas masses of greater than or similar to 0.01M(J) and some dust present (greater than or similar to 10(-7) M-J) to heat the gas. We model Spitzer upper limits on line fluxes from HD 105, a 30 Myr old GOV star, and provide upper limits on the gas surface density and mass (less than or similar to 1M(J)) in the planet-forming region (1-40 AU). Preliminary results for younger, optically thick disks are briefly discussed. C1 [Hollenbach, David] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. [Gorti, Uma] Univ Calif Berkeley, Berkeley, CA 94720 USA. RP Hollenbach, D (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. FU FEPS Legacy Project FX We acknowledge support through the Spitzer Legacy Program which has funded the FEPS Legacy Project. NR 11 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-583812-25-9 J9 ASTR SOC P PY 2006 VL 357 BP 47 EP + PG 2 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation GA BGG38 UT WOS:000246656400006 ER PT B AU Cushing, MC Roellig, TL AF Cushing, Michael C. Roellig, Thomas L. BE Armus, L Reach, WT TI Spitzer Space Telescope observations of M, L, and T dwarfs SO SPITZER SPACE TELESCOPE: NEW VIEWS OF THE COSMOS SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Meeting on Spitzer Space Telescope - New Views of the Cosmos CY NOV 09-12, 2004 CL Pasadena, CA ID BROWN DWARF AB We present the first mid-infrared spectra of very low-mass stars and brown dwarfs obtained with the Infrared Spectrograph onboard the Spitzer Space Telescope. We observed GJ 1001 A (M3.5 V), DENIS 0255-4700 (L8), and epsilon Ind Ba/Bb (T1/T6). As expected from the predictions of model atmospheres, the spectra show absorption features of H2O, CH4 at 7.8 mu m, and NH3 at 10.5 mu m. This is the first detection of the 7.8 mu m CH4 band in the spectrum of a brown dwarf and the first detection of NH3 in the atmosphere of a brown dwarf. C1 [Cushing, Michael C.] Univ Arizona, Steward Observ, 933 N Cherry Rd, Tucson, AZ 85721 USA. [Roellig, Thomas L.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Cushing, MC (reprint author), Univ Arizona, Steward Observ, 933 N Cherry Rd, Tucson, AZ 85721 USA. NR 7 TC 0 Z9 0 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-583812-25-9 J9 ASTR SOC P PY 2006 VL 357 BP 66 EP + PG 2 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation GA BGG38 UT WOS:000246656400010 ER PT B AU Peeters, E Mattioda, AL Kemper, F Hudgins, DM Allamandola, LJ AF Peeters, E. Mattioda, A. L. Kemper, F. Hudgins, D. M. Allamandola, L. J. BE Armus, L Reach, WT TI The 15-21 mu m PAH plateau SO SPITZER SPACE TELESCOPE: NEW VIEWS OF THE COSMOS SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Meeting on Spitzer Space Telescope - New Views of the Cosmos CY NOV 09-12, 2004 CL Pasadena, CA ID EMISSION AB We present 14-21 mu m emission spectra of star forming regions and compare them with the PAH spectra from the Ames PAH database. We show that while the emission in this region can be quite variable, the bulk of these variations can be accommodated by variations in the IS PAH population. C1 [Peeters, E.; Mattioda, A. L.; Hudgins, D. M.; Allamandola, L. J.] NASA, Ames Res Ctr, MS245-6,Moffett Field, Moffett Field, CA 94035 USA. [Kemper, F.] Univ Virginia, Charlottesville, VA 22903 USA. RP Peeters, E (reprint author), NASA, Ames Res Ctr, MS245-6,Moffett Field, Moffett Field, CA 94035 USA. RI Kemper, Francisca/D-8688-2011 OI Kemper, Francisca/0000-0003-2743-8240 FU NASA's; National Research Council FX This work was supported by NASAs Long Term Space Astrophysics Program, the Spitzer Fellowship Program and the National Research Council. NR 7 TC 4 Z9 4 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-583812-25-9 J9 ASTR SOC P PY 2006 VL 357 BP 95 EP + PG 2 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation GA BGG38 UT WOS:000246656400018 ER PT B AU Cami, J Blommaert, J AF Cami, Jan Blommaert, Joris BE Armus, L Reach, WT TI The dust sequence along the AGB SO Spitzer Space Telescope: New Views of the Cosmos SE ASTRONOMICAL SOCIETY OF THE PACIFIC CONFERENCE SERIES LA English DT Proceedings Paper CT Meeting on Spitzer Space Telescope - New Views of the Cosmos CY NOV 09-12, 2004 CL Pasadena, CA ID ISOGAL; BULGE AB We present a preview of a Spitzer-IRS program aimed to study the formation and evolution of dust in the outflows of oxygen-rich stars as they climb the Asymptotic Giant Branch (AGB). Previous studies were generally biased to bright, nearby stars which provided studies limited to a biased and inhomogeneous sample of stars. The unique sensitivity of Spitzer-IRS now allows to carefully select a homogeneous sample of stars along the AGB at the same distance and with comparable progenitor masses, thereby greatly limiting the remaining parameters of importance for the process of dust formation. We present here how this program will help to understand mass loss evolution and dust formation mechanisms around evolved stars. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Cami, J (reprint author), NASA, Ames Res Ctr, Mail Stop 245-6, Moffett Field, CA 94035 USA. 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 978-1-583812-25-9 J9 ASTR SOC P PY 2006 VL 357 BP 146 EP 149 PG 4 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation GA BGG38 UT WOS:000246656400031 ER PT B AU Polomski, E Gehrz, RD Woodward, CE Humphreys, RM Boyer, M Brandl, B van Loon, J Fazio, G Willner, SP Barmby, P Ashby, M Pahre, M Rieke, G Gordon, K Hinz, J Engelbracht, C Alonso-Herrero, A Misselt, K Perez-Gonzalez, PG Roellig, T AF Polomski, E. Gehrz, R. D. Woodward, C. E. Humphreys, R. M. Boyer, M. Brandl, B. van Loon, J. Fazio, G. Willner, S. P. Barmby, P. Ashby, M. Pahre, M. Rieke, G. Gordon, K. Hinz, J. Engelbracht, C. Alonso-Herrero, A. Misselt, K. Perez-Gonzalez, P. G. Roellig, T. BE Armus, L Reach, WT TI Multi-epoch imaging and spectroscopy of M33 SO SPITZER SPACE TELESCOPE: NEW VIEWS OF THE COSMOS SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Meeting on Spitzer Space Telescope - New Views of the Cosmos CY NOV 09-12, 2004 CL Pasadena, CA AB We have initiated a multi-epoch Spitzer observing campaign of the galaxy M33. The observing program involves mapping the galaxy multiple times over a period of 2.5 years using the IRAC (3-8 mu m) and MIPS (24-160 mu m) cameras and conducting followup IRS spectroscopy of specific sources. The current data set includes IRAC maps from 2003 December, 2004 July, August, and 2005 January, and MIPS maps from 2004 January and 2005 January. These images reveal the entire range of phenomena involved in the creation, evolution, and destruction of dust in star formation regions, evolved stars, and SNR. C1 [Polomski, E.; Gehrz, R. D.; Woodward, C. E.; Humphreys, R. M.; Boyer, M.] Univ Minnesota, Dept Astron, 116 Church St SE, Minneapolis, MN 55455 USA. [Brandl, B.] Leiden Observ, NL-2300 RA Leiden, Netherlands. [van Loon, J.] Keele Univ, Sch Chem & Phys, Keele ST5 5BG, Staffs, England. [Fazio, G.; Willner, S. P.; Barmby, P.; Ashby, M.; Pahre, M.] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. [Rieke, G.; Gordon, K.; Hinz, J.; Engelbracht, C.; Alonso-Herrero, A.; Misselt, K.; Perez-Gonzalez, P. G.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Roellig, T.] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Polomski, E (reprint author), Univ Minnesota, Dept Astron, 116 Church St SE, Minneapolis, MN 55455 USA. RI Barmby, Pauline/I-7194-2016; Alonso-Herrero, Almudena/H-1426-2015 OI Barmby, Pauline/0000-0003-2767-0090; Alonso-Herrero, Almudena/0000-0001-6794-2519 NR 3 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-583812-25-9 J9 ASTR SOC P PY 2006 VL 357 BP 196 EP + PG 2 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation GA BGG38 UT WOS:000246656400046 ER PT B AU Gorjian, V Werner, MW Lawrence, CR AF Gorjian, V. Werner, M. W. Lawrence, C. R. BE Armus, L Reach, WT TI MIPS and IRS analysis of nearby X-ray selected Seyfert galaxies SO SPITZER SPACE TELESCOPE: NEW VIEWS OF THE COSMOS SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Meeting on Spitzer Space Telescope - New Views of the Cosmos CY NOV 09-12, 2004 CL Pasadena, CA ID SPITZER-SPACE-TELESCOPE AB We have obtained MIPS 24 and 70 micron photometry as well as IRS 5 to 38 micron spectra (low and high resolution) of 30 nearby Seyfert Active Galactic Nuclei (AGN). The AGNs were chosen to have a broad range of X-ray determined Hydrogen column densities from Compton thin to Compton thick sources. We will discuss the continuum and emission line properties of the sample, and their relationship to the X-ray properties. C1 [Gorjian, V.; Werner, M. W.; Lawrence, C. R.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RP Gorjian, V (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 ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-583812-25-9 J9 ASTR SOC P PY 2006 VL 357 BP 200 EP + PG 2 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation GA BGG38 UT WOS:000246656400048 ER PT B AU Engelbracht, CW Gordon, KD Misselt, KA Smith, JDT Perez-Gonzalez, PG Rieke, GH Werner, MW Vanzi, L Brandl, BR AF Engelbracht, C. W. Gordon, K. D. Misselt, K. A. Smith, J. D. T. Perez-Gonzalez, P. G. Rieke, G. H. Werner, M. W. Vanzi, L. Brandl, B. R. BE Armus, L Reach, WT TI Infrared properties of low-metallicity galaxies SO SPITZER SPACE TELESCOPE: NEW VIEWS OF THE COSMOS SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Meeting on Spitzer Space Telescope - New Views of the Cosmos CY NOV 09-12, 2004 CL Pasadena, CA AB We present new Spitzer photometry of three low-metallicity galaxies. These galaxies have metallicities more than 30 times lower than the solar value and include the two galaxies with the lowest known metallicities, I Zw 18 and SBS 0335-52. Our TRAC and MIPS data represent the first mid- to far-infrared detections for most of these galaxies and allow us for the first time to explore the range of infrared properties of extremely low metallicity galaxies as a class. We derive dust temperatures, dust masses, and optical/infrared luminosities of the galaxies. To put our sample of low-metallicity galaxies into context, we use infrared colors and spectra of galaxies over the full range of metallicities observed in local galaxies to show that there is a transition metallicity below which PAHs are not observed in galaxies. C1 [Engelbracht, C. W.; Gordon, K. D.; Misselt, K. A.; Smith, J. D. T.; Perez-Gonzalez, P. G.; Rieke, G. H.] Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. [Werner, M. W.] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. [Vanzi, L.] European Southern Observ Alonso de Cordova, Santiago, Chile. [Brandl, B. R.] Leiden Univ, NL-2300 RA Leiden, Netherlands. RP Engelbracht, CW (reprint author), Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RI Vanzi, Leonardo/D-1381-2014 FU NASA [960785] FX This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under NASA contract 1407. Support for this work was provided by NASA through Contract Number 960785 issued by JPL/Caltech. NR 0 TC 1 Z9 1 U1 0 U2 0 PU ASTRONOMICAL SOC PACIFIC PI SAN FRANCISCO PA 390 ASHTON AVE, SAN FRANCISCO, CA 94112 USA BN 978-1-583812-25-9 J9 ASTR SOC P PY 2006 VL 357 BP 215 EP + PG 2 WC Engineering, Aerospace; Astronomy & Astrophysics; Instruments & Instrumentation SC Engineering; Astronomy & Astrophysics; Instruments & Instrumentation GA BGG38 UT WOS:000246656400053 ER PT S AU Malekpour, MR AF Malekpour, Mahyar R. BE Datta, AK Gradinariu, M TI A Byzantine-fault tolerant self-stabilizing protocol for distributed clock synchronization systems SO Stabilization, Safety, and Security of Distributed Systems, Proceedings SE LECTURE NOTES IN COMPUTER SCIENCE LA English DT Proceedings Paper CT 8th International Symposium on Stabilization, Safety and Security of Distributed Systems (SSS 2006) CY NOV 17-19, 2006 CL Dallas, TX DE Byzantine; fault tolerant; self-stabilization; clock synchronization; distributed; protocol; algorithm; model checking; verification AB Embedded distributed systems have become an integral part of safety-critical computing applications, necessitating system designs that incorporate fault tolerant clock synchronization in order to achieve ultra-reliable assurance levels. Many efficient clock synchronization protocols do not, however, address Byzantine failures, and most protocols that do tolerate Byzantine failures do not self-stabilize. Of the Byzantine self-stabilizing clock synchronization algorithms that exist in the literature, they are based on either unjustifiably strong assumptions about initial synchrony of the nodes or on the existence of a common pulse at the nodes. The Byzantine self-stabilizing clock synchronization protocol presented here does not rely on any assumptions about the initial state of the clocks. Furthermore, there is neither a central clock nor an externally generated pulse system. The proposed protocol converges deterministically, is scalable, and self-stabilizes in a short amount of time. The convergence time is linear with respect to the self-stabilization period. Proofs of the correctness of the protocol as well as the results of formal verification efforts are reported. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Malekpour, MR (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. NR 14 TC 8 Z9 8 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0302-9743 BN 3-540-49018-3 J9 LECT NOTES COMPUT SC PY 2006 VL 4280 BP 411 EP 427 PG 17 WC Computer Science, Theory & Methods; Telecommunications SC Computer Science; Telecommunications GA BFM97 UT WOS:000243130600029 ER PT B AU Miroshnichenko, AS Bernabei, S Jorkman, KS Chentsov, EL Klochkova, VG Gray, RO Levato, H Grosso, M Hinkle, KH Kuratov, KS Kusakin, AV Garcia-Lario, P Calderon, JVP Polcaro, VF Viotti, RF Norci, L Manset, N Men'shchikov, AB Rudy, RJ Lynch, DK Venturini, CC Mazuk, S Puetter, RC Perry, RB Gandet, TL AF Miroshnichenko, A. S. Bernabei, S. Jorkman, K. S. Chentsov, E. L. Klochkova, V. G. Gray, R. O. Levato, H. Grosso, M. Hinkle, K. H. Kuratov, K. S. Kusakin, A. V. Garcia-Lario, P. Perea Calderon, J. V. Polcaro, V. F. Viotti, R. F. Norci, L. Manset, N. Men'shchikov, A. B. Rudy, R. J. Lynch, D. K. Venturini, C. C. Mazuk, S. Puetter, R. C. Perry, R. B. Gandet, T. L. BE Kraus, M Miroshnnichenko, AS TI B[e] stars with warm dust: Revealing the nature of unclassified B[e] stars and expanding the family SO STARS WITH THE B[E] PHENOMENON, PROCEEDINGS SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Meeting on Stars with the B (e) Phenomenon CY JUL 10-16, 2005 CL Isl Vlieland, NETHERLANDS ID EMISSION-LINE STARS; BINARY-SYSTEM; PHOTOMETRIC BEHAVIOR; B STAR; SUPERGIANTS; EVOLUTION; HD-45677; SPECTROPHOTOMETRY; SPECTROSCOPY; EXCESSES AB Until recently, unclassified B[e] stars represented half of the entire B[e] group. Our study of these objects with strong emission-line spectra and IRAS fluxes, decreasing toward longer wavelengths, resulted in a suggestion that they currently form dust in their envelopes. The objects have been tentatively called B[e] stars with warm dust (B[e]WD). Their luminosity range (similar to 3 orders of magnitude) is much larger compared to previous suggestions that dust formation occurs only near very luminous hot stars. A significant fraction of B[e]WD are recognized or suspected binaries. The group has been expanded with both previously detected hot emission-line stars with IR fluxes, typical for confirmed B[e]WD, and new candidates, found in recent all-sky surveys. Currently the number of B[e]WD members and candidates is similar to 60 with an opportunity to find more in existing stellar catalogs. Main observational and physical properties of B[e]WD and their envelopes are summarized. Our results on newly found group members are presented. C1 [Miroshnichenko, A. S.] Univ N Carolina, Dept Phys & Astron, POB 26170, Greensboro, NC 27402 USA. [Bernabei, S.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Jorkman, K. S.] Univ Toledo, Ritter Observ, Toledo, OH 43606 USA. [Chentsov, E. L.; Klochkova, V. G.] Russian Acad Sci, Special Astrophys Observ, Nizhnii Arkhyz R-369167, Russia. [Gray, R. O.] Appalachian State Univ, Dept Phys & Astron, Boone, NC 28608 USA. [Levato, H.; Grosso, M.] Complejo Astron Leoncito, San Juan RA-5400, Argentina. [Hinkle, K. H.] Natl Opt Astron Observ, Tucson, AZ 85726 USA. [Kuratov, K. S.] Fesenkov Astrophy Inst, Alma Ata 480068, Kazakhstan. [Kusakin, A. V.] Sternberg Astron Inst, Moscow, Russia. [Garcia-Lario, P.; Perea Calderon, J. V.] European Space Astron Ctr, E-28080 Madrid, Spain. [Polcaro, V. F.; Viotti, R. F.] Inst Astrofis Spaziale Fis Cosm, I-00133 Rome, Italy. [Norci, L.] Dublin City Univ, Sch Phys Sci, Dublin, Ireland. [Manset, N.] Canada France Hawaii Telescope Corp, Kamuela, HI 96743 USA. [Men'shchikov, A. B.] St Marys Univ, Inst Computat Astrophy, Halifax, NS B3H 3C3, Canada. [Rudy, R. J.; Lynch, D. K.; Venturini, C. C.; Mazuk, S.] Aerosp Corp, Los Angeles, CA 92957 USA. [Perry, R. B.] NASA, Langley Res Ctr, Hampton, VA 23681 USA. [Gandet, T. L.] Lizard Hollow Observ, Tucson, AZ 85752 USA. RP Miroshnichenko, AS (reprint author), Univ N Carolina, Dept Phys & Astron, POB 26170, Greensboro, NC 27402 USA. NR 43 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 978-1-58381-223-5 J9 ASTR SOC P PY 2006 VL 355 BP 315 EP + PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BFU88 UT WOS:000244732000040 ER PT B AU Miroshnichenko, AS Bernabei, S Polcaro, VF Viotti, RF Norci, L Manset, N Klochkova, VG Rudy, RJ Lynch, DK Venturini, CC Mazuk, S Puetter, RC Perry, RB Gandet, TL AF Miroshnichenko, A. S. Bernabei, S. Polcaro, V. F. Viotti, R. F. Norci, L. Manset, N. Klochkova, V. G. Rudy, R. J. Lynch, D. K. Venturini, C. C. Mazuk, S. Puetter, R. C. Perry, R. B. Gandet, T. L. BE Kraus, M Miroshnnichenko, AS TI Optical and near-IR observations of the B[e] star AS 119 SO STARS WITH THE B[E] PHENOMENON, PROCEEDINGS SE Astronomical Society of the Pacific Conference Series LA English DT Proceedings Paper CT Meeting on Stars with the B (e) Phenomenon CY JUL 10-16, 2005 CL Isl Vlieland, NETHERLANDS AB AS 119 is a poorly-studied emission-line object with a large IR excess (Dong & Hu 1991). Optical spectrophotometry by Cidale et al. (2001) suggests that it is a B3 IVe star, while its strong Balmer lines and IR spectral energy distribution (SED) allow us to classify AS 119 as a B[e] star with warm dust (B[e]WD). We present the first high-resolution optical and low-resolution near-IR spectroscopy and multicolor optical photometry of the object. The optical spectrum is dominated by emission [Fe II] lines, which are stronger than Fe II lines and whose radial velocities (RV) are different from those of the photospheric lines. Such a behavior may be due to the object's binary nature, but no traces of the secondary have been found in our spectra. C1 [Miroshnichenko, A. S.] Univ N Carolina, Dept Phys & Astron, POB 26170, Greensboro, NC 27402 USA. [Bernabei, S.] Osservatorio Astron Bologna, INAF, I-40127 Bologna, Italy. [Polcaro, V. F.; Viotti, R. F.] Inst Astrofis Spaziale & Fisica Cosmica, INAF, I-00133 Rome, Italy. [Norci, L.] Dublin City Univ, Sch Phys Sci, Dublin, Ireland. [Manset, N.] CFHT Corp, Kamuela, HI 96743 USA. [Klochkova, V. G.] Russian Acad Sci, Special Astrophys Observ, Nizhnii Arkhyz, Russia. [Rudy, R. J.; Lynch, D. K.; Venturini, C. C.; Mazuk, S.] Aerosp Corp, Los Angeles, CA 90009 USA. [Puetter, R. C.] Univ Calif San Diego, La Jolla, CA 92093 USA. [Perry, R. B.] NASA, Langley Res Ctr, Sci Support Off, Hampton, VA 23681 USA. [Gandet, T. L.] Lizard Hollow Observ, Tucson, AZ 85752 USA. RP Miroshnichenko, AS (reprint author), Univ N Carolina, Dept Phys & Astron, POB 26170, Greensboro, NC 27402 USA. FU NASA [NAG58054]; The Aerospace Corporation FX A. M. and K. B. were supported by NASA grant NAG58054. D. L., S. M., C. V., and R. R. were supported by the Independent Research and Development program at The Aerospace Corporation. NR 11 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 978-1-58381-223-5 J9 ASTR SOC P PY 2006 VL 355 BP 347 EP + PG 3 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BFU88 UT WOS:000244732000044 ER PT B AU Smith, M AF Smith, Michele GP STC TI When "YES" does not mean "Yes" SO STC's 53rd Annual Conference Proceedings 2005 LA English DT Proceedings Paper CT Annual Meeting of the Society-for-Technical-Communication CY MAY 07-10, 2006 CL Las Vegas, NV SP Soc Tech Commun AB One of today's most ambitious projects is the International Space Station which combines the expertise and resources of 16 nations. This paper will discuss the challenges of multi-national teams, as well as how communication which is unclear, or simply misunderstood, can impact budget, schedule and stress levels. Examples will be based on the International Space Station Program. Hopefully these examples will spur thought and appreciation for what the diversity of cultures can bring to a project. It will also offer concepts and tools to help avoid some of the challenges and some tools for avoiding some of the difficulties. C1 NASA, Kennedy Space Ctr, Cape Canaveral, FL USA. NR 1 TC 0 Z9 0 U1 0 U2 0 PU SOC TECHNICAL COMMUNICATION PI ARLINGTON PA 901 N STUART ST, SUITE 904, ARLINGTON, VA 22203-1854 USA BN 1-891709-21-6 PY 2006 BP 82 EP 87 PG 6 WC Communication SC Communication GA BEP98 UT WOS:000238839500017 ER PT J AU Levine, M Fanson, J AF Levine, M Fanson, J TI Advanced thermo-structural technologies for the NASA terrestrial planet finder mission SO STRUCTURAL CONTROL & HEALTH MONITORING LA English DT Article DE telescope; integrated modelling; mechanical systems AB The primary objective of the NASA Terrestrial Planet Finder flight missions will be to detect and characterize Earth-like planets around nearby stars. Because of the complexity of the design concepts, the project will rely heavily on the use of analytical simulations to predict on-orbit performance. Furthermore, current understanding of these missions indicates that the 3-8 m class optical systems need to be as stable as picometres in wavefront and sub-milli arcsec in pointing. These extremely small requirements impose on the models a level of predictive accuracy heretofore never achieved, especially in the area of microgravity effects, material property accuracy, thermal solution convergence, microdynamic stability and all other second-order modelling effects typically ignored. New modelling tools and analysis paradigms are developed which emphasize computational accuracy and fully integrated analytical simulations. The process is demonstrated on sample problems using a TPF Coronagraph design concept. The TPF project is also planning a suite of testbeds through which various aspects of the models and simulations will be verified. Copyright (c) 2005 John Wiley & Sons, Ltd. C1 CALTECH, Jet Prop Lab, Adv Opt Syst Grp, Pasadena, CA 91109 USA. RP Levine, M (reprint author), CALTECH, Jet Prop Lab, Adv Opt Syst Grp, 4800 Oak Grove Dr,MS 157-316, Pasadena, CA 91109 USA. EM Marie.B.Levine@jpl.nasa.gov NR 10 TC 1 Z9 1 U1 0 U2 1 PU JOHN WILEY & SONS LTD PI CHICHESTER PA THE ATRIUM, SOUTHERN GATE, CHICHESTER PO19 8SQ, W SUSSEX, ENGLAND SN 1545-2255 J9 STRUCT CONTROL HLTH JI Struct. Control. Health Monit. PD JAN-FEB PY 2006 VL 13 IS 1 BP 190 EP 209 DI 10.1002/stc.136 PG 20 WC Construction & Building Technology; Engineering, Civil; Instruments & Instrumentation SC Construction & Building Technology; Engineering; Instruments & Instrumentation GA 015YN UT WOS:000235587600012 ER PT J AU Kremic, T Tukel, OI Rom, WO AF Kremic, Tibor Tukel, Oya Icmeli Rom, Walter O. TI Outsourcing decision support: a survey of benefits, risks, and decision factors SO SUPPLY CHAIN MANAGEMENT-AN INTERNATIONAL JOURNAL LA English DT Review DE outsourcing; publications; multivariate analysis; decision support systems ID TRANSACTION COST APPROACH; KNOWLEDGE MANAGEMENT; INFORMATION-SYSTEMS; MANAGING KNOWLEDGE; STRATEGY; COMPETENCES; DYNAMICS; TECHNOLOGY; SERVICES; CAPABILITIES AB Purpose - The purpose of this study is twofold. The first is to provide a structured review of the vast amount of outsourcing literature that has accumulated in the past two decades using a decision support framework. The second purpose is to statistically analyze the contents of the studies to identify commonalities as well as gaps, in order to suggest directions for future research. Design/methodology/approach - The contents of more than 200 publications are analyzed using a variety of approaches. A decision support framework is used to first classify whether the studies address outsourcing benefits, risks, motivations or factors. Next, each classification is further described by the type of benefits, risks, etc. Additional relevant contents such as type of organization, and the location of the outsourcing practice are also considered. Multivariate analyses consisting of cross tabulations, chi-square testing and cluster analysis are used for categorizing the studies with the aim of identifying relationships among the studies which are not apparent when they are considered individually. Findings - A number of trends and relationships are identified. For example, most studies focus on US for-profit organizations and are typically theoretical, discussing benefits, risks and motivators. On the other hand, the research on outsourcing practices of non-profit organizations, where objectives for outsourcing are typically politically driven, is found to be scarce. Furthermore, the results of the cluster analysis indicate that the studies can be grouped into six clusters where the five small clusters are characterized by strong relationships with a few variables while the large cluster is characterized by variables that are not addressed in the studies. Practical implications - Outsourcing has become commonplace in today's businesses. In addition to outsourcing in profit seeking organizations, there is considerable outsourcing effort in governmental and non-profit organizations also. It is not easy for managers who are exploring outsourcing opportunities for the very first time and academicians who want to build upon existing studies to search the literature to find what they are looking for. This study addresses this difficulty by providing different classifications of the literature based on a variety of research criteria. Originality/value - This study is a first attempt to organize the outsourcing literature using statistical as well as decision support tools. Using cluster analysis and discriminant analysis to explore the relationships among the contents of the studies is a new approach. C1 NASA, Glenn Res Ctr, Cleveland, OH USA. Cleveland State Univ, Coll Business Adm, Operat Management Dept, Cleveland, OH 44115 USA. RP Kremic, T (reprint author), NASA, Glenn Res Ctr, Cleveland, OH USA. EM o.icmeli@scuohio.edu NR 213 TC 92 Z9 92 U1 8 U2 55 PU EMERALD GROUP PUBLISHING LTD PI BINGLEY PA HOWARD HOUSE, WAGON LANE, BINGLEY BD16 1WA, W YORKSHIRE, ENGLAND SN 1359-8546 EI 1758-6852 J9 SUPPLY CHAIN MANAG JI Supply Chain Manag. PY 2006 VL 11 IS 6 BP 467 EP 482 DI 10.1108/13598540610703864 PG 16 WC Business; Management SC Business & Economics GA 103BG UT WOS:000241858400001 ER PT J AU Funk, S Bozzolo, G Garces, JE Burghaus, U AF Funk, S Bozzolo, G Garces, JE Burghaus, U TI Atomistic modeling of Zn deposition on the low index faces of Cu SO SURFACE SCIENCE LA English DT Article DE adatoms; computer simulations; zinc; copper; surface alloys; surface structure; semi-empirical methods and model calculations ID METHANOL SYNTHESIS; CU(111); SURFACE; CATALYSTS; ALLOYS; GROWTH AB The formation process of Zn/Cu surface alloys is investigated using the Bozzolo-Ferrante-Smith (BFS) method for alloys. The effects of the crystallographic orientation on the deposition process, formation of surface alloys as a function of temperature and coverage, Zn surface migration, and interdiffusion in the Cu substrate, are modeled and discussed with atom-by-atom energy analyses and large scale simulations. (c) 2005 Elsevier B.V. All rights reserved. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. Ohio Aerosp Inst, Cleveland, OH 44142 USA. N Dakota State Univ, Dept Chem & Mol Biol, Fargo, ND 58105 USA. Comis Nacl Energia Atom, Ctr Atom Bariloche, RA-8400 San Carlos De Bariloche, Rio Negro, Argentina. RP Bozzolo, G (reprint author), NASA, Glenn Res Ctr, Mail Stop 23-2, Cleveland, OH 44135 USA. EM Guillermo.H.Bozzolo@grc.nasa.gov NR 17 TC 8 Z9 8 U1 0 U2 6 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0039-6028 J9 SURF SCI JI Surf. Sci. PD JAN 1 PY 2006 VL 600 IS 1 BP 195 EP 204 DI 10.1016/j.susc.2005.10.015 PG 10 WC Chemistry, Physical; Physics, Condensed Matter SC Chemistry; Physics GA 007DJ UT WOS:000234948000020 ER PT B AU Tan, HZ Adelstein, BD Traylor, R Kocsis, M Hirleman, ED AF Tan, Hong Z. Adelstein, Bernard D. Traylor, Ryan Kocsis, Matthew Hirleman, E. Dan BE Hannaford, B Weisenberger, J Gillespie, B TI Discrimination of real and virtual high-definition textured surfaces SO SYMPOSIUM ON HAPTICS INTERFACES FOR VIRTUAL ENVIRONMENT AND TELEOPERATOR SYSTEMS 2006, PROCEEDINGS LA English DT Proceedings Paper CT 14th Symposium on Haptics Interfaces for Virtual Environment and Teleoperator Systems CY MAR 25-26, 2006 CL Alexandria, VA SP IEEE Comp Soc, Visualizat & Graph Tech Comm ID TACTILE ROUGHNESS; ACTIVE TOUCH; PERCEPTION; AMPLITUDE; GRATINGS; GEOMETRY; DISPLAY; OBJECTS; FORCE AB Research on haptic texture perception requires the availability of textured surfaces with high precision and fine resolution. Given the exquisite sensitivity of the human fingers to minute differences in surface details, the textured surfaces need to be precisely defined to a micron level. Real and virtual high-definition textured surfaces were used in the present study of amplitude discrimination of sinusoidal gratings. Similar thresholds were obtained despite the difference in contact modes (fingertip on real textures and a point on virtual textures). The results support the use of high position-resolution force-feedback devices in studying texture perception, especially in situations where the fabrication of real textures is either beyond the resolution of the fabrication process or simply too expensive and time-consuming. C1 [Tan, Hong Z.; Traylor, Ryan; Kocsis, Matthew] Purdue Univ, Hapt Interface Res Lab, W Lafayette, IN 47907 USA. [Adelstein, Bernard D.] NASA, Ames Res Ctr, Human Factors Div, Moffett Field, CA 94035 USA. [Hirleman, E. Dan] Purdue Univ, Sch Mech Engn, W Lafayette, IN 47907 USA. RP Tan, HZ (reprint author), Purdue Univ, Hapt Interface Res Lab, W Lafayette, IN 47907 USA. EM hongtan@purdue.edu; bda@eos.arc.nasa.gov; traylorr@purdue.edu; mkocsis@purdue.edu; hirleman@purdue.edu FU National Science Foundation [0098443-IIS]; NASA [NCC 2-1363]; NASA's Space Human Factors Engineering Program [131-20-30] FX This work was supported in part by a National Science Foundation Award under Grant No. 0098443-IIS, and in part by NASA under award no. NCC 2-1363. BDA was supported by NASAs Space Human Factors Engineering Program (131-20-30). The authors wish to thank Drs. Susan Lederman and Roberta Klatzky for discussions on experimental methods, and Mike Sherwood at Purdue University for his assistance with the fabrication of the stainless steel texture samples used in Exp. I. NR 33 TC 5 Z9 5 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 1-4244-0226-3 PY 2006 BP 3 EP 9 PG 7 WC Computer Science, Cybernetics; Computer Science, Hardware & Architecture; Engineering, Biomedical SC Computer Science; Engineering GA BEG57 UT WOS:000237225000001 ER PT J AU Linde, C AF Linde, C TI Shouldering risks: The culture of control in the nuclear power industry. SO TECHNOLOGY AND CULTURE LA English DT Book Review C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Linde, C (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. NR 1 TC 0 Z9 0 U1 0 U2 1 PU JOHNS HOPKINS UNIV PRESS PI BALTIMORE PA JOURNALS PUBLISHING DIVISION, 2715 NORTH CHARLES ST, BALTIMORE, MD 21218-4363 USA SN 0040-165X J9 TECHNOL CULT JI Technol. Cult. PD JAN PY 2006 VL 47 IS 1 BP 226 EP 227 DI 10.1353/tech.2006.0079 PG 2 WC History & Philosophy Of Science SC History & Philosophy of Science GA 030SH UT WOS:000236654200042 ER PT S AU Cramer, KE Winfree, WP Hodges, K Koshti, A Ryan, D Reinhardt, WW AF Cramer, K. Elliott Winfree, William P. Hodges, Kenneth Koshti, Ajay Ryan, Daniel Reinhardt, Walter W. BE Miles, JJ Peacock, GR Knettel, KM TI Status of thermal NDT of space shuttle materials at NASA - art. no. 62051B SO Thermosense XXVIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Thermosense XXVII CY APR 17-20, 2006 CL Kissimmee, FL SP SPIE DE thermography; reinforced carbon-carbon ID DEPTH AB Since the Space Shuttle Columbia accident, NASA has focused on improving advanced NDE techniques for the Reinforced Carbon-Carbon (RCC) panels that comprise the orbiter's wing leading edge and nose cap. Various nondestructive inspection techniques have been used in the examination of the RCC, but thermography has emerged as an effective inspection alternative to more traditional methods. Thermography is a non-contact inspection method as compared to ultrasonic techniques which typically require the use of a coupling medium between the transducer and material. Like radiographic techniques, thermography can inspect large areas, but has the advantage of minimal safety concerns and the ability for single-sided measurements. Details of the analysis technique that has been developed to allow insitu inspection of a majority of shuttle RCC components is discussed. Additionally, validation testing, performed to quantify the performance of the system, will be discussed. Finally, the results of applying this technology to the Space Shuttle Discovery after its return from the STS-114 mission in July 2005 are discussed. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Cramer, KE (reprint author), NASA, Langley Res Ctr, MS 231, Hampton, VA 23681 USA. NR 6 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 0-8194-6261-6 J9 P SOC PHOTO-OPT INS PY 2006 VL 6205 BP B2051 EP B2051 AR 62051B DI 10.1117/12.669684 PG 9 WC Optics SC Optics GA BES54 UT WOS:000239298200042 ER PT S AU Gazarik, M Johnson, D Kist, E Novak, F Antill, C Haakenson, D Howell, P Pandolf, J Jenkins, R Yates, R Stephan, R Hawk, D Amoroso, M AF Gazarik, Michael Johnson, Dave Kist, Ed Novak, Frank Antill, Charles Haakenson, David Howell, Patricia Pandolf, John Jenkins, Rusty Yates, Rusty Stephan, Ryan Hawk, Doug Amoroso, Michael BE Miles, JJ Peacock, GR Knettel, KM TI Development of an extra-vehicular (EVA) infrared (IR) camera inspection system - art. no. 62051C SO Thermosense XXVIII SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Thermosense XXVII CY APR 17-20, 2006 CL Kissimmee, FL SP SPIE AB Designed to fulfill a critical inspection need for the Space Shuttle Program, the EVA IR Camera System can detect crack and subsurface defects in the Reinforced Carbon-Carbon (RCC) sections of the Space Shuttle's Thermal Protection System (TPS). The EVA IR Camera performs this detection by taking advantage of the natural thermal gradients induced in the RCC by solar flux and thermal emission from the Earth. This instrument is a compact, low-mass, low-power solution (1.2cm3, 1.5kg, 5.0W) for TPS inspection that exceeds existing requirements for feature detection. Taking advantage of ground-based IR thermography techniques, the EVA IR Camera System provides the Space Shuttle program with a solution that can be accommodated by the existing inspection system. The EVA IR Camera System augments the visible and laser inspection systems and finds cracks and subsurface damage that is not measurable by the other sensors, and thus fills a critical gap in the Space Shuttle's inspection needs. This paper discusses the on-orbit RCC inspection measurement concept and requirements, and then presents a detailed description of the EVA IR Camera System design. C1 NASA, Lyndon B Johnson Space Ctr, Washington, DC 20546 USA. RP Gazarik, M (reprint author), NASA, Lyndon B Johnson Space Ctr, 300 E St SW, Washington, DC 20546 USA. RI Johnson, David/F-2376-2015 OI Johnson, David/0000-0003-4399-5653 NR 0 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 0-8194-6261-6 J9 P SOC PHOTO-OPT INS PY 2006 VL 6205 BP C2051 EP C2051 AR 62051C DI 10.1117/12.669683 PG 12 WC Optics SC Optics GA BES54 UT WOS:000239298200043 ER PT B AU Atkinson, DJ AF Atkinson, DJ BE Sterritt, R Hinchey, MG Bapty, T TI Constellation program return to the moon: Software systems challenges SO Third IEEE International Workshop on Engineering of Autonomic & Autonomous Systems (EASe 2006), Proceedings LA English DT Proceedings Paper CT 3rd IEEE International Workshop on Engineering of Autonomic and Autonomous Systems CY APR 24-28, 2006 CL Columbia, MD SP IEEE Comp Soc Task Force Autonomous & Autonom Syst, IEEE Comp Soc TC Engn Comp Based Syst, IBM, Univ Ulster Ctr Software Proc Technologies, Univ Ulster Comp Sci Res Inst, NASA Software Engn Lab, NASA Goddard Space Flight Ctr, Vanderbilt Univ Inst Software Integrated Syst AB This talk will introduce NASA's Constellation Program, which is developing new space systems for renewed human exploration of the moon, and eventually, Mars. A selection of challenges for software systems will be introduced that arise from the special circumstances of Constellation Systems. These challenges illustrate a variety of the types of problems that must be addressed related to software quality, automation and autonomy. For example, Constellation program-level systems engineering and integration activities are tasked with ensuring interoperability, reuse, compatibility, and evolutionary upgrade of all systems. To further compound the challenges, Constellation missions represent a mixing of the human space-flight processes with those of NASA's robotic exploration missions. These factors and others give rise to many unique and/or significantly more complex engineering than has been previously faced in the development of space systems. In this context, software reliability and safety become critical qualities for what will arguably be the most complex software systems artifact ever created. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Atkinson, DJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 0 TC 0 Z9 0 U1 1 U2 1 PU IEEE COMPUTER SOC PI LOS ALAMITOS PA 10662 LOS VAQUEROS CIRCLE, PO BOX 3014, LOS ALAMITOS, CA 90720-1264 USA BN 0-7695-2544-X PY 2006 BP 5 EP 162 PG 158 WC Automation & Control Systems; Computer Science, Software Engineering; Computer Science, Theory & Methods SC Automation & Control Systems; Computer Science GA BEE15 UT WOS:000236909400009 ER PT B AU Pena, J Hinchey, MG Sterritt, R AF Pena, J Hinchey, MG Sterritt, R BE Sterritt, R Hinchey, MG Bapty, T TI Towards modeling, specifying and deploying policies in autonomous and autonomic systems using an AOSE methodology SO THIRD IEEE INTERNATIONAL WORKSHOP ON ENGINEERING OF AUTONOMIC & AUTONOMOUS SYSTEMS (EASE 2006), PROCEEDINGS LA English DT Proceedings Paper CT 3rd IEEE International Workshop on Engineering of Autonomic and Autonomous Systems CY MAR 27-30, 2006 CL Potsdam, GERMANY SP IEEE Comp Soc Task Force Autonomous & Autonom Syst, IEEE Comp Soc TC Engn Comp Based Syst, IBM, Univ Ulster Ctr Software Proc Technologies, Univ Ulster Comp Sci Res Inst, NASA Software Engn Lab, NASA Goddard Space Flight Ctr, Vanderbilt Univ Inst Software Integrated Syst 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. We look at ways to achieve this, and in particular focus on Agent-Oriented Software Engineering. We propose utilizing an AOSE methodology for specifying autonomic and autonomous properties of the system independently, and later by means of composition of these specifications, to construct a specification for the policy and its subsequent deployment. C1 Univ Seville, Seville, Spain. NASA, Goddard Space Flight Ctr, Washington, DC USA. Univ Ulster, Coleraine BT52 1SA, Londonderry, North Ireland. RP Univ Seville, Seville, Spain. EM joaquinp@us.es; Michael.G.Hinchey@nasa.gov; r.sterritt@ulster.ac.uk RI Pena, Joaquin /K-8217-2012 OI Pena, Joaquin /0000-0001-9216-9695 NR 27 TC 3 Z9 3 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 0-7695-2544-X PY 2006 BP 37 EP + DI 10.1109/EASE.2006.22 PG 2 WC Automation & Control Systems; Computer Science, Software Engineering; Computer Science, Theory & Methods SC Automation & Control Systems; Computer Science GA BEE15 UT WOS:000236909400005 ER PT B AU Breitman, K Truszkowski, W Felicissimo, CH AF Breitman, K Truszkowski, W Felicissimo, CH BE Sterritt, R Hinchey, MG Bapty, T TI The Autonomic Semantic Desktop: helping users cope with information system complexity SO THIRD IEEE INTERNATIONAL WORKSHOP ON ENGINEERING OF AUTONOMIC & AUTONOMOUS SYSTEMS (EASE 2006), PROCEEDINGS LA English DT Proceedings Paper CT 3rd IEEE International Workshop on Engineering of Autonomic and Autonomous Systems CY APR 24-28, 2006 CL Columbia, MD SP IEEE Comp Soc Task Force Autonomous & Autonom Syst, IEEE Comp Soc TC Engn Comp Based Syst, IBM, Univ Ulster Ctr Software Proc Technologies, Univ Ulster Comp Sci Res Inst, NASA Software Engn Lab, NASA Goddard Space Flight Ctr, Vanderbilt Univ Inst Software Integrated Syst ID WEB AB In this paper we present the architecture for the Autonomic Semantic Desktop, an self managing application designed to hide system complexity and alleviate users from burdening and time consuming management tasks. The proposed architecture is founded in the basic principles of autonomic systems, i.e. the set of self attributes. We introduce a semantic layer to the architecture, to allow machines to process and exchange information without requiring human mediation. The underlying conceptual model used in this layer is Ontology, currently the lingua franca in application on the Semantic Web. C1 Pontificia Univ Catolica Rio de Janeiro, BR-22453 Rio De Janeiro, Brazil. NASA, Goddard Space Flight Ctr, Washington, DC USA. RP Pontificia Univ Catolica Rio de Janeiro, BR-22453 Rio De Janeiro, Brazil. EM karin@inf.puc-rio.br; Walt.Truszkowski@nasa.gov; carol@les.inf.puc-rio.br RI Felicissimo, Carolina/G-8629-2016 OI Felicissimo, Carolina/0000-0001-5065-2689 FU CNPq - ESSMA [552068/2002-0]; CNPq-PROSET [551241/2005-5] FX This research was supported in part by CNPq under contracts ESSMA - 552068/2002-0, and PROSET - 551241/2005-5. 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 0-7695-2544-X PY 2006 BP 156 EP + PG 2 WC Automation & Control Systems; Computer Science, Software Engineering; Computer Science, Theory & Methods SC Automation & Control Systems; Computer Science GA BEE15 UT WOS:000236909400018 ER PT S AU Groce, A Joshi, R AF Groce, Alex Joshi, Rajeev BE Hermanns, H Palsberg, J TI Exploiting m-aces in program analysis SO TOOLS AND ALGORITHMS FOR THE CONSTRUCTION AND ANALYSIS OF SYSTEMS, PROCEEDINGS SE Lecture Notes in Computer Science LA English DT Article; Proceedings Paper CT 12th International Conference on Tools and Algorithms for the Construction and Analysis of Systems CY MAR 25-APR 02, 2006 CL Vienna, AUSTRIA AB From operating systems and web browsers to spacecraft, many software systems maintain a log of events that provides a partial history of execution, supporting post-mortem (or post-reboot) analysis. Unfortunately, bandwidth, storage limitations, and privacy concerns limit the information content of logs, making it difficult to fully reconstruct execution from these traces. This paper presents a technique for modifying a program such that it can produce exactly those executions consistent with a given (partial) trace of events, enabling efficient analysis of the reduced program. Our method requires no additional history variables to track log events, and it can slice away code that does not execute in a given trace. We describe initial experiences with implementing our ideas by extending the CBMC bounded model checker for C programs. Applying our technique to a small, 400-line file system written in C, we get more than three orders of magnitude improvement in running time over a naive approach based on adding history variables, along with fifty- to eighty-fold reductions in the sizes of the SAT problems solved. C1 CALTECH, Jet Prop Lab, Lab Reliable Software, Pasadena, CA 91109 USA. RP Groce, A (reprint author), CALTECH, Jet Prop Lab, Lab Reliable Software, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Alex.D.Groce@jpl.nasa.gov; Rajeev.Joshi@jpl.nasa.gov NR 20 TC 3 Z9 3 U1 0 U2 0 PU SPRINGER-VERLAG BERLIN PI BERLIN PA HEIDELBERGER PLATZ 3, D-14197 BERLIN, GERMANY SN 0302-9743 BN 3-540-33056-9 J9 LECT NOTES COMPUT SC PY 2006 VL 3920 BP 379 EP 393 PG 15 WC Computer Science, Theory & Methods SC Computer Science GA BEE50 UT WOS:000236941100025 ER PT J AU Tsuji, JS Maynard, AD Howard, PC James, JT Lam, CW Warheit, DB Santamaria, AB AF Tsuji, JS Maynard, AD Howard, PC James, JT Lam, CW Warheit, DB Santamaria, AB TI Research strategies for safety evaluation of nanomaterials, part IV: Risk assessment of nanoparticles SO TOXICOLOGICAL SCIENCES LA English DT Editorial Material DE nanotechnology; nanoparticles; risk assessment; exposure assessment ID TITANIUM-DIOXIDE PARTICLES; COMPARATIVE PULMONARY TOXICITY; CARBON NANOTUBE MATERIAL; ULTRAFINE PARTICLES; INHALED PARTICLES; OXIDE PARTICLES; TIO2 PARTICLES; INHALATION; LUNG; EXPOSURE AB Nanoparticles are small-scale substances (< 100 nm) with unique properties and, thus, complex exposure and health risk implications. This symposium review summarizes recent findings in exposure and toxicity of nanoparticles and their application for assessing human health risks. Characterization of airborne particles indicates that exposures will depend on particle behavior (e.g., disperse or aggregate) and that accurate, portable, and cost-effective measurement techniques are essential for understanding exposure. Under many conditions, dermal penetration of nanoparticles may be limited for consumer products such as sunscreens, although additional studies are needed on potential photooxidation products, experimental methods, and the effect of skin condition on penetration. Carbon nanotubes apparently have greater pulmonary toxicity (inflammation, granuloma) in mice than fine-scale carbon graphite, and their metal content may affect toxicity. Studies on TiO2 and quartz illustrate the complex relationship between toxicity and particle characteristics, including surface coatings, which make generalizations (e.g., smaller particles are always more toxic) incorrect for some substances. These recent toxicity and exposure data, combined with therapeutic and other related literature, are beginning to shape risk assessments that will be used to regulate the use of nanomaterials in consumer products. C1 Exponent, Bellevue, WA 98007 USA. Woodrow Wilson Int Ctr Scholars, Washington, DC 20004 USA. US FDA, Natl Ctr Toxicol Res, Jefferson, AR 72079 USA. US FDA, Natl Toxicol Program, Ctr Phototoxicol, Jefferson, AR 72079 USA. NASA, Houston, TX 77058 USA. DuPont Co Inc, Haskell Lab, Newark, DE 19714 USA. Environ Int, Houston, TX 77002 USA. RP Tsuji, JS (reprint author), 15375 SE 30th Pl,Suite 250, Bellevue, WA 98007 USA. EM tsujij@exponent.com RI Maynard, Andrew/D-1076-2010; OI Maynard, Andrew/0000-0003-2117-5128 NR 61 TC 239 Z9 260 U1 9 U2 66 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 1096-6080 J9 TOXICOL SCI JI Toxicol. Sci. PD JAN PY 2006 VL 89 IS 1 BP 42 EP 50 DI 10.1093/toxsci/kfi339 PG 9 WC Toxicology SC Toxicology GA 993XN UT WOS:000233991000004 PM 16177233 ER PT J AU Gray, AK Kendall, AW Wing, BL Carls, MG Heifetz, J Li, ZZ Gharrett, AJ AF Gray, AK Kendall, AW Wing, BL Carls, MG Heifetz, J Li, ZZ Gharrett, AJ TI Identification and first documentation of larval rockfishes in southeast Alaskan waters was possible using mitochondrial markers but not pigmentation patterns SO TRANSACTIONS OF THE AMERICAN FISHERIES SOCIETY LA English DT Article ID GENUS SEBASTES; PACIFIC-OCEAN AB More than 30 species of rockfish (genus Sebastes) occur in Alaskan waters, but their larvae generally cannot be identified by morphology. Consequently, knowledge of life histories is incomplete for this commercially and ecologically valuable taxon, and the locations and habitats of the larvae of specific species have not been determined. We used mitochondrial DNA markers, which now can delineate most Alaskan rockfishes, to identify larvae collected in ichthyoplankton surveys conducted in Southeast Alaskan waters. We report the occurrence of 15 species or species groups. Sebastes zacentrus (sharpchin rockfish), S. proriger (redstripe rockfish), and members of the indistinguishable group S. variegatus (harlequin rockfish)-S. wilsoni (pygmy rockfish)-S. emphaeus (Puget Sound rockfish) were observed every year and in most collections in Chatham Strait and along western Prince of Wales Island. Sebastes zacentrus was abundant only in Chatham Strait; S. auriculatus (brown rockfish) and S. elongatus (greenstriped rockfish) were abundant only along Prince of Wales Island. All of the larvae detected occur in Southeast Alaskan waters as adults. In addition, we investigated whether pigmentation patterns can be used for visual identification. Larvae were divided into groups of similar pigmentation distribution and identified by means of mitochondrial markers. Pigment patterns on preflexion larvae do not appear to offer an effective way of identifying the species. Only the patterns of S. maliger (quillback rockfish) and S. caurinus (copper rockfish) in the subgenus Pteropodus were unique, and those patterns may be diagnostic for that subgenus. Intraspecific variation in pigmentation probably reflects a combination of ontogenetic change and adaptive responses to environmental variation. C1 Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, Div Fisheries, Juneau, AK 99801 USA. Natl Marine Fisheries Serv, Auke Bay Lab, Juneau, AK 99801 USA. RP Gharrett, AJ (reprint author), Univ Alaska Fairbanks, Sch Fisheries & Ocean Sci, Div Fisheries, 11120 Glacier Highway, Juneau, AK 99801 USA. EM ffajg@uaf.edu RI Bizzarro, Joseph/A-2988-2012 NR 33 TC 12 Z9 13 U1 1 U2 8 PU AMER FISHERIES SOC PI BETHESDA PA 5410 GROSVENOR LANE SUITE 110, BETHESDA, MD 20814-2199 USA SN 0002-8487 J9 T AM FISH SOC JI Trans. Am. Fish. Soc. PD JAN PY 2006 VL 135 IS 1 BP 1 EP 11 DI 10.1577/T04-168.1 PG 11 WC Fisheries SC Fisheries GA 013AH UT WOS:000235381500001 ER PT B AU Rankin, AL Matthies, LH Huertas, A AF Rankin, A. L. Matthies, L. H. Huertas, A. BE Parmentola, JA Rajendran, AM Bryzik, W Walker, BJ McCaulehy, JW Reifman, J Nasrabadi, NM TI Daytime water detection by fusing multiple cues for autonomous off-road navigation SO Transformational Science and Technology for the Current and Future Force SE SELECTED TOPICS IN ELECTRONICS AND SYSTEMS LA English DT Proceedings Paper CT 24th Army Science Conference CY NOV 29-DEC 02, 2004 CL Orlando, FL SP Army Acquist, Logist, & Technol, Assistant Secretary AB Detecting water hazards is a significant challenge to unmanned ground vehicle autonomous off-road navigation. This paper focuses on detecting the presence of water during the daytime using color cameras. A multi-cue approach is taken. Evidence of the presence of water is generated from color, texture, and the detection of reflections in stereo range data. A rule base for fusing water cues was developed by evaluating detection results from an extensive archive of data collection imagery containing water. This software has been implemented into a run-time passive perception subsystem and tested thus far under Linux on a Pentium based processor. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Rankin, AL (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 WORLD SCIENTIFIC PUBL CO PTE LTD PI SINGAPORE PA PO BOX 128 FARRER RD, SINGAPORE 9128, SINGAPORE BN 978-981-270-201-2 J9 SEL TOP ELECTR SYST PY 2006 VL 42 BP 177 EP + DI 10.1142/9789812772572_0023 PG 9 WC Engineering, Multidisciplinary; Multidisciplinary Sciences SC Engineering; Science & Technology - Other Topics GA BFR63 UT WOS:000244038200023 ER PT S AU Markwardt, CB AF Markwardt, C. B. BE DAmico, F Braga, J Rothschild, RE TI RXTE observations of galactic center transients SO Transient Milky Way: A Perspective for Mirax SE AIP CONFERENCE PROCEEDINGS LA English DT Proceedings Paper CT Workshop on Transient Milky Way - A Perspective for MIRAX CY DEC 07-09, 2005 CL Sao Jose dos Campos, BRAZIL SP Natl Inst Space Res, Brazilian Space Agcy DE galactic bulge RXTE PCA ID X-RAY BINARY; LOW-MASS; PULSAR; SYSTEM AB We present the results of monitoring observations of the galactic center and plane regions with the Rossi X-ray Timing Explorer PCA instrument. Since 1999, we have been performing these monitoring observations twice weekly, and since 2003, the survey solid angle is similar to 500 square degrees. Approximately 150 sources have been detected, of which about 32 were newly discovered. Four millisecond X-ray pulsars have been detected. Sources vary widely in flux as a function of time, and spend a significant portion of their lives in quiescence. C1 NASA, Goddard Space Flight Ctr, Astroparticle Lab, Greenbelt, MD 20771 USA. RP Markwardt, CB (reprint author), NASA, Goddard Space Flight Ctr, Astroparticle Lab, Code 661, Greenbelt, MD 20771 USA. NR 10 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 0-7354-0332-5 J9 AIP CONF PROC PY 2006 VL 840 BP 45 EP 49 PG 5 WC Astronomy & Astrophysics; Physics, Multidisciplinary SC Astronomy & Astrophysics; Physics GA BEO88 UT WOS:000238510000008 ER PT J AU Farman, M AF Farman, Mike TI THE SHAMBHALA ANTHOLOGY OF CHINESE POETRY SO TRANSLATION REVIEW LA English DT Book Review C1 [Farman, Mike] NASA, Washington, DC 20546 USA. RP Farman, M (reprint author), NASA, Washington, DC 20546 USA. NR 1 TC 0 Z9 0 U1 0 U2 2 PU UNIV TEXAS PI RICHARDSON PA TRANSLATION CENTER, BOX 830688, RICHARDSON, TX 75083-0688 USA SN 0737-4836 J9 TRANSLATION REV JI Transl. Rev. PY 2006 IS 72 BP 61 EP 62 PG 2 WC Language & Linguistics; Literature SC Linguistics; Literature GA V11VH UT WOS:000207558600009 ER PT B AU Nunes, A McClure, J Avila, R AF Nunes, Arthur McClure, John Avila, Ricardo BE David, SA DebRoy, T Lippold, JC Smartt, HB Vitek, JM TI TORQUE AND PLUNGE FORCE DURING THE PLUNGE PHASE OF FRICTION STIR WELDING SO TRENDS IN WELDING RESEARCH, PROCEEDINGS LA English DT Proceedings Paper CT 7th International Conference on Trends in Welding Research CY MAY 16-20, 2005 CL Pine Mt, GA SP ASM AB Torque and plunge force during the initial plunge phase in Friction Stir Welding were measured for a 0.5 inch diameter pin entering a 2219 aluminum alloy plate. Weld structures were preserved for metallographic observation by making emergency stops at various plunge depths. The plunging pin tool is seen to be surrounded by a very fine grained layer of recrystallized metal extending substantially below the bottom of the pin, implying a shear interface in the metal below and not at the tool-metal interface. Torque and plunge force during the initial plunge phase in Friction Stir Welding are calculated from a straightforward model based on a concept to plastic flow in the vicinity of the plunging tool compatible with structural observations. The concept: a disk of weld metal seized to and rotating with the bottom of the pin is squeezed out laterally by the plunge force and extruded upwards in a hollow cylinder around the tool. As the shear surface separating rotating disk from stationary weld metal engulfs fresh metal, the fresh metal is subjected to severe shear deformation, which results in its recrystallization. Encouraging agreement between computations and measured torque and plunge force is obtained. C1 [Nunes, Arthur] NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Nunes, A (reprint author), NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. NR 11 TC 0 Z9 0 U1 0 U2 1 PU ASM INTERNATIONAL PI MATERIALS PARK PA 9503 KINSMAN RD, MATERIALS PARK, OH 44073 USA BN 978-0-87170-842-7 PY 2006 BP 241 EP 245 PG 5 WC Metallurgy & Metallurgical Engineering SC Metallurgy & Metallurgical Engineering GA BPT87 UT WOS:000279918300038 ER PT J AU DellaCorte, C AF DellaCorte, C TI 2006 begins with a decidedly technical emphasis SO TRIBOLOGY & LUBRICATION TECHNOLOGY LA English DT Editorial Material C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP DellaCorte, C (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM cdellacorte@stle.org NR 0 TC 1 Z9 1 U1 0 U2 0 PU SOC TRIBOLOGISTS & LUBRICATION ENGINEERS PI PARK RIDGE PA 840 BUSSE HIGHWAY, PARK RIDGE, IL 60068 USA SN 0024-7154 J9 TRIBOL LUBR TECHNOL JI Tribol. Lubr. Technol. PD JAN PY 2006 VL 62 IS 1 BP 6 EP 6 PG 1 WC Engineering, Mechanical SC Engineering GA 004AS UT WOS:000234725000002 ER PT B AU Grant, MM Hill, JR AF Grant, Michael M. Hill, Janette R. BE Lambert, R McCarthy, C TI WEIGHING THE RISKS WITH THE REWARDS Implementing Student-Centered Pedagogy Within High Stakes Testing SO UNDERSTANDING TEACHER STRESS IN AN AGE OF ACCOUNTABILITY SE Research on Stress and Coping in Education LA English DT Article; Book Chapter ID K-W-L; TEACHERS; ENVIRONMENTS; STRATEGIES; STANDARDS; CLASSROOM; CULTURE; SCHOOL C1 [Grant, Michael M.] Univ Memphis, Instruct Design & Technol Program, Memphis, TN 38152 USA. [Hill, Janette R.] Univ Georgia, Coll Educ, Athens, GA 30602 USA. [Grant, Michael M.] NASA, Johnson Space Ctr, Washington, DC USA. RP Grant, MM (reprint author), Univ Memphis, Instruct Design & Technol Program, Memphis, TN 38152 USA. NR 68 TC 0 Z9 0 U1 0 U2 0 PU INFORMATION AGE PUBLISHING-IAP PI CHARLOTTE PA PO BOX 79049, CHARLOTTE, NC 28271-7047 USA BN 978-1-59311-473-2 J9 RES STRESS COPING ED PY 2006 BP 19 EP 42 PG 24 WC Education & Educational Research; Psychology, Educational SC Education & Educational Research; Psychology GA BKD78 UT WOS:000267842400002 ER PT S AU Jobson, DJ Rahman, ZU Woodell, GA Hines, GD AF Jobson, Daniel J. Rahman, Zia-ur Woodell, Glenn A. Hines, Glenn D. BE Rahman, Z Reichenbach, SE Neifeld, MA TI A comparison of visual statistics for the image enhancement of FORESITE aerial images with those of major image classes - art. no. 62460 SO Visual Information Processing XV SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Visual Information Processing XV CY APR 18-19, 2006 CL Kissimmee, FL SP SPIE ID RETINEX AB Aerial images from the Follow-On Radar, Enhanced and Synthetic Vision Systems Integration Technology Evaluation (FORESITE) flight tests with the NASA Langley Research Center's research Boeing 757 were acquired during severe haze and haze/mixed clouds visibility conditions. These images were enhanced using the Visual Servo (VS) process that makes use of the Multiscale Retinex. The images were then quantified with visual quality metrics used internally within the VS. One of these metrics, the Visual Contrast Measure, has been computed for hundreds of FORESITE images, and for major classes of imaging-terrestrial (consumer), orbital Earth observations, orbital Mars surface imaging, NOAA aerial photographs, and underwater imaging. The metric quantifies both the degree of visual impairment of the original, un-enhanced images as well as the degree of visibility improvement achieved by the enhancement process. The large aggregate data exhibits trends relating to degree of atmospheric visibility attenuation, and its impact on the limits of enhancement performance for the various image classes. Overall results support the idea that in most cases that do not involve extreme reduction in visibility, large gains in visual contrast are routinely achieved by VS processing. Additionally, for very poor visibility imaging, lesser, but still substantial, gains in visual contrast are also routinely achieved. Further, the data suggest that these visual quality metrics can be used as external standalone metrics for establishing performance parameters. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Jobson, DJ (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 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 0-8194-6302-7 J9 P SOC PHOTO-OPT INS PY 2006 VL 6246 BP 62460 EP 62460 AR 62460 DI 10.1117/12.664591 PG 8 WC Imaging Science & Photographic Technology SC Imaging Science & Photographic Technology GA BES09 UT WOS:000239233200001 ER PT S AU Woodell, G Jobson, DJ Rahmanb, ZU Hines, G AF Woodell, Glenn Jobson, Daniel J. Rahmanb, Zia-ur Hines, Glenn BE Rahman, Z Reichenbach, SE Neifeld, MA TI Advanced image processing of aerial imagery - art. no. 62460E SO Visual Information Processing XV SE PROCEEDINGS OF THE SOCIETY OF PHOTO-OPTICAL INSTRUMENTATION ENGINEERS (SPIE) LA English DT Proceedings Paper CT Conference on Visual Information Processing XV CY APR 18-19, 2006 CL Kissimmee, FL SP SPIE DE retinex; visual servo; image enhancement; poor visibility; aerial imagery ID RETINEX AB Aerial imagery of the Earth is an invaluable tool for the assessment of ground features, especially during times of disaster. Researchers at NASA's Langley Research Center have developed techniques which have proven to be useful for such imagery. Aerial imagery from various sources, including Langley's Boeing 757 Aries aircraft, has been studied extensively. This paper discusses these studies and demonstrates that better-than-observer imagery can be obtained even when visibility is severely compromised. A real-time, multi-spectral experimental system will be described and numerous examples will be shown. C1 NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Woodell, G (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA. NR 14 TC 5 Z9 5 U1 0 U2 0 PU SPIE-INT SOC OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98227-0010 USA SN 0277-786X BN 0-8194-6302-7 J9 P SOC PHOTO-OPT INS PY 2006 VL 6246 BP E2460 EP E2460 AR 62460E DI 10.1117/12.666767 PG 12 WC Imaging Science & Photographic Technology SC Imaging Science & Photographic Technology GA BES09 UT WOS:000239233200013 ER PT S AU Gerald-Yamasaki, MJ AF Gerald-Yamasaki, Michael J. BE Erbacher, RF Roberts, JC Grohn, MT Borner, K TI Correspondence-based visualization techniques SO VISUALIZATION AND DATA ANALYSIS 2006 SE Proceedings of SPIE LA English DT Proceedings Paper CT Conference on Visualization and Data Analysis 2006 CY JAN 16-17, 2006 CL San Jose, CA SP Soc Imaging Sci & Technol, SPIE DE flow visualization; texture synthesis; vector field topology ID OF-THE-ART; FLOW VISUALIZATION; VECTOR-FIELDS; TOPOLOGY AB A Visual representation model is an abstract pattern used to create images which characterize quantitative information. By using a texture image to define a visual representation model, correspondence of color to denote similarity, and correspondence of image location over multiple images to associate information into collections, highly effective Visualization techniques are made possible. One Such technique for two-dimensional texture-based vector field Visualization is vector field marquetry. Vector field marquetry uses a synthesized image representing direction as a conditioner for pixel replacement over a collection of vector field direction-magnitude portraits. The resulting synthesized image displays easily recognizable local and global features. vector direction, and magnitude. A related technique enabled by correspondence-based methods is the sparse representation of a vector field by a topological skeleton constructed from isodirection lines. Each vector in a vector field along an isodirection line points in the same direction. Isodirection lines Subdivide the domain into regions of similar vectors, converge at critical points, and represent global characteristics of the vector field. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Gerald-Yamasaki, MJ (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. NR 20 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 0-8194-6100-8 J9 PROC SPIE PY 2006 VL 6060 AR 606014 DI 10.1117/12.643097 PG 12 WC Computer Science, Information Systems SC Computer Science GA BEF54 UT WOS:000237098700037 ER PT S AU de Mello, DF AF de Mello, D. F. GP Unam BE Infante, L Rubio, M TorresPeimbert, S TI Census of the star-forming galaxy population at z < 1.5 SO XI IAU Regional Latin American Meeting of Astronomy SE REVISTA MEXICANA DE ASTRONOMIA Y ASTROFISICA, SERIE DE CONFERENCIAS LA English DT Proceedings Paper CT 11th IAU Regional Latin American Meeting of Astronomy CY DEC 12-16, 2005 CL Pucon, CHILE DE galaxies : evolution; galaxies : formation; galaxies : starburst ID HIGH-REDSHIFT GALAXIES; DEEP FIELD; ULTRAVIOLET; SPECTRA; LIMIT AB A key question in galaxy evolution is the physical nature of the intermediate redshift galaxies and their present-day counterparts. It is known that the star formation rate density increases rapidly from z = 0 to z = 1 - 2. However, the type of galaxies that contribute to the rise of the star formation density is still debatable. In principle, a steep luminosity function where most of the star-formation is in newly-formed dwarf galaxies or a population of massive galaxies undergoing modest but continuous star formation can produce similar star-formation rate density at a given redshift. Therefore, a census of the star-forming galaxy population as a function of time is needed in order to help us better understand how galaxies acquired their present morphology. C1 NASA, Goddard Space Flight Ctr, CUA, Observat Cosmol Lab, Greenbelt, MD 20771 USA. RP de Mello, DF (reprint author), NASA, Goddard Space Flight Ctr, CUA, Observat Cosmol Lab, Code 661, Greenbelt, MD 20771 USA. NR 13 TC 0 Z9 0 U1 0 U2 0 PU UNIVERSIDAD NACIONAL AUTONOMA MEXICO INSTITUTO ASTRONOMIA PI MEXICO CITY PA APARTADO POSTAL 70-264, MEXICO CITY 04510, MEXICO SN 1405-2059 BN 978-970-32-2804-1 J9 REV MEX AST ASTR PY 2006 VL 26 BP 115 EP 116 PG 2 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA BFY87 UT WOS:000245470400046 ER PT J AU Stel'makh, S Grzanka, E Zhao, Y Palosz, W Palosz, B AF Stel'makh, S Grzanka, E Zhao, Y Palosz, W Palosz, B TI Neutron diffraction studies of the atomic vibrations of bulk and surface atoms of nanocrystalline SiC SO ZEITSCHRIFT FUR KRISTALLOGRAPHIE LA English DT Article; Proceedings Paper CT 9th European Powder Diffraction Conference CY SEP 02-05, 2004 CL Prague, CZECH REPUBLIC DE powder diffraction; neutron diffraction; atomic vibrations ID X-RAY-DIFFRACTION AB Thermal atomic motions of nanocrystalline SiC were characterized by two temperature atomic factors B-core and B-shell. With the use of wide angle neutron diffraction data it was shown that at the diffraction vector of above 15 angstrom(-1) the Wilson plot gives directly the temperature factor of the grain interior (B-core). At lower Q values the slope of the plot provides information on the relative amplitudes of vibrations of the core and shell atoms. C1 Inst High Pressure Phys, UNIPRESS, PL-01142 Warsaw, Poland. Los Alamos Neutron Scattering Ctr, Los Alamos, NM 87545 USA. NASA, George C Marshall Space Flight Ctr, BAE Syst, Huntsville, AL 35812 USA. RP Stel'makh, S (reprint author), Inst High Pressure Phys, UNIPRESS, Ul Sokolowska 29-37, PL-01142 Warsaw, Poland. EM svrit@unipress.waw.pl RI Lujan Center, LANL/G-4896-2012 NR 10 TC 2 Z9 2 U1 0 U2 2 PU OLDENBOURG VERLAG PI MUNICH PA LEKTORAT MINT, POSTFACH 80 13 60, D-81613 MUNICH, GERMANY SN 0044-2968 J9 Z KRISTALLOGR JI Z. Kristall. PY 2006 SU 23 BP 331 EP 336 PN 2 PG 6 WC Crystallography SC Crystallography GA 057PQ UT WOS:000238608100012 ER PT J AU Crow, WT Koster, RD Reichle, RH Sharif, HO AF Crow, WT Koster, RD Reichle, RH Sharif, HO TI Relevance of time-varying and time-invariant retrieval error sources on the utility of spaceborne soil moisture products SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SYSTEM SIMULATION EXPERIMENT; AMSR-E; MICROWAVE; MODELS; IMPACT; WATER AB Errors in remotely-sensed soil moisture retrievals originate from a combination of time-invariant and time-varying sources. For land modeling applications such as forecast initialization, some of the impact of time-invariant sources can be removed given known differences between observed and modeled soil moisture climatologies. Nevertheless, the distinction is seldom made when evaluating remotely-sensed soil moisture products. Here we describe an Observing System Simulation Experiment (OSSE) for radiometer-only soil moisture products derived from the NASA Hydrosphere States ( Hydros) mission where the impact of time-invariant errors is explicitly removed via the linear rescaling of retrievals. OSSE results for the 575,000 km(2) Red-Arkansas River Basin indicate that climatological rescaling may significantly reduce the perceived magnitude of Hydros soil moisture retrieval errors and expands the geographic areas over which retrievals demonstrate value for land surface modeling applications. C1 ARS, Hydrol & Remote Sensing Lab, USDA, Beltsville, MD 20705 USA. NASA, Goddard Space Flight Ctr, Global Modeling & Assimilat Off, Greenbelt, MD 20771 USA. Univ Texas, Dept Civil Engn, San Antonio, TX 78249 USA. Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. RP Crow, WT (reprint author), ARS, Hydrol & Remote Sensing Lab, USDA, Rm 104,Bldg 007,BARC-W, Beltsville, MD 20705 USA. EM wcrow@hydrolab.arsusda.gov RI Sharif, Hatim/E-4426-2010; Reichle, Rolf/E-1419-2012; Koster, Randal/F-5881-2012 OI Koster, Randal/0000-0001-6418-6383 NR 15 TC 25 Z9 25 U1 1 U2 5 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 31 PY 2005 VL 32 IS 24 AR L24405 DI 10.1029/2005GL024889 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 001AZ UT WOS:000234506100007 ER PT J AU Kwok, R AF Kwok, R TI Variability of Nares Strait ice flux SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SEA-ICE; WATER; VOLUME; OCEAN; HEAT AB Six years ( 1996 - 2002) of Arctic Ocean ice flux into the Nares Strait are estimated using RADARSAT ice motion. This represents a first consistent multi-year record of Nares Strait outflow for examination of seasonal and interannual variability. Across an similar to 30 km gate at the entrance to Robeson Channel, the average annual (Sept - Aug) ice area flux is 33 x 10(3) km(2) and ranges from 16 x 10(3) km(2) in 2000 to 48 x 10(3) km(2) in 1999. Uncertainties in the 3-day ice displacements and ice flux are small. Assuming 4 m thick ice, the average volume flux amounts to similar to 130 km(3) (similar to 4 mSv); this is similar to 7% of the mean annual Fram Strait ice flux. Seasonally, ice flux is most active after July, ceases after the formation of an ice arch in mid- to late-winter, and re-commences after breakup in summer. The multiyear ( MY) ice coverage of the area poleward of the gate is high (> 80%). South of the gate, the MY ice coverage is highly variable and the strait may be filled with multiyear or seasonal ice. Our estimates are placed in the context of others and uncertainties in the other components of Canadian Archipelago ice flux and are discussed. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kwok, R (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM ron.kwok@jpl.nasa.gov RI Kwok, Ron/A-9762-2008 OI Kwok, Ron/0000-0003-4051-5896 NR 14 TC 10 Z9 10 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 31 PY 2005 VL 32 IS 24 AR L24502 DI 10.1029/2005GL024768 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 001AZ UT WOS:000234506100006 ER PT J AU Wooster, MJ Roberts, G Perry, GLW Kaufman, YJ AF Wooster, MJ Roberts, G Perry, GLW Kaufman, YJ TI Retrieval of biomass combustion rates and totals from fire radiative power observations: FRP derivation and calibration relationships between biomass consumption and fire radiative energy release SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SENSITIVITY-ANALYSIS; PYROGENIC EMISSIONS; SOUTHERN AFRICA; BURNED AREA; EOS-MODIS; SCAR-B; TEMPERATURE; SATELLITE; AEROSOLS; SAVANNA AB [1] Estimates of wildfire aerosol and trace gas emissions are most commonly derived from assessments of biomass combusted. The radiative component of the energy liberated by burning fuel can be measured by remote sensing, and spaceborne fire radiative energy (FRE) measures can potentially provide detailed information on the amount and rate of biomass consumption over large areas. To implement the approach, spaceborne sensors must be able to derive fire radiative power (FRP) estimates from subpixel fires using observations in just one or two spectral channels, and calibration relationships between radiated energy and fuel consumption must be developed and validated. This paper presents results from a sensitivity analysis and from experimental fires conducted to investigate these issues. Within their methodological limits, the experimental work shows that FRP assessments made via independent hyperspectral and MIR radiance approaches in fact show good agreement, and fires are calculated to radiate 14 +/- 3% [ mean +/- 1S. D.] of their theoretically available heat yield in a form capable of direct assessment by a nadir-viewing MIR imager. The relationship between FRE and fuel mass combusted is linear and highly significant ( r(2) = 0.98, n = 29, p < 0.0001), and FRP is well related to combustion rate ( r(2) = 0.90, n = 178, p < 0.0001), though radiation from the still-hot fuel bed can sometimes contribute significant FRP from areas where combustion has ceased. We conclude that FRE assessment offers a powerful tool for supplementing existing burned-area based fuel consumption measures, and thus shows significant promise for enhancing pyrogenic trace gas and aerosol emissions estimates. C1 Kings Coll London, Dept Geog, London WC2R 2LS, England. NASA, Atmospheres Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Auckland, Sch Geog & Environm Sci, Auckland 1, New Zealand. RP Kings Coll London, Dept Geog, London WC2R 2LS, England. EM martin.wooster@kcl.ac.uk NR 60 TC 196 Z9 200 U1 13 U2 38 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 31 PY 2005 VL 110 IS D24 AR D24311 DI 10.1029/2005JD006318 PG 24 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 001BF UT WOS:000234506700001 ER PT J AU Ponomareva, I Menon, M Srivastava, D Andriotis, AN AF Ponomareva, I Menon, M Srivastava, D Andriotis, AN TI Structure, stability, and quantum conductivity of small diameter silicon nanowires SO PHYSICAL REVIEW LETTERS LA English DT Article ID MOLECULAR-DYNAMICS SCHEME; LASER-ABLATION; TEMPERATURE; FLOW AB Structures and energetics of various types of silicon nanowires have been investigated using both quantum and classical molecular dynamics simulations to determine the most stable forms. The tetrahedral type nanowires have been found to be the most stable and, surprisingly, the polycrystalline forms of nanowires, while having the smallest surface to bulk ratio, are found to be the least stable. We also show that the cagelike nanowires have greater thermal stability than the tetrahedral nanowires. Furthermore, their electrical conducting properties are found to be better than those of tetrahedral nanowires, suggesting useful molecular electronic applications. C1 Univ Arkansas, Dept Phys, Fayetteville, AR 72701 USA. Univ Kentucky, Dept Phys & Astron, Lexington, KY 40506 USA. Univ Kentucky, Ctr Computat Sci, Lexington, KY 40506 USA. NASA, Ames Ctr Nanotechnol, UARC, Moffett Field, CA 94035 USA. Fdn Res & Technol Hellas, Inst Elect Struct & Laser, Iraklion 71100, Crete, Greece. RP Ponomareva, I (reprint author), Univ Arkansas, Dept Phys, Fayetteville, AR 72701 USA. EM iponoma@uark.edu; super250@pop.uky.edu; deepak@nas.nasa.gov; andriot@iesl.forth.gr RI Ponomareva, Inna/C-4067-2012; Andriotis, Antonios/A-2848-2014 NR 20 TC 58 Z9 61 U1 0 U2 6 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 0031-9007 EI 1079-7114 J9 PHYS REV LETT JI Phys. Rev. Lett. PD DEC 31 PY 2005 VL 95 IS 26 AR 265502 DI 10.1103/PhysRevLett.95.265502 PG 4 WC Physics, Multidisciplinary SC Physics GA 998RV UT WOS:000234337900055 PM 16486370 ER PT J AU Kumar, S Hedges, SB AF Kumar, S Hedges, SB TI Pushing back the expansion of introns in animal genomes SO CELL LA English DT Article ID GENES C1 Arizona State Univ, Ctr Evolut Funct Genom, Biodesign Inst, Tempe, AZ 85287 USA. Arizona State Univ, Sch Life Sci, Tempe, AZ 85287 USA. Penn State Univ, Dept Biol, University Pk, PA 16802 USA. Penn State Univ, NASA, Astrobiol Inst, University Pk, PA 16802 USA. RP Kumar, S (reprint author), Arizona State Univ, Ctr Evolut Funct Genom, Biodesign Inst, Tempe, AZ 85287 USA. EM s.kumar@asu.edu RI Kumar, Sudhir/F-1411-2011 NR 8 TC 3 Z9 3 U1 0 U2 3 PU CELL PRESS PI CAMBRIDGE PA 1100 MASSACHUSETTS AVE, CAMBRIDGE, MA 02138 USA SN 0092-8674 J9 CELL JI Cell PD DEC 29 PY 2005 VL 123 IS 7 BP 1182 EP 1184 DI 10.1016/j.cell.2005.12.007 PG 3 WC Biochemistry & Molecular Biology; Cell Biology SC Biochemistry & Molecular Biology; Cell Biology GA 002AT UT WOS:000234584500006 PM 16377558 ER PT J AU Gerard, B Deuze, JL Herman, M Kaufman, YJ Lallart, P Oudard, C Remer, LA Roger, B Six, B Tanre, D AF Gerard, B Deuze, JL Herman, M Kaufman, YJ Lallart, P Oudard, C Remer, LA Roger, B Six, B Tanre, D TI Comparisons between POLDER 2 and MODIS/Terra aerosol retrievals over ocean SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID RESOLUTION IMAGING SPECTRORADIOMETER; ATMOSPHERE; SYSTEM; MODIS; INSTRUMENT; LAND; SCATTERING; CLIMATE AB [1] This paper presents a comparison between simultaneous radiance measurements and aerosol retrievals of POLDER 2/ADEOS 2 and MODIS/Terra, two instruments devoted to monitor the Earth and its atmosphere from space. This study focuses on aerosol remote sensing over ocean. Geophysical results from both inversions are compared. MODIS and POLDER total radiance ( and also polarized radiance for POLDER) measurements are compared with radiance simulations based on POLDER and MODIS inversed aerosol products (cross-simulations). Such comparisons emphasize advantages of each instrument and its inversion process. Both instruments generally agree on aerosol retrievals except when POLDER detects nonspherical particles within the coarse mode, which is not possible for MODIS. Combining measurements provided by POLDER 2 and MODIS, the spectral variation of optical properties of nonspherical aerosols can be derived. In order to retrieve more accurately aerosol optical properties, combining directional and polarized information from POLDER 2 with simultaneous MODIS spectral data is needed. The results of this study will guide us in the realization of a coupled inversion scheme. C1 Univ Sci & Technol Lille, Opt Atmospher Lab, F-59655 Villeneuve Dascq, France. NASA, Atmospheres Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Sci & Technol Lille, Pole ICARE, F-59655 Villeneuve Dascq, France. Univ Sci & Technol Lille, Ctr Ressources Informat, F-59655 Villeneuve Dascq, France. RP Gerard, B (reprint author), Univ Sci & Technol Lille, Opt Atmospher Lab, F-59655 Villeneuve Dascq, France. EM benoit.gerard@loa.univ-lille1.fr NR 22 TC 17 Z9 18 U1 2 U2 8 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 29 PY 2005 VL 110 IS D24 AR D24211 DI 10.1029/2005JD006218 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 001BD UT WOS:000234506500003 ER PT J AU Syed, TH Famiglietti, JS Chen, J Rodell, M Seneviratne, SI Viterbo, P Wilson, CR AF Syed, TH Famiglietti, JS Chen, J Rodell, M Seneviratne, SI Viterbo, P Wilson, CR TI Total basin discharge for the Amazon and Mississippi River basins from GRACE and a land-atmosphere water balance SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID FRESH-WATER; VARIABILITY; GRAVITY; STORAGE; SYSTEM AB Freshwater discharge along continental margins is a key Earth system variable that is not well monitored globally. Here we propose a method for estimating monthly river basin outflows based on the use of new GRACE satellite estimates of terrestrial water storage changes in a coupled land-atmosphere water balance. Using GRACE land water storage changes ( which include changes in groundwater storage) in the water balance method results in more holistic estimates of basin discharge, which we call total basin discharge, that include not only streamflow, but the net of surface, groundwater and tidal inflows and outflows. The method was tested on the Amazon and Mississippi river basins, and could ultimately be applied to the major drainage regions and river basins of the globe. Estimated Amazon total basin discharge was well correlated with observed streamflow, but with a phase lag and underestimation of low flows. Estimated total basin discharge in the Mississippi river basin had a greater annual amplitude than observed streamflow, but showed good temporal covariance. Results for both basins highlight important differences between estimated total basin discharge and observed streamflow, at least part of which can be attributed to groundwater storage changes. Atmospheric moisture data and methods of GRACE data processing also contributed to the differences. C1 Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. Univ Texas, Ctr Space Res, Austin, TX 78759 USA. NASA, Hydrol Sci Branch, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Swiss Fed Inst Technol, Inst Atmospher & Climate Sci, CH-8057 Zurich, Switzerland. European Ctr Medium Range Weather Forecasts, Reading RG2 9AX, Berks, England. Univ Texas, Dept Geol Sci, Austin, TX 78712 USA. RP Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. EM jfamigli@uci.edu RI Viterbo, Pedro/B-7184-2008; Seneviratne, Sonia/G-8761-2011; Rodell, Matthew/E-4946-2012; Syed, Tajdarul/G-6731-2014 OI Viterbo, Pedro/0000-0001-6587-3062; Seneviratne, Sonia/0000-0001-9528-2917; Rodell, Matthew/0000-0003-0106-7437; NR 18 TC 70 Z9 72 U1 2 U2 14 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 28 PY 2005 VL 32 IS 24 AR L24404 DI 10.1029/2005GL024851 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 001AW UT WOS:000234505700009 ER PT J AU Kim, W McMillan, RA Snyder, JP Conticello, VP AF Kim, W McMillan, RA Snyder, JP Conticello, VP TI A stereoelectronic effect on turn formation due to proline substitution in elastin-mimetic polypeptides SO JOURNAL OF THE AMERICAN CHEMICAL SOCIETY LA English DT Article ID INVERSE TEMPERATURE TRANSITION; DETERMINING COLLAGEN STABILITY; PROTEIN SECONDARY-STRUCTURE; NMR CHEMICAL-SHIFTS; TRIPLE-HELIX; AQUEOUS-SOLUTION; EXTRACELLULAR-MATRIX; MOLECULAR-DYNAMICS; CIRCULAR-DICHROISM; DIPEPTIDE ANALOGS AB Stereoelectronic effects have been identified as contributing factors to the conformational stability of collagen-mimetic peptide sequences. To assess the relevance of these factors within other protein structural contexts, three polypeptide sequences were prepared in which the sequences were derived from the canonical repeat unit (Val-Pro-Gly-Val-Gly) of the protein material elastin. These elastin-mimetic polypeptides, elastin-1, elastin-2, and elastin-3, incorporate (2S)-proline, (2S,4S)-4-fluoroproline, and (2S,4R)-4-fluoroproline, respectively, at the second position of the elastin repeat. Calorimetric and spectroscopic investigations of these three polypeptides indicate that the incorporation of the substituted proline residues had a dramatic effect upon the self-assembly of the corresponding elastin peptide. The presence of (2S,4R)-4-fluoroproline in elastin-3 lowered the temperature of the phase transition and increased the type II beta-turn population with respect to the parent polypeptide, while the presence of (2S,4S)-4-fluoroproline in elastin-2 had the opposite effect. These results suggest that stereoelectronic effects could either enhance or hinder the self-assembly of elastin-mimetic polypeptides, depending on the influence of the proline analogue on the energetics of the beta-turn conformation that develops within the pentapeptide structural repeats above the phase transition. Density functional theory (DFT) was employed to model three possible turn types (beta(I)-,beta(II)-, and inverse gamma-turns) derived from model peptide segments (MeCO-Xaa-Gly-NHMe) (Xaa = Pro, 4S-F-Pro, or 4R-F-Pro) corresponding to the turn-forming residues of the elastin repeat unit (Val-Pro-Gly-Val-Gly). The results of the these calculations suggested a similar outcome to the experimental data for the elastin-mimetic polypeptides, in that type II beta-turn structures were stabilized for peptide segments containing (2S,4R)-fluoroproline and destabilized for segments containing (2S,4S)fluoroproline relative to the canonical proline residue. C1 Emory Univ, Dept Chem, Atlanta, GA 30322 USA. NASA, Ames Res Ctr, Bioengn Branch, Moffett Field, CA 94035 USA. RP Conticello, VP (reprint author), Emory Univ, Dept Chem, 1515 Dickey Dr, Atlanta, GA 30322 USA. EM vcontic@emory.edu OI Conticello, Vincent/0000-0001-6940-6947 FU NHLBI NIH HHS [5R01HL071136-04] NR 81 TC 53 Z9 54 U1 1 U2 17 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 0002-7863 J9 J AM CHEM SOC JI J. Am. Chem. Soc. PD DEC 28 PY 2005 VL 127 IS 51 BP 18121 EP 18132 DI 10.1021/ja054105j PG 12 WC Chemistry, Multidisciplinary SC Chemistry GA 997PK UT WOS:000234258700043 PM 16366565 ER PT J AU Sato, R Sakamoto, T Kataoka, J Yoshida, A Suzuki, M Kotoku, J Urata, Y Yamamoto, Y Arimoto, M Tamagawa, T Shirasaki, Y Torii, K Matsuoka, M Nakagawa, Y Yamazaki, T Tanaka, K Maetou, M Yamauchi, M Takagishi, K Lamb, DQ Atteia, JL Vanderspek, R Graziani, C Prigozhin, G Villasenor, J Jernigan, JG Crew, GB Hurley, K Ricker, GR Woosley, SE Butler, N Levine, A Doty, JP Donaghy, TQ Fenimore, EE Galassi, M Boer, M Dezalay, JP Olive, JF Braga, J Manchanda, R Pizzichini, G Kawai, N AF Sato, R Sakamoto, T Kataoka, J Yoshida, A Suzuki, M Kotoku, J Urata, Y Yamamoto, Y Arimoto, M Tamagawa, T Shirasaki, Y Torii, K Matsuoka, M Nakagawa, Y Yamazaki, T Tanaka, K Maetou, M Yamauchi, M Takagishi, K Lamb, DQ Atteia, JL Vanderspek, R Graziani, C Prigozhin, G Villasenor, J Jernigan, JG Crew, GB Hurley, K Ricker, GR Woosley, SE Butler, N Levine, A Doty, JP Donaghy, TQ Fenimore, EE Galassi, M Boer, M Dezalay, JP Olive, JF Braga, J Manchanda, R Pizzichini, G Kawai, N TI HETE-2 localization and observations of the gamma-ray burst GRB 020813 SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN LA English DT Article DE gamma-rays : bursts ID MAGNETIC-FIELDS; ENERGY; MODEL; EMISSION; SHOCK; AFTERGLOW; PROMPT AB A bright, long gamma-ray burst (GRB) was detected and localized by the instruments on board the High Energy Transient Explorer 2 satellite (HETE-2) at 02:44:19.17 UTC (9859.17 s UT) on 2002 August 13. The location was reported to the GRB Coordinates Network (GCN) about 4 min after the burst. In the prompt emission, the burst had a duration of approximately 125 s, and more than four peaks. We analyzed the time-resolved 2-400 keV energy spectra of the prompt emission of GRB 020813 using the Wide Field X-Ray Monitor (WXM) and the French Gamma Telescope (FREGATE) in detail. We found that the early part of the burst (17-52 s after the burst trigger) shows a depletion of low-energy photons below about 50 keV. It is difficult to explain the depletion by either synchrotron self-absorption or Comptonization. One possibility is that the low-energy depletion may be understood as a mixture of "jitter" radiation with the usual synchrotron radiation component. C1 Tokyo Inst Technol, Dept Phys, Meguro Ku, Tokyo 1528551, Japan. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RIKEN, Wako, Saitama 3510198, Japan. Aoyama Gakuin Univ, Dept Phys, Sagamihara, Kanagawa 2298558, Japan. Natl Astron Observ, Mitaka, Tokyo 1818588, Japan. Osaka Univ, Grad Sch Sci, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan. JAXA, Tsukuba, Ibaraki 3048505, Japan. Miyazaki Univ, Fac Engn, Miyazaki, Miyazaki 8992192, Japan. Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA. Observ Midi Pyrenees, Astrophys Lab, F-31400 Toulouse, France. MIT, CSR, Cambridge, MA 02139 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. Observ Midi Pyrenees, Ctr Etud Spatiale Rayonnements, F-31028 Toulouse, France. Inst Nacl Pesquisas Espaciais, BR-12227010 Sao Jose Dos Campos, Brazil. Tata Inst Fundamental Res, Dept Astron & Astrophys, Bombay 400005, Maharashtra, India. INAF, IASF, Sez Bologna, I-40129 Bologna, Italy. RP Tokyo Inst Technol, Dept Phys, Meguro Ku, Tokyo 1528551, Japan. EM rsato@hp.phys.titech.ac.jp OI Boer, Michel/0000-0001-9157-4349 NR 27 TC 4 Z9 4 U1 0 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0004-6264 EI 2053-051X J9 PUBL ASTRON SOC JPN JI Publ. Astron. Soc. Jpn. PD DEC 25 PY 2005 VL 57 IS 6 BP 1031 EP 1039 DI 10.1093/pasj/57.6.1031 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 002JF UT WOS:000234607000016 ER PT J AU Crown, DA Bleamaster, LF Mest, SC AF Crown, DA Bleamaster, LF Mest, SC TI Styles and timing of volatile-driven activity in the eastern Hellas region of Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID GROUND ICE; MARGARITIFER SINUS; VOLCANIC GEOLOGY; MARTIAN VOLCANOS; IMPACT BASINS; FLOW FEATURES; DEBRIS APRONS; EVOLUTION; EROSION; SURFACE AB [1] Recent analyses of Mars Global Surveyor and Mars Odyssey data sets provide new insights into the geologic evolution of the eastern Hellas region of Mars, in particular, the role of volatiles. Here, we present results of our recent work and integrate these with previous studies by various investigators to provide a synthesis of the history of volatile-driven activity of the region. We utilize high-resolution images from the Mars Orbiter Camera and Thermal Emission Imaging System combined with Mars Orbiter Laser Altimeter digital elevation models and profiles to examine fluvial systems that dissect the circum-Hellas highlands, to characterize stages in the development of the Dao, Niger, Harmakhis, and Reull Valles canyon systems, and to evaluate evidence for ancient lakes in Hellas Planitia. The occurrence of valley networks, dissected highland crater rims, and crater interior deposits such as layered plateaus suggests widespread ancient degradation of the circum-Hellas highlands. Canyon development, which represents subsequent more localized activity, may have included an early fluvial phase followed by the collapse and sapping dominated stages that, along with recent wall erosion and floor resurfacing, produced the currently observed morphologies. The prominent role of collapse and sapping along the east rim of Hellas, along with the presence of numerous channels extending toward the basin and sequences of finely layered deposits along the basin rim, suggests a volatile-rich substrate across a broad depositional shelf. The east rim of the basin was an accumulation zone for atmospheric volatiles and/or the edge of volatile-rich deposits associated with the basin floor. This evidence combined with topographic data and cratered terrain preservation around the basin is consistent with a lacustrine period or periods in early Martian history. The style, magnitude, and spatial extent of volatile-driven activity in eastern Hellas have varied considerably with time, and these variations may represent a transition from a water-to an ice-dominated surface environment. C1 Planetary Sci Inst, Tucson, AZ 85719 USA. NASA, Goddard Space Flight Ctr, Planetary Geodynam Lab, Greenbelt, MD 20771 USA. RP Crown, DA (reprint author), Planetary Sci Inst, 1700 E Ft Lowell Rd,Suite 106, Tucson, AZ 85719 USA. EM crown@psi.edu NR 97 TC 27 Z9 27 U1 0 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD DEC 24 PY 2005 VL 110 IS E12 AR E12S22 DI 10.1029/2005JE002496 PG 19 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 999CR UT WOS:000234366800001 ER PT J AU Paton-Walsh, C Jones, NB Wilson, SR Haverd, V Meier, A Griffith, DWT Rinsland, CP AF Paton-Walsh, C Jones, NB Wilson, SR Haverd, V Meier, A Griffith, DWT Rinsland, CP TI Measurements of trace gas emissions from Australian forest fires and correlations with coincident measurements of aerosol optical depth SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID ATMOSPHERIC CHEMISTRY; NORTHERN; SAVANNAS; PLUME; SMOKE; C2H4 AB [1] We present vertically integrated measurements of C2H2, C2H4, C2H6, HCOOH, CO, H2CO, HCN and NH3 through smoke plumes from Australian forest fires measured by ground-based solar absorption spectroscopy. The column amounts of these gases are highly correlated with simultaneous, colocated measurements of aerosol optical depth, providing a potential method of mapping biomass-burning emissions using satellite measurements of aerosol optical depth. We have calculated emission ratios relative to CO for the trace gases using aerosol optical depth as a proxy for CO and converted to emission factors by using an average emission factor for CO from literature measurements of extratropical forest fires. The results show that Australian forest fire emissions are broadly similar to those from other geographical regions except for comparatively low emissions of C2H6. C1 Univ Wollongong, Dept Chem, Wollongong, NSW 2522, Australia. NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Univ Wollongong, Dept Chem, Wollongong, NSW 2522, Australia. EM njones@uow.edu.au RI Paton-Walsh, Clare/B-2774-2009; haverd, vanessa/G-8683-2011; Wilson, Stephen/B-8541-2008; Jones, Nicholas/G-5575-2011 OI Paton-Walsh, Clare/0000-0003-1156-4138; Wilson, Stephen/0000-0003-4546-2527; Jones, Nicholas/0000-0002-0111-2368 NR 21 TC 36 Z9 36 U1 0 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 23 PY 2005 VL 110 IS D24 AR D24305 DI 10.1029/2005JD006202 PG 6 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 999CB UT WOS:000234365200007 ER PT J AU Lasserre, C Peltzer, G Crampe, F Klinger, Y Van der Woerd, J Tapponnier, P AF Lasserre, C Peltzer, G Crampe, F Klinger, Y Van der Woerd, J Tapponnier, P TI Coseismic deformation of the 2001 M-w=7.8 Kokoxili earthquake in Tibet, measured by synthetic aperture radar interferometry SO JOURNAL OF GEOPHYSICAL RESEARCH-SOLID EARTH LA English DT Article ID 7.1 HECTOR MINE; KUNLUN FAULT; SLIP-RATE; LANDERS EARTHQUAKE; CHINA; TECTONICS; RUPTURE; CALIFORNIA; PLATEAU; ORIGIN AB [1] The 14 November 2001, M-w = 7.8, Kokoxili earthquake ruptured more than 400 km of the westernmost stretch of the left-lateral Kunlun fault in northern Tibet. Interferometric synthetic aperture radar data from descending orbits, along four adjacent tracks covering almost the entire rupture, and 1-m pixel Ikonos satellite images are used to map the rupture geometry and the surface displacements produced by the event. Interferograms are then inverted to solve for coseismic slip on the fault at depth. The radar data show that the rupture connected the Heituo fault, where the earthquake initiated, to the main Kunlun fault, cutting across a pull-apart trough in between the two strike-slip faults. The fault model includes two vertical sections extending to a depth of 20 km and discretized into 5 km x 5 km patches. Using a nonnegative least squares method that includes an appropriate degree of smoothing, we solve for the left-lateral slip on each fault patch. Our solution shows that the largest slip occurred at depths between 0 and 5 km, reaching similar or equal to 8 m in two areas, 200 and 250 km east of the earthquake epicenter. Significant slip took place below 10 km at both ends of the rupture. Slip appears to have been highly variable along the fault, defining six sections of major moment release. These sections correspond to six subsegments of the Kunlun fault system, defined from the surface morphology of the fault. This suggests that fault geometry exerted a predominant influence on controlling the rupture propagation. C1 Univ Calif Los Angeles, Dept Earth & Space Sci, Los Angeles, CA 90095 USA. CALTECH, Jet Prop Lab, Pasadena, CA USA. Inst Phys Globe Strasbourg, Lab Tecton & Mecan Lithospherre, Paris, France. CNRS, UMR 7516, Inst Phys Globe Strasbourg, Strasbourg, France. RP Lasserre, C (reprint author), Ecole Normale Super, CNRS, UMR 8538, Geol Lab, 24 Rue Lhomond, F-75231 Paris 05, France. EM lasserre@geologie.ens.fr; Peltzer@ess.ucla.edu; frederic.crampe@silogic.fr; klinger@ipgp.jussieu.fr; jerome.vanderwoerd@eost.u-strasbg.fr; tappon@ipgp.jussieu.fr RI klinger, yann/B-1226-2011; Tapponnier, .Paul/B-7033-2011; Lasserre, Cecile/D-7073-2017 OI Tapponnier, .Paul/0000-0002-7135-1962; Lasserre, Cecile/0000-0002-0582-0775 NR 49 TC 73 Z9 74 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9313 EI 2169-9356 J9 J GEOPHYS RES-SOL EA JI J. Geophys. Res.-Solid Earth PD DEC 23 PY 2005 VL 110 IS B12 AR B12408 DI 10.1029/2004JB003500 PG 22 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 999CZ UT WOS:000234367600001 ER PT J AU Hellinger, P Velli, M Travnicek, P Gary, SP Goldstein, BE Liewer, PC AF Hellinger, P Velli, M Travnicek, P Gary, SP Goldstein, BE Liewer, PC TI Alfven wave heating of heavy ions in the expanding solar wind: Hybrid simulations SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID ALFVEN/CYCLOTRON FLUCTUATIONS; VELOCITY DISTRIBUTIONS; CYCLOTRON WAVES; CORONAL HOLES; ACCELERATION; ANISOTROPY; DIFFUSION; RESONANCE; SPECTRA; PROTONS AB [1] We present hybrid expanding box simulations of the interaction of left-handed Alfven waves with protons, alpha particles, and a tenuous population of oxygen O5+. The Alfven waves are initially nonresonant with the ions, and the expansion brings them to the cyclotron resonance with O5+ ions, then with alpha particles, and finally with protons. The simulations show that O5+ ions are efficiently heated in the directions perpendicular to the background magnetic field but are only slightly accelerated. Oxygen scattering has a finite time span and saturates mainly due to the marginal stabilization with respect to the oxygen cyclotron instability generated by the temperature anisotropy. During the scattering, oxygen ions are able to absorb only a limited amount of available fluctuating energy and, for the parameters used in the simulations, their presence has a minimum influence on alpha particles and protons. C1 Acad Sci Czech Republic, Inst Atmospher Phys, Prague 14131, Czech Republic. Univ Florence, Dept Astron & Space Sci, I-50125 Florence, Italy. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Acad Sci Czech Republic, Inst Atmospher Phys, Prague 14131, Czech Republic. EM petr.hellinger@ufa.cas.cz; velli@arcetri.astro.it; trav@ufa.cas.cz; pgary@lanl.gov; bruce.goldstein@jpl.nasa.gov; paulett.liewer@jpl.nasa.gov RI Hellinger, Petr/F-5267-2014; Travnicek, Pavel/G-8608-2014 OI Hellinger, Petr/0000-0002-5608-0834; NR 27 TC 37 Z9 37 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 23 PY 2005 VL 110 IS A12 AR A12109 DI 10.1029/2005JA011244 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 999DJ UT WOS:000234368600002 ER PT J AU Picardi, G Plaut, JJ Biccari, D Bombaci, O Calabrese, D Cartacci, M Cicchetti, A Clifford, SM Edenhofer, P Farrell, WM Federico, C Frigeri, A Gurnett, DA Hagfors, T Heggy, E Herique, A Huff, RL Ivanov, AB Johnson, WTK Jordan, RL Kirchner, DL Kofman, W Leuschen, CJ Nielsen, E Orosei, R Pettinelli, E Phillips, RJ Plettemeier, D Safaeinili, A Seu, R Stofan, ER Vannaroni, G Watters, TR Zampolini, E AF Picardi, G Plaut, JJ Biccari, D Bombaci, O Calabrese, D Cartacci, M Cicchetti, A Clifford, SM Edenhofer, P Farrell, WM Federico, C Frigeri, A Gurnett, DA Hagfors, T Heggy, E Herique, A Huff, RL Ivanov, AB Johnson, WTK Jordan, RL Kirchner, DL Kofman, W Leuschen, CJ Nielsen, E Orosei, R Pettinelli, E Phillips, RJ Plettemeier, D Safaeinili, A Seu, R Stofan, ER Vannaroni, G Watters, TR Zampolini, E TI Radar soundings of the subsurface of Mars SO SCIENCE LA English DT Article ID GEOLOGIC HISTORY; EVOLUTION AB The martian subsurface has been probed to kilometer depths by the Mars Advanced Radar for Subsurface and Ionospheric Sounding instrument aboard the Mars Express orbiter. Signals penetrate the polar layered deposits, probably imaging the base of the deposits. Data from the northern lowlands of Chryse Planitia have revealed a shallowly buried quasi-circular structure about 250 kilometers in diameter that is interpreted to be an impact basin. In addition, a planar reflector associated with the basin structure may indicate the presence of a low-loss deposit that is more than 1 kilometer thick. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Roma La Sapienza, Infocom Dept, I-00184 Rome, Italy. Alcatel Alenia Space Italia, I-00131 Rome, Italy. Lunar & Planetary Inst, Houston, TX 77058 USA. Ruhr Univ Bochum, Fak Elektrotech & Informat Tech, D-44780 Bochum, Germany. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Perugia, Dipartimento Sci Terra, I-06123 Perugia, Italy. Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. Lab Planetol Grenoble, F-38041 Grenoble, France. Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. Ist Nazl Astrofis, Ist Astrofis Spaziale & Fis Cosm, I-00133 Rome, Italy. Ist Nazl Astrofis, Ist Fis Spazio Interplanetario, I-00133 Rome, Italy. Univ Rome 3, Dipartimento Fis, I-00146 Rome, Italy. Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. Tech Univ Dresden, Fak Elektrotech & Informat Tech, D-01062 Dresden, Germany. Proxemy Res, Laytonville, MD 20882 USA. Smithsonian Inst, Natl Air & Space Museum, Ctr Earth & Planetary Studies, Washington, DC 20560 USA. RP Plaut, JJ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM plaut@jpl.nasa.gov RI Kofman, Wlodek/C-4556-2008; Frigeri, Alessandro/F-2151-2010; Heggy, Essam/E-8250-2013; Farrell, William/I-4865-2013; Ivanov, Anton/C-8944-2014; Herique, Alain/E-7210-2017 OI Frigeri, Alessandro/0000-0002-9140-3977; Heggy, Essam/0000-0001-7476-2735; Ivanov, Anton/0000-0001-8376-8581; Herique, Alain/0000-0003-3699-883X NR 27 TC 159 Z9 166 U1 1 U2 20 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD DEC 23 PY 2005 VL 310 IS 5756 BP 1925 EP 1928 DI 10.1126/science.1122165 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 997UX UT WOS:000234275400034 PM 16319122 ER PT J AU Gurnett, DA Kirchner, DL Huff, RL Morgan, DD Persoon, AM Averkamp, TF Duru, F Nielsen, E Safaeinili, A Plalut, JJ Picardi, G AF Gurnett, DA Kirchner, DL Huff, RL Morgan, DD Persoon, AM Averkamp, TF Duru, F Nielsen, E Safaeinili, A Plalut, JJ Picardi, G TI Radar soundings of the ionosphere of Mars SO SCIENCE LA English DT Article ID MAGNETIC-FIELD; GLOBAL SURVEYOR; CRUSTAL MAGNETIZATION; TOPSIDE SOUNDERS; ABSORPTION AB We report the first radar soundings of the ionosphere of Mars with the MARSIS (Mars Advanced Radar for Subsurface and Ionosphere Sounding) instrument on board the orbiting Mars Express spacecraft. Several types of ionospheric echoes are observed, ranging from vertical echoes caused by specular reflection from the horizontally stratified ionosphere to a wide variety of oblique and diffuse echoes. The oblique echoes are believed to arise mainly from ionospheric structures associated with the complex crustal magnetic fields of Mars. Echoes at the electron plasma frequency and the cyclotron period also provide measurements of the local electron density and magnetic field strength. C1 Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Roma La Sapienza, Infocom Dept, I-00184 Rome, Italy. RP Gurnett, DA (reprint author), Univ Iowa, Dept Phys & Astron, Iowa City, IA 52242 USA. EM donald-gurnett@uiowa.edu NR 24 TC 130 Z9 135 U1 1 U2 7 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD DEC 23 PY 2005 VL 310 IS 5756 BP 1929 EP 1933 DI 10.1126/science.1121868 PG 5 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 997UX UT WOS:000234275400035 PM 16319123 ER PT J AU Kobayashi, S Tanelli, S Im, E AF Kobayashi, S Tanelli, S Im, E TI Second-order multiple-scattering theory associated with backscattering enhancement for a millimeter wavelength weather radar with a finite beam width SO RADIO SCIENCE LA English DT Article ID DISCRETE RANDOM-MEDIA; RADIATIVE-TRANSFER EQUATION; WEAK-LOCALIZATION; COHERENT BACKSCATTERING; DISORDERED MEDIA; POLARIZED-LIGHT; RAIN; ATTENUATION; REFLECTION; INCOHERENT AB [1] Effects of multiple scattering on reflectivity are studied for millimeter wavelength weather radars. A time-independent vector theory, including up to second-order scattering, is derived for a single layer of hydrometeors of a uniform density and a uniform diameter. In this theory, spherical waves with a Gaussian antenna pattern are used to calculate ladder and cross terms in the analytical scattering theory. The former terms represent the conventional multiple scattering, while the latter terms cause backscattering enhancement in both the copolarized and cross-polarized components. As the optical thickness of the hydrometeor layer increases, the differences from the conventional plane wave theory become more significant, and essentially, the reflectivity of multiple scattering depends on the ratio of mean free path to radar footprint radius. These results must be taken into account when analyzing radar reflectivity for use in remote sensing. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kobayashi, S (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 300-243, Pasadena, CA 91109 USA. EM satoru@radar-sci.jpl.nasa.gov NR 37 TC 19 Z9 19 U1 0 U2 3 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0048-6604 J9 RADIO SCI JI Radio Sci. PD DEC 22 PY 2005 VL 40 IS 6 AR RS6015 DI 10.1029/2004RS003219 PG 16 WC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications SC Astronomy & Astrophysics; Geochemistry & Geophysics; Meteorology & Atmospheric Sciences; Remote Sensing; Telecommunications GA 999DN UT WOS:000234369000001 ER PT J AU Nieto, MM Anderson, JD AF Nieto, MM Anderson, JD TI Using early data to illuminate the Pioneer anomaly SO CLASSICAL AND QUANTUM GRAVITY LA English DT Article ID LONG-RANGE ACCELERATION; ULYSSES DATA; PROSAIC EXPLANATION; DISTANT SPACECRAFT; JUPITER; GALILEO; WEAK; TRACKING; MATTER AB Analysis of the radio tracking data from the Pioneer 10/11 spacecraft at distances between about 20-70 AU from the Sun has consistently indicated the presence of an unmodelled, small, constant, Doppler blue shift drift of order 6 x 10(-9) Hz s(-1). After accounting for systematics, this drift can be interpreted as a constant acceleration of a(P) = (8.74 +/- 1.33) x 10(-8) cm s(-2) directed towards the Sun, or perhaps as a time acceleration of a(t) = (2.92 +/- 0.44) x 10(-18) s(-2). Although it is suspected that there is a systematic origin to this anomaly, none has been unambiguously demonstrated. We review the current status of the anomaly, and then point out how the analysis of early data, which was never analysed in detail, could allow a clearer understanding of the origin of the anomaly, be it a systematic or a manifestation of unsuspected physics. C1 Los Alamos Natl Lab, Theoret Div MSB285, Los Alamos, NM 87545 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Nieto, MM (reprint author), Los Alamos Natl Lab, Theoret Div MSB285, Los Alamos, NM 87545 USA. EM mmn@lanl.gov; john.d.anderson@jpl.nasa.gov NR 25 TC 33 Z9 33 U1 0 U2 3 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0264-9381 J9 CLASSICAL QUANT GRAV JI Class. Quantum Gravity PD DEC 21 PY 2005 VL 22 IS 24 BP 5343 EP 5354 DI 10.1088/0264-9381/22/24/008 PG 12 WC Astronomy & Astrophysics; Physics, Multidisciplinary; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 002QN UT WOS:000234626400008 ER PT J AU Gopalswamy, N Torsti, J AF Gopalswamy, N Torsti, J TI Introduction to special section on Solar Coronal Mass Ejections and Energetic Particles SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Editorial Material C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Turku, Dept Phys, SF-20500 Turku, Finland. Univ Turku, Vaisala Inst Space Phys & Astron, SF-20500 Turku, Finland. RP Gopalswamy, N (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI Gopalswamy, Nat/D-3659-2012 NR 0 TC 1 Z9 1 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 21 PY 2005 VL 110 IS A12 AR A12S00 DI 10.1029/2005JA011523 PG 1 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 999DG UT WOS:000234368300001 ER PT J AU Lyapustin, AI AF Lyapustin, AI TI Radiative transfer code SHARM for atmospheric and terrestrial applications SO APPLIED OPTICS LA English DT Article ID DISCRETE-ORDINATE-METHOD; SCATTERING; SURFACE; APPROXIMATION; REFLECTANCE; ALGORITHMS; THICK; MODIS; WATER; LAND AB An overview of the publicly available radiative transfer Spherical Harmonies code (SHARM) is presented. SHARM is a rigorous code, as accurate as the Discrete Ordinate Radiative Transfer (DISORT) code, yet faster. It performs simultaneous calculations for different solar zenith angles, view zenith angles, and view azimuths and allows the user to make multiwavelength calculations in one run. The Delta-M method is implemented for calculations with highly anisotropic: phase functions. Rayleigh scattering is automatically included as a function of wavelength, surface elevation, and the selected vertical profile of one of the standard atmospheric models. The current version of the SHARM code does not explicitly include atmospheric gaseous absorption, which should be provided by the user. The SHARM code has several built-in models of the bidirectional reflectance of land and wind-ruffled water surfaces that are most widely used in research and satellite data processing. A modification of the SHARM code with the built-in Mie algorithm designed for calculations with spherical aerosols is also described. (c) 2005 Optical Society of America. C1 Univ Maryland Baltimore Cty, Goddard Earth Sci Technol Ctr, Greenbelt, MD 20771 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Univ Maryland Baltimore Cty, Goddard Earth Sci Technol Ctr, Code 614-4, Greenbelt, MD 20771 USA. EM alyapust@pop900.gsfc.nasa.gov RI Lyapustin, Alexei/H-9924-2014 OI Lyapustin, Alexei/0000-0003-1105-5739 NR 33 TC 33 Z9 33 U1 0 U2 0 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 DEC 20 PY 2005 VL 44 IS 36 BP 7764 EP 7772 DI 10.1364/AO.44.007764 PG 9 WC Optics SC Optics GA 995CT UT WOS:000234078200012 PM 16381525 ER PT J AU Bielewicz, P Eriksen, HK Banday, AJ Gorski, KM Lilje, PB AF Bielewicz, P Eriksen, HK Banday, AJ Gorski, KM Lilje, PB TI Multipole vector anomalies in the first-year WMAP data: A cut-sky analysis SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmic microwave background; cosmology : observations; methods : numerical ID MICROWAVE-ANISOTROPY-PROBE; PRIMORDIAL INHOMOGENEITY; COSMOLOGICAL PARAMETERS; NON-GAUSSIANITY; POWER SPECTRUM; MAPS; EMISSION; SPHERE AB We apply the recently defined multipole vector framework to the frequency-specific first-year WMAP sky maps, estimating the low-l multipole coefficients from the high-latitude sky by means of a power equalization filter. While most previous analyses of this type have considered only heavily processed (and foreground-contaminated) full-sky maps, the present approach allows for greater control of residual foregrounds and therefore potentially also for cosmologically important conclusions. The low-l spherical harmonic coefficients and corresponding multipole vectors are tabulated for easy reference. Using this formalism, we reassess a set of earlier claims of both cosmological and noncosmological low-l correlations on the basis of multipole vectors. First, we show that the apparent l 3 and 8 correlation claimed by Copi and coworkers is present only in the heavily processed map produced by Tegmark and coworkers and must therefore be considered an artifact of that map. Second, the well-known quadrupole-octopole correlation is confirmed at the 99% significance level and shown to be robust with respect to frequency and sky cut. Previous claims are thus supported by our analysis. Finally, the low-l alignment with respect to the ecliptic claimed by Schwarz and coworkers is nominally confirmed in this analysis, but also shown to be very dependent on severe a posteriori choices. Indeed, we show that given the peculiar quadrupole-octopole arrangement, finding such a strong alignment with the ecliptic is not unusual. C1 Warsaw Univ, Inst Theoret Phys, PL-00681 Warsaw, Poland. Univ Oslo, Inst Theoret Astrophys, N-0315 Oslo, Norway. Max Planck Inst Astrophys, D-85741 Garching, Germany. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Warsaw Observ, PL-00478 Warsaw, Poland. RP Bielewicz, P (reprint author), Warsaw Univ, Inst Theoret Phys, Ul Hoza 69, PL-00681 Warsaw, Poland. EM pawel.bielewicz@fuw.edu.pl; h.k.k.eriksen@astro.uio.no; banday@mpa-garching.mpg.de; krzysztof.m.gorski@jpl.nasa.gov; per.lilje@astro.uio.no RI Lilje, Per/A-2699-2012; OI Lilje, Per/0000-0003-4324-7794 NR 30 TC 64 Z9 64 U1 0 U2 1 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 DEC 20 PY 2005 VL 635 IS 2 BP 750 EP 760 DI 10.1086/497263 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996NZ UT WOS:000234182100002 ER PT J AU Dwek, E Arendt, RG Krennrich, F AF Dwek, E Arendt, RG Krennrich, F TI The near-infrared background: Interplanetary dust or primordial stars? SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : theory; diffuse radiation; early universe; galaxies : formation; infrared : general; stars : formation ID SPITZER-SPACE-TELESCOPE; PROBE WMAP OBSERVATIONS; POPULATION-III STARS; DIGITAL SKY SURVEY; ENERGY GAMMA-RAYS; COBE DIRBE MAPS; 1ST STARS; EXPERIMENT SEARCH; SOURCE COUNTS; PKS 2155-304 AB The intensity of the diffuse similar to 1-4 mu m sky emission from which solar system and Galactic foregrounds have been subtracted is in excess of that expected from energy released by galaxies and stars that formed during the z less than or similar to 5 redshift interval. The spectral signature of this excess near-infrared background light (NIRBL) component is almost identical to that of reflected sunlight from the interplanetary dust cloud and could therefore be the result of the incomplete subtraction of this foreground emission component from the diffuse sky maps. Alternatively, this emission component could be extragalactic. Its spectral signature is consistent with that of redshifted continuum and recombination line emission from H II regions formed by the first generation of very massive stars. In this paper we analyze the implications of this spectral component for the formation rate of these Population III stars, the redshift interval during which they formed, the reionization of the universe, and evolution of collapsed halo masses. Assuming that these Population III stars are massive objects radiating at the Eddington luminosity and ending their lives by directly collapsing into black holes, we find that to reproduce the intensity and spectral shape of the NIRBL requires a peak star formation rate of similar to 2.5M(circle dot) yr(-1) Mpc(-3), with a (1 + z)(-2) dependence on redshift, until the epoch ends at redshifts z approximate to 7-9. It requires a comoving luminosity density of about 2.7 x 10(11) L-circle dot Mpc(-3), corresponding to a total energy input of 670-820 keV per baryon, and that about 10% of the total number of baryons in the universe be converted to Population III stars. All these numbers are higher by about a factor of 4-10 than those derived from models in which Population III stars form at a rate that is proportional to the collapse rate of halos in a cold dark matter dominated universe. Furthermore, an extragalactic origin for the NIRBL leads to physically unrealistic absorption-corrected spectra of distant TeV blazars. All these results suggest that Population III stars contribute only a fraction of the NIRBL intensity, with zodiacal light, star-forming galaxies, and/or nonnuclear sources giving rise to the remaining fraction. Further 0.1-10 mu m observations of the diffuse sky and the zodiacal cloud are therefore crucial for resolving the true spectrum and origin of the NIRBL. C1 NASA, Goddard Space Flight Ctr, Observ Cosmol Lab, Sci Syst & Applicat Inc, Greenbelt, MD 20771 USA. Iowa State Univ, Dept Phys & Astron, Ames, IA 50011 USA. RP NASA, Goddard Space Flight Ctr, Observ Cosmol Lab, Sci Syst & Applicat Inc, Code 665, Greenbelt, MD 20771 USA. EM eli.dwek@nasa.gov; arendt@milkyway.gsfc.nasa.gov; krennich@iastate.edu OI Arendt, Richard/0000-0001-8403-8548 NR 58 TC 61 Z9 61 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2005 VL 635 IS 2 BP 784 EP 794 DI 10.1086/497569 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996NZ UT WOS:000234182100004 ER PT J AU Mobasher, B Dickinson, M Ferguson, HC Giavalisco, M Wiklind, T Stark, D Ellis, RS Fall, SM Grogin, NA Moustakas, LA Panagia, N Sosey, M Stiavelli, M Bergeron, E Casertano, S Ingraham, P Koekemoer, A Labbe, I Livio, M Rodgers, B Scarlata, C Vernet, J Renzini, A Rosati, P Kuntschner, H Kummel, M Walsh, JR Chary, R Eisenhardt, P Pirzkal, N Stern, D AF Mobasher, B Dickinson, M Ferguson, HC Giavalisco, M Wiklind, T Stark, D Ellis, RS Fall, SM Grogin, NA Moustakas, LA Panagia, N Sosey, M Stiavelli, M Bergeron, E Casertano, S Ingraham, P Koekemoer, A Labbe, I Livio, M Rodgers, B Scarlata, C Vernet, J Renzini, A Rosati, P Kuntschner, H Kummel, M Walsh, JR Chary, R Eisenhardt, P Pirzkal, N Stern, D TI Evidence for a massive poststarburst galaxy at z similar to 6.5 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; galaxies : formation; galaxies : high-redshift; galaxies : photometry ID ULTRA-DEEP-FIELD; HIGH-REDSHIFT GALAXIES; LYMAN-BREAK GALAXIES; STAR-FORMING GALAXIES; RED GALAXIES; STELLAR POPULATIONS; DATA REDUCTION; X-RAY; HUBBLE; EVOLUTION AB We describe results from a search for high-redshift J-band "dropout'' galaxies in the portion of the Great Observatories Origins Deep Survey (GOODS) southern field that is covered by extremely deep imaging from the Hubble Ultradeep Field (HUDF). Using observations at optical, near-infrared, and mid-infrared wavelengths from the Hubble and Spitzer Space Telescopes and the European Southern Observatory Very Large Telescope, we find one particularly remarkable candidate, which we designate HUDF-JD2. Its spectral energy distribution has distinctive features that are consistent with those of a galaxy at z similar to 6.5, observed several hundred million years after a powerful burst of star formation that produced a stellar mass of 6 x 10(11) M-circle dot (for a Salpeter IMF). We interpret a prominent photometric break between the near-infrared and Spitzer bandpasses as the 3646 angstrom Balmer discontinuity. The best-fitting models have low reddening and ages of several hundred Myr, placing the formation of the bulk of the stars at z > 9. Alternative models of dusty galaxies at z approximate to 2.5 are possible, but provide significantly poorer fits to the photometric data. The object is detected with Spitzer at 24 mu m. We consider interpretations of the 24 mu m emission as originating either from an obscured active nucleus or from star formation and find that the 24 mu m detection does not help to uniquely discriminate between the z = 6.5 and 2.5 alternatives. We present optical and near-infrared spectroscopy that has, thus far, failed to detect any spectral features. This nondetection helps limit the solution in which the galaxy is a starburst or active galaxy at z approximate to 2.5, but does not rule it out. If the high-redshift interpretation is correct, HUDF-JD2 is an example of a galaxy that formed by a process strongly resembling traditional models of monolithic collapse, in which a very large mass of stars formed within a remarkably short period of time, at very high redshift. C1 Space Telescope Sci Inst, Baltimore, MD 21218 USA. European Space Agcy, Dept Space Sci, F-75738 Paris 15, France. Natl Opt Astron Observ, Tucson, AZ 85726 USA. CALTECH, Dept Astron, Pasadena, CA 91125 USA. Johns Hopkins Univ, Baltimore, MD 21218 USA. Gemini Observ, La Serena, Chile. Observ Carnegie Inst Washington, Pasadena, CA 91101 USA. ETH, Inst Astron, CH-8099 Zurich, Switzerland. European So Observ, Space Telescope European Coordinating Facil, D-85748 Garching, Germany. Osserv Astron Padova, INAF, I-35122 Padua, Italy. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA. EM b.mobasher@stsci.edu OI Moustakas, Leonidas/0000-0003-3030-2360; Koekemoer, Anton/0000-0002-6610-2048 NR 58 TC 115 Z9 115 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2005 VL 635 IS 2 BP 832 EP 844 DI 10.1086/497626 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996NZ UT WOS:000234182100009 ER PT J AU Maloney, PR Glenn, J Aguirre, JE Golwala, SR Laurent, GT Ade, PAR Bock, JJ Edgington, SF Goldin, A Haig, D Lange, AE Mauskopf, PD Nguyen, H Rossinot, P Sayers, J Stover, P AF Maloney, PR Glenn, J Aguirre, JE Golwala, SR Laurent, GT Ade, PAR Bock, JJ Edgington, SF Goldin, A Haig, D Lange, AE Mauskopf, PD Nguyen, H Rossinot, P Sayers, J Stover, P TI A fluctuation analysis of the Bolocam 1.1 mm Lockman Hole Survey SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : high-redshift; galaxies : starburst; submillimeter ID NUMBER COUNTS; GALAXY EVOLUTION; CONFUSION; MAPS; ANISOTROPY AB We perform a fluctuation analysis of the 1.1 mm Bolocam Lockman Hole Survey, which covers 324 arcmin(2) to a very uniform point-source-filtered rms noise level of sigma similar or equal to 1.4 mJy beam(-1). The fluctuation analysis has the significant advantage of using all of the available data, since no extraction of sources is performed: direct comparison is made between the observed pixel flux density distribution [P( D)] and the theoretical distributions for a broad range of power-law number count models, n(S) = n(0)S(-delta). We constrain the number counts in the 1 - 10 mJy range and derive significantly tighter constraints than in previous work: the power-law index delta = 2.7(-0.15)(+0.18), while the amplitude is n(0) 1595(-238)(+85) mJy(-1) deg(-2), or N(> 1 mJy) 940(-140)(+50) deg(-2) (95% confidence). At flux densities above 4 mJy, where a valid comparison can be made, our results agree extremely well with those derived from the extracted source number counts by Laurent et al.: the best-fitting differential slope is somewhat shallower (delta = 2.7 vs. 3.2), but well within the 68% confidence limit, and the amplitudes ( number of sources per square degree) agree to 10%. At 1 mJy, however [the limit of the P(D) analysis], the shallower slope derived here implies a substantially smaller amplitude for the integral number counts than extrapolation from above 4 mJy would predict. Our derived normalization is about 2.5 times smaller than that determined by the Max-Planck Millimeter Bolometer (MAMBO) at 1.2 mm ( Greve et al.). However, the uncertainty in the normalization for both data sets is dominated by the systematic (i.e., absolute flux calibration) rather than statistical errors; within these uncertainties, our results are in agreement. Our best-fit amplitude at 1 mJy is also about a factor of 3 below the prediction of Blain et al., but we are in agreement above a few millijanskys. We estimate that about 7% of the 1.1 mm background has been resolved at 1 mJy. C1 Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. Univ Colorado, Dept Astrophys & Planetary Sci, Boulder, CO 80309 USA. CALTECH, Pasadena, CA 91125 USA. Univ Cardiff Wales, Cardiff CF24 3YB, Wales. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Maloney, PR (reprint author), Univ Colorado, Ctr Astrophys & Space Astron, Boulder, CO 80309 USA. EM maloney@casa.colorado.edu NR 23 TC 20 Z9 20 U1 0 U2 1 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 DEC 20 PY 2005 VL 635 IS 2 BP 1044 EP 1052 DI 10.1086/497585 PN 1 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996NZ UT WOS:000234182100025 ER PT J AU Still, M Roming, PWA Mason, KO Blustin, A Boyd, P Breeveld, A Brown, P De Pasquale, M Gronwall, C Holland, ST Hunsberger, S Ivanushkina, M James, C Landsman, W McGowan, K Morgan, A Poole, T Rosen, S Schady, P Zhang, B Krimm, H Sakamoto, T Giommi, P Goad, MR Mangano, V Page, K Perri, M Burrows, DN Gehrels, N Nousek, J AF Still, M Roming, PWA Mason, KO Blustin, A Boyd, P Breeveld, A Brown, P De Pasquale, M Gronwall, C Holland, ST Hunsberger, S Ivanushkina, M James, C Landsman, W McGowan, K Morgan, A Poole, T Rosen, S Schady, P Zhang, B Krimm, H Sakamoto, T Giommi, P Goad, MR Mangano, V Page, K Perri, M Burrows, DN Gehrels, N Nousek, J TI Swift UVOT detection of GRB 050318 SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrometry; galaxies : distances and redshifts; gamma rays : bursts; shock waves; X-rays : individual (GRB 050318) ID GAMMA-RAY BURSTS; MILKY-WAY; H-I; DUST; EXTINCTION; REDSHIFTS AB We present observations of GRB 050318 by the Ultraviolet/Optical Telescope (UVOT) on board the Swift observatory. The data are the first detections of a gamma-ray burst (GRB) afterglow decay by the UVOT instrument, launched specifically to open a new window on these transient sources. We showcase UVOT's ability to provide multicolor photometry and the advantages of combining UVOT data with simultaneous and contemporaneous observations from the high-energy detectors on the Swift spacecraft. Multiple filters covering 1800-6000 angstrom reveal a red source with a spectral slope steeper than the simultaneous X-ray continuum. Spectral fits indicate that the UVOT colors are consistent with dust extinction by systems at z = 1.2037 and 1.4436, redshifts where absorption systems have been preidentified. However, the data can be most easily reproduced with models containing a foreground system of neutral gas redshifted by z = 2.8 +/- 0.3. For both of the above scenarios, spectral and decay slopes are, for the most part, consistent with fireball expansion into a uniform medium, provided a cooling break occurs between the energy ranges of the UVOT and Swift's X-ray instrumentation. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Space Res Assoc, Columbia, MD USA. Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. UCL, Mullard Space Sci Lab, Dorking RH5 6NT, Surrey, England. Univ Maryland, Joint Ctr Astrophys, Baltimore, MD 21250 USA. Brigham Young Univ, Dept Phys & Astron, Provo, UT 84602 USA. Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. ESRIN, ASI Sci Data Ctr, I-00044 Frascati, Italy. Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. Osserv Astron Roma, Sede Monteporzio Catone, I-00040 Rome, Italy. RP NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RI Boyd, Patricia/D-3274-2012; Gehrels, Neil/D-2971-2012; OI giommi, paolo/0000-0002-2265-5003; Perri, Matteo/0000-0003-3613-4409 NR 29 TC 21 Z9 21 U1 0 U2 5 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2005 VL 635 IS 2 BP 1187 EP 1191 DI 10.1086/497627 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996NZ UT WOS:000234182100039 ER PT J AU Brown, PJ Holland, ST James, C Milne, P Roming, PWA Mason, KO Page, KL Beardmore, AP Burrows, D Morgan, A Gronwall, C Blustin, AJ Boyd, P Still, M Breeveld, A de Pasquale, M Hunsberger, S Ivanushkina, M Landsman, W McGowan, K Poole, T Rosen, S Schady, P Gehrels, N AF Brown, PJ Holland, ST James, C Milne, P Roming, PWA Mason, KO Page, KL Beardmore, AP Burrows, D Morgan, A Gronwall, C Blustin, AJ Boyd, P Still, M Breeveld, A de Pasquale, M Hunsberger, S Ivanushkina, M Landsman, W McGowan, K Poole, T Rosen, S Schady, P Gehrels, N TI Ultraviolet, optical, and X-ray observations of the type Ia supernova 2005am with Swift SO ASTROPHYSICAL JOURNAL LA English DT Article DE supernovae : individual (SN 2005am) ID LIGHT CURVES; UNIVERSE; IUE AB We present ultraviolet and optical light curves in six broadband filters and grism spectra obtained by Swift's Ultraviolet/Optical Telescope for the Type Ia supernova SN 2005am. The data were collected beginning about 4 days before the B-band maximum, with excellent coverage of the rapid decline phase and later observations extending out to 69 days after the peak. The optical and near-UV light curve match well those of SN 1992A. The other UV observations constitute the first set of light curves shorter than 2500 angstrom and allow us to compare the light curve evolution in three UV bands. One interesting feature is that the decay in the intermediate UVM2 band is shallower than in the filters on either side and may result from the bump in the interstellar extinction curve. The UV behavior of this and other low-redshift supernovae can be used to constrain theories of progenitor evolution or to interpret optical light curves of high-redshift supernovae. Using Swift's X-Ray Telescope, we also report the upper limit to SN 2005am's X-ray luminosity to be 6 x 10(39) ergs s(-1) in the 0.3 - 10 keV. This result is derived from 58 ks of exposure time spread out over 7 weeks beginning 4 days before the B-band maximum. C1 Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. Univ Space Res Assoc, Columbia, MD USA. UCL, Mullard Space Sci Lab, Dept Space & Climate Phys, Dorking RH5 6NT, Surrey, England. Steward Observ, Tucson, AZ 85721 USA. Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. RP Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. EM pbrown@astro.psu.edu RI Boyd, Patricia/D-3274-2012; Gehrels, Neil/D-2971-2012 NR 23 TC 23 Z9 23 U1 0 U2 4 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2005 VL 635 IS 2 BP 1192 EP 1196 DI 10.1086/497437 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996NZ UT WOS:000234182100040 ER PT J AU Barthelmy, SD Cannizzo, JK Gehrels, N Cusumano, G Mangano, V O'Brien, PT Vaughan, S Zhang, B Burrows, DN Campana, S Chincarini, G Goad, MR Kouveliotou, C Kumar, P Meszaros, P Nousek, JA Osborne, JP Panaitescu, A Reeves, JN Sakamoto, T Tagliaferri, G Wijers, RAMJ AF Barthelmy, SD Cannizzo, JK Gehrels, N Cusumano, G Mangano, V O'Brien, PT Vaughan, S Zhang, B Burrows, DN Campana, S Chincarini, G Goad, MR Kouveliotou, C Kumar, P Meszaros, P Nousek, JA Osborne, JP Panaitescu, A Reeves, JN Sakamoto, T Tagliaferri, G Wijers, RAMJ TI Discovery of an afterglow extension of the prompt phase of two gamma-ray bursts observed by Swift SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : bursts; X-rays : individual (GRB 050315, GRB 050319) ID EMISSION; BATSE AB BAT and XRT observations of two recent well-covered GRBs observed by Swift, GRB 050315 and GRB 050319, clearly show a prompt component joining the onset of the afterglow emission. By fitting a power-law form to the gamma-ray spectrum, we extrapolate the time-dependent fluxes measured by BAT, in the energy band 15 350 keV, into the spectral regime observed by XRT, 0.2-10 keV, and examine the functional form of the rate of decay of the two light curves. We find that the BAT and XRT light curves merge to form a unified curve. There is a period of steep decay up to similar to 300 s, followed by a flatter decay. The duration of the steep decay, similar to 100 s in the source frame after correcting for cosmological time dilation, agrees roughly with a theoretical estimate for the deceleration time of the relativistic ejecta as it interacts with circumstellar material. For GRB 050315, the steep decay can be characterized by an exponential form, where the e-folding decay time s ( BAT), tau(e) similar or equal to 24 +/- 2 s e and s ( XRT). For GRB 050319, a power-law decay, -d 1n f/d 1n t = n where n similar or equal to 3 provides a tau(e) similar or equal to 35 +/- 2 e reasonable fit. The early-time X-ray fluxes are consistent with representing the lower energy tail of the prompt emission and provide our first quantitative measure of the decay of the prompt gamma-ray emission over a large dynamic range in flux. The initial steep decay is expected, due to the delayed high-latitude photons from a curved shell of relativistic plasma illuminated only for a short interval. The overall conclusion is that the prompt phase of GRBs remains observable for hundreds of seconds longer than previously thought. C1 NASA, Goddard Space Flight Ctr, Explorat Universe Div, Greenbelt, MD 20771 USA. Univ Maryland Baltimore Cty, Joint Ctr Astrophys, Baltimore, MD 21250 USA. Ist Astrofis Spaziale & Cosm, INAF, I-90146 Palermo, Italy. Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. Penn State Univ, Dept Phys, Dept Astron & Astrophys, University Pk, PA 16802 USA. Osserv Astron Brera, INAF, I-23807 Merate, Italy. Univ Milano Bicocca, Dipartimento Fis, I-20126 Milan, Italy. NASA, George C Marshall Space Flight Ctr, NSSTC, Huntsville, AL 35805 USA. Univ Texas, Dept Astron, Austin, TX 78712 USA. Los Alamos Natl Lab, Los Alamos, NM 87545 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. Univ Space Res Assoc, Columbia, MD 21044 USA. CNR, Washington, DC 20418 USA. Univ Amsterdam, Astron Inst Anton Pannekoek, Amsterdam, Netherlands. RP Barthelmy, SD (reprint author), NASA, Goddard Space Flight Ctr, Explorat Universe Div, Greenbelt, MD 20771 USA. RI Gehrels, Neil/D-2971-2012; Barthelmy, Scott/D-2943-2012; OI Cusumano, Giancarlo/0000-0002-8151-1990; Tagliaferri, Gianpiero/0000-0003-0121-0723; Campana, Sergio/0000-0001-6278-1576; Wijers, Ralph/0000-0002-3101-1808 NR 30 TC 56 Z9 57 U1 0 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 DEC 20 PY 2005 VL 635 IS 2 BP L133 EP L136 DI 10.1086/499432 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996OC UT WOS:000234182500006 ER PT J AU Bemporad, A Sterling, AC Moore, RL Poletto, G AF Bemporad, A Sterling, AC Moore, RL Poletto, G TI A new variety of coronal mass ejection: Streamer puffs from compact ejective flares SO ASTROPHYSICAL JOURNAL LA English DT Article DE sun : coronal mass ejections (CMEs); sun : magnetic fields; sun : UV radiation ID TRANSITION REGION; SOLAR; LASCO; EIT AB We report on SOHO UVCS, LASCO, EIT, and MDI observations of a series of narrow ejections that occurred at the solar limb. These ejections originated from homologous compact flares whose source was an island of included polarity located just inside the base of a coronal streamer. Some of these ejections result in narrow CMEs ("streamer puffs") that move out along the streamer. These streamer puffs differ from "streamer blowout" CMEs in that ( 1) while the streamer is transiently inflated by the puff, it is not disrupted, and ( 2) each puff comes from a compact explosion in the outskirts of the streamer arcade, not from an extensive eruption along the main neutral line of the streamer arcade. From the observations, we infer that each streamer puff is produced by means of the inflation or blowing open of an outer loop of the arcade by ejecta from the compact-flare explosion in the foot of the loop. So, in terms of their production, our streamer puffs are a new variety of CME. C1 Univ Florence, Dipartimento Astron & Sci Spazio, I-50125 Florence, Italy. NASA, George C Marshall Space Flight Ctr, Space Sci Branch, Huntsville, AL 35805 USA. Osserv Astrofis Arcetri, INAF, I-50125 Florence, Italy. RP Bemporad, A (reprint author), Univ Florence, Dipartimento Astron & Sci Spazio, Largo Enrico Fermi 2, I-50125 Florence, Italy. OI Bemporad, Alessandro/0000-0001-5796-5653 NR 14 TC 37 Z9 38 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 DEC 20 PY 2005 VL 635 IS 2 BP L189 EP L192 DI 10.1086/499625 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996OC UT WOS:000234182500020 ER PT J AU Liang, MC Shia, RL Lee, AYT Allen, M Friedson, AJ Yung, YL AF Liang, MC Shia, RL Lee, AYT Allen, M Friedson, AJ Yung, YL TI Meridional transport in the stratosphere of Jupiter SO ASTROPHYSICAL JOURNAL LA English DT Article DE atmospheric effects; methods : numerical; planetary systems; planets and satellites : individual (Jupiter); radiative transfer ID PHOTOCHEMISTRY; CIRCULATION; ATMOSPHERE; CHEMISTRY; IMPACTS; HCN AB The Cassini measurements of C2H2 and C2H6 at similar to 5 mbar provide a constraint on meridional transport in the stratosphere of Jupiter. We performed a two-dimensional photochemical calculation coupled with mass transport due to vertical and meridional mixing. The modeled profile of C2H2 at latitudes less than 70 degrees follows the latitude dependence of the solar insolation, while that of C2H6 shows little latitude dependence, consistent with the measurements. In general, our model study suggests that the meridional transport timescale above 5-10 mbar altitude level is >= 1000 yr, and the time could be as short as 10 yr below 10 mbar level, in order to fit the Cassini measurements. The derived meridional transport timescale above the 5 mbar level is 100 times longer than that obtained from the spreading of gas-phase molecules deposited after the impact of Shoemaker-Levy 9 comet. There is no explanation at this time for this discrepancy. C1 CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Liang, MC (reprint author), CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. EM mcl@gps.caltech.edu NR 16 TC 15 Z9 15 U1 1 U2 7 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 20 PY 2005 VL 635 IS 2 BP L177 EP L180 DI 10.1086/499624 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996OC UT WOS:000234182500017 ER PT J AU Reach, WT Kuchner, MJ von Hippel, T Burrows, A Mullally, F Kilic, M Winget, DE AF Reach, WT Kuchner, MJ von Hippel, T Burrows, A Mullally, F Kilic, M Winget, DE TI The dust cloud around the white dwarf G29-38 SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : stars; stars : individual (G29-38, WD 2326+049); white dwarfs ID SPITZER-SPACE-TELESCOPE; INFRARED ARRAY CAMERA; BROWN DWARF; SPECTRUM; STARS; METALS; EXCESS; CALIBRATION; CATALOG; ORIGIN AB We present new observations of the white dwarf G29-38 with the camera (4.5 and 8 mu m), photometer (24 mm), and spectrograph (5.5-14 mm) of the Spitzer Space Telescope. This star has an exceptionally large infrared excess, amounting to 3% of the bolometric luminosity. The spectral energy distribution (SED) has a continuum peak around 4.5 mm and a 9-11 mu m emission feature 1.25 times brighter than the continuum. A mixture of amorphous olivine and a small amount of forsterite in an emitting region 1-5R(circle dot) from the star can reproduce the shape of the 9-11 mu m R, feature. The SED also appears to require amorphous carbon to explain the hot continuum. Our new measurements support the idea that a relatively recent disruption of a comet or asteroid created the cloud. C1 CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Texas, Dept Astron, Austin, TX 78712 USA. Univ Arizona, Dept Astron, Tucson, AZ 85721 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. RP Reach, WT (reprint author), CALTECH, Spitzer Sci Ctr, MS 220-6, Pasadena, CA 91125 USA. EM reach@ipac.caltech.edu RI Reach, William/C-4710-2008; Kuchner, Marc/E-2288-2012; OI Reach, William/0000-0001-8362-4094 NR 35 TC 113 Z9 113 U1 0 U2 2 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 DEC 20 PY 2005 VL 635 IS 2 BP L161 EP L164 DI 10.1086/499561 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 996OC UT WOS:000234182500013 ER PT J AU Yu, J Gloersen, P AF Yu, J Gloersen, P TI Interannual variations in global SST deviations through SMMR from 1978 to 1987 SO INTERNATIONAL JOURNAL OF REMOTE SENSING LA English DT Article ID ANTARCTIC CIRCUMPOLAR WAVE; OCEAN-ATMOSPHERE SYSTEM; CLIMATE VARIABILITY; TROPOSPHERIC RESPONSE; NORTH PACIFIC; TEMPERATURE; ANOMALIES; MODES; WIND AB We study variability of global sea surface temperature (SST) utilizing the data of scanning multichannel microwave radiometer (SMMR) on board the NASA Nimbus 7 satellite from 1978 to 1987. First, we model, and then remove from the SMMR SST data, the seasonal cycle by using an intercept, a trend and first five harmonics of the annual cycle to fit the data at each grid point by the method of least squares. A general negative nine-year trend was observed. In order to analyse the deviations in the global SSTs, we calculate and remove zonally averaged temperatures. We then show Hoffmueller diagrams for the deviations along paths in different oceanic regions over the globe. These paths include a quadrangle in the south Pacific and paths in the north Pacific, Atlantic and along the equatorial Pacific. Both 1983 and 1987 El Nino events as well as the 1984-85 La Nina event are clearly depicted. During these events, the SSTs in the equatorial Pacific and Atlantic are completely out of phase. We also demonstrate spatial propagation of SST waves over interannual scales. In particular, a wave of a period of about 3-4 years following the North Pacific Current will be shown. C1 Univ Vermont, Burlington, VT 05401 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Yu, J (reprint author), Univ Vermont, Burlington, VT 05401 USA. EM Jun.Yu@uvm.edu NR 30 TC 0 Z9 0 U1 1 U2 4 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0143-1161 J9 INT J REMOTE SENS JI Int. J. Remote Sens. PD DEC 20 PY 2005 VL 26 IS 24 BP 5419 EP 5431 DI 10.1080/01431160500285688 PG 13 WC Remote Sensing; Imaging Science & Photographic Technology SC Remote Sensing; Imaging Science & Photographic Technology GA 003AK UT WOS:000234653800004 ER PT J AU Chen, X Vierling, L Deering, D Conley, A AF Chen, X Vierling, L Deering, D Conley, A TI Monitoring boreal forest leaf area index across a Siberian burn chronosequence: a MODIS validation study SO INTERNATIONAL JOURNAL OF REMOTE SENSING LA English DT Article ID SPECTRAL VEGETATION INDEXES; ATMOSPHERIC CORRECTION; SATELLITE DATA; LAND-COVER; TM IMAGES; EOS-MODIS; ETM PLUS; LAI; ECOSYSTEM; SITES AB Landscapes containing differing amounts of ecological disturbance provide an excellent opportunity to validate and better understand the emerging Moderate Resolution Imaging Spectrometer (MODIS) vegetation products. Four sites, including 1-year post-fire coniferous, 13-year post-fire deciduous, 24-year post-fire deciduous, and > 100 year old post-fire coniferous forests, were selected to serve as a post-fire chronosequence in the central Siberian region of Krasnoyarsk (57.3 degrees N, 91.6 degrees E) with which to study the MODIS leaf area index (LAI) and vegetation index (VI) products. The collection 4 MODIS LAI product correctly represented the summer site phenologies, but significantly underestimated the LAI value of the >100 year old coniferous forest during the November to April time period. Landsat 7-derived enhanced vegetation index (EVI) performed better than normalized difference vegetation index (NDVI) to separate the deciduous and conifer forests, and both indices contained significant correlation with field-derived LAI values at coniferous forest sites (r(2) = 0.61 and r(2) = 0.69, respectively). The reduced simple ratio (RSR) markedly improved LAI prediction from satellite measurements (r(2) = 0.89) relative to NDVI and EVI LAI estimates derived from ETM + images were scaled up to evaluate the 1 km resolution MODIS LAI product; from this analysis MODIS LAI overestimated values in the low LAI deciduous forests (where LAI < 5) and underestimated values in the high LAI conifer forests (where LAI > 6). Our results indicate that further research on the MODIS LAI product is warranted to better understand and improve remote LAI quantification in disturbed forest landscapes over the course of the year. C1 S Dakota Sch Mines & Technol, Inst Atmospher Sci, Rapid City, SD 57701 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Chen, X (reprint author), Sci Applicat Int Corp, Natl Ctr EROS, 47914 252nd St, Sioux Falls, SD 57198 USA. EM xuchen@usgs.gov RI Vierling, Lee/E-6428-2010 OI Vierling, Lee/0000-0001-5344-1983 NR 47 TC 34 Z9 35 U1 1 U2 12 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0143-1161 J9 INT J REMOTE SENS JI Int. J. Remote Sens. PD DEC 20 PY 2005 VL 26 IS 24 BP 5433 EP 5451 DI 10.1080/01431160500285142 PG 19 WC Remote Sensing; Imaging Science & Photographic Technology SC Remote Sensing; Imaging Science & Photographic Technology GA 003AK UT WOS:000234653800005 ER PT J AU Wang, MH AF Wang, MH TI A refinement for the Rayleigh radiance computation with variation of the atmospheric pressure SO INTERNATIONAL JOURNAL OF REMOTE SENSING LA English DT Article ID WATER-LEAVING RADIANCE; OCEAN-COLOR SENSORS; SURFACE-ROUGHNESS; SEAWIFS; ALGORITHM; SYSTEM; INSTRUMENT; SCANNER; IMAGERY; EARTH AB The Rayleigh scattering radiance at the top of the atmosphere (TOA) depends on the surface atmospheric pressure. In processing the Coastal Zone Color Scanner (CZCS) imagery, Gordon et al. (Applied Optics, 27, 862-871, 1988) developed a simple formula to account for the Rayleigh radiance changes with the variation of the surface atmospheric pressure. For the atmospheric pressure changes within +/- 3%, the accuracy of the Gordon et al. (1988) formula in computing the Rayleigh radiance is usually within 0.4%, 0.3%, 0.15% and 0.05% for the wavelengths 412, 443, 555 and 865 nm, respectively. This could result in up to similar to 3% uncertainty in the derived water-leaving radiance at the blue wavelengths for very clear atmospheres. To improve the performance, a refinement to the Gordon et al. (1988) formula is developed based on the radiative transfer simulations. The refined scheme can produce Rayleigh radiance with an uncertainty within 0.1% (often within 0.05%) at the blue, while uncertainty is within 0.05% for the green to near-infrared wavelengths. The refined algorithm has been implemented in the Sea-viewing Wide Field-of-view Sensor (SeaWiFS) data processing system. Results from the SeaWiFS data show the improved ocean colour products in the southern oceans where consistently low atmospheric pressures are usually observed. This could also significantly improve the performance of the Rayleigh radiance computations over the high altitude lakes. In addition, with the refined algorithm, the same Rayleigh radiance tables can be possibly used for the various ocean colour satellite sensors in which there are slightly different sensor spectral band characterizations. C1 Univ Maryland Baltimore Cty, NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Wang, MH (reprint author), NOAA, Natl Environm Satellite Data & Informat Serv, Off Res & Applicat, E-RA3,Room 102,5200 Auth Rd, Camp Springs, MD 20746 USA. EM Menghua.Wang@noaa.gov RI Wang, Menghua/F-5631-2010 OI Wang, Menghua/0000-0001-7019-3125 NR 16 TC 38 Z9 39 U1 1 U2 5 PU TAYLOR & FRANCIS LTD PI ABINGDON PA 4 PARK SQUARE, MILTON PARK, ABINGDON OX14 4RN, OXON, ENGLAND SN 0143-1161 J9 INT J REMOTE SENS JI Int. J. Remote Sens. PD DEC 20 PY 2005 VL 26 IS 24 BP 5651 EP 5663 DI 10.1080/01431160500168793 PG 13 WC Remote Sensing; Imaging Science & Photographic Technology SC Remote Sensing; Imaging Science & Photographic Technology GA 003AK UT WOS:000234653800018 ER PT J AU Chen, JS Fritz, TA Sheldon, RB AF Chen, JS Fritz, TA Sheldon, RB TI Comparison of energetic ions in cusp and outer radiation belt SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID ACCELERATION REGION; GEOMAGNETIC-FIELD; MAGNETIC-FIELD; SOLAR-WIND; MAGNETOSPHERE; PARTICLES; POLAR; POPULATION AB [1] Recently, large diamagnetic cavities with a size of as large as 6 Re have been observed in the dayside high-altitude cusp regions. Associated with these cavities are charged particles with energies from 20 keV up to 10 MeV. Their seed population is a mixture of ionospheric and solar wind particles. The energetic ion intensity, charge composition, energy spectrum, and phase space density observed in the high-altitude dayside cusp have been compared with that measured in the outer radiation belt over an energy range of 1 - 200 keV/e for protons and He++ ions and of 41 - 200 keV/ e for O+ ions. It is found that ( 1) the shape of ion energy spectra in the cusp is different from that in the outer radiation belt, ( 2) the ion phase space densities in the outer radiation belt are organized by magnetic moment, and ( 3) the ion phase space density of both He++ and O+ in the cusp are higher than that in the outer radiation belt at a given magnetic moment. These results suggest that ( 1) the measured cusp energetic ions cannot be explained by simple transport from an outer radiation belt ( or ring current) source; rather, ( 2) a nonadiabatic energization process would be required to relate the cusp energetic ion population to the belt ion population, and ( 3) cusp energetic particles are potentially an additional independent source of the charged particles in the outer radiation belt. C1 Boston Univ, Ctr Space Phys, Boston, MA 02215 USA. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA. RP Chen, JS (reprint author), Boston Univ, Ctr Space Phys, 725 Commonwealth Ave, Boston, MA 02215 USA. EM jschen@bu.edu; rob.sheldon@msfc.nasa.gov NR 19 TC 6 Z9 6 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 20 PY 2005 VL 110 IS A12 AR A12219 DI 10.1029/2004JA010718 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 999DE UT WOS:000234368100001 ER PT J AU Sodano, HA Bae, JS Inman, DJ Belvin, WK AF Sodano, HA Bae, JS Inman, DJ Belvin, WK TI Concept and model of eddy current damper for vibration suppression of a beam SO JOURNAL OF SOUND AND VIBRATION LA English DT Article ID MAGNETIC BRAKING AB Electromagnetic forces are generated by the movement of a conductor through a stationary magnetic field or a time varying magnetic field through a stationary conductor and can be used to suppress the vibrations of a flexible structure. In the present study, a new electromagnetic damping mechanism is introduced. This mechanism is different from previously developed electromagnetic braking systems and eddy current dampers because the system investigated in the subsequent manuscript uses the radial magnetic flux to generate the electromagnetic damping force rather than the flux perpendicular to the magnet's face as done in other studies. One important advantage of the proposed mechanism is that it is simple and easy to apply. Additionally, a single magnet can be used to damp the transverse vibrations that are present in many structures. Furthermore, it does not require any electronic devices or external power supplies, therefore functioning as a non-contacting passive damper. A theoretical model of the system is derived using electromagnetic theory enabling us to estimate the electromagnetic damping force induced on the structure. The proposed eddy current damper was constructed and experiments were performed to verify the precision of the theoretical model. It is found that the proposed eddy current damping mechanism could increase the damping ratio by up to 150 times and provide sufficient damping force to quickly suppress the beam's vibration. (c) 2005 Elsevier Ltd. All rights reserved. C1 Virginia Polytech Inst & State Univ, Ctr Intelligent Mat Syst & Struct, Blacksburg, VA 24061 USA. Hankuk Aviat Univ, Sch Aerosp & Mech Engn, Goyang 412791, Geonggi, South Korea. NASA, Langley Res Ctr, Struct Dynam Branch, Hampton, VA 23681 USA. RP Sodano, HA (reprint author), Virginia Polytech Inst & State Univ, Ctr Intelligent Mat Syst & Struct, Blacksburg, VA 24061 USA. EM hsodano@vt.edu NR 18 TC 55 Z9 61 U1 1 U2 15 PU ACADEMIC PRESS LTD ELSEVIER SCIENCE LTD PI LONDON PA 24-28 OVAL RD, LONDON NW1 7DX, ENGLAND SN 0022-460X J9 J SOUND VIB JI J. Sound Vibr. PD DEC 20 PY 2005 VL 288 IS 4-5 BP 1177 EP 1196 DI 10.1016/j.jsv.2005.01.016 PG 20 WC Acoustics; Engineering, Mechanical; Mechanics SC Acoustics; Engineering; Mechanics GA 978MP UT WOS:000232878000018 ER PT J AU Jun, I Garrett, HB AF Jun, I Garrett, HB TI Comparison of high-energy trapped particle environments at the Earth and Jupiter SO RADIATION PROTECTION DOSIMETRY LA English DT Article AB The 'Van Allen belts' of the trapped energetic particles in the Earth's magnetosphere were discovered by the Explorer I satellite in 1958. In addition, in 1959, it was observed that UHF radio emissions from Jupiter probably had a similar source-the Jovian radiation belts. In this paper, the global characteristics of these two planets' trapped radiation environments and respective magnetospheres are compared and state-of-the-art models used to generate estimates of the high-energy electron (>= 100 keV) and proton (>= 1 MeV) populations-the dominant radiation particles in these environments. The models used are the AP8/AE8 series for the Earth and the Divine-Garrett/GIRE model for Jupiter. To illustrate the relative magnitude of radiation effects at each planet, radiation transport calculations were performed to compute the total ionising dose levels at the geosynchronous orbit for the Earth and at Europa (Jupiter's 4th largest moon) for Jupiter. The results show that the dose rates are similar to 0.1 krad(Si) d(-1) at the geosynchronous orbit and similar to 30 krad(Si) d(-1) at Europa for a 2.5 mm spherical shell aluminium shield-a factor of similar to 300 between the two planets. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Jun, I (reprint author), CALTECH, Jet Prop Lab, Mail Stop 122-107,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM insoo.jun@jpl.nasa.gov NR 12 TC 6 Z9 6 U1 0 U2 1 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0144-8420 J9 RADIAT PROT DOSIM JI Radiat. Prot. Dosim. PD DEC 20 PY 2005 VL 116 IS 1-4 BP 50 EP 54 DI 10.1093/rpd-nci074 PG 5 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 004XA UT WOS:000234784800012 PM 16604595 ER PT J AU Andersen, V Ballarini, F Battistoni, G Cerutti, F Empl, A Fasso, A Ferrari, A Garzelli, MV Ottolenghi, A Paretzke, H Pinsky, L Ranft, J Sala, P Wilson, T Zankl, M AF Andersen, V Ballarini, F Battistoni, G Cerutti, F Empl, A Fasso, A Ferrari, A Garzelli, MV Ottolenghi, A Paretzke, H Pinsky, L Ranft, J Sala, P Wilson, T Zankl, M TI The application of FLUKA to dosimetry and radiation therapy SO RADIATION PROTECTION DOSIMETRY LA English DT Article AB The FLUKA Monte Carlo code has been evolving over the last several decades and is now widely used for radiation shielding calculations. In order to facilitate the use of FLUKA in dosimetry and therapy applications, supporting software has been developed to allow the direct conversion of the output files from standard CT-scans directly into a voxel geometry for transport within FLUKA. Since the CT-scan information essentially contains only the electron density information over the scanned volume, one needs the specific compositions for each voxel individually. We present here the results of a simple algorithm to assign tissues in the human body to one of four categories: soft-tissue, hard-bone, trabecular-bone and porous-lung. In addition, we explore the problem of the pathlength distributions in porous media such as trabecular bone. A mechanism will be implemented within FLUKA to allow for variable multipal fixed density materials to accommodate the pathlength distributions discovered. C1 Univ Houston, Houston, TX 77004 USA. Univ Pavia, I-27100 Pavia, Italy. Univ Milan, I-20122 Milan, Italy. CERN, Geneva, Switzerland. SLAC, Stanford, CA USA. GSF, Neuherberg, Germany. Univ Leipzig, Leipzig, Germany. ETH, Zurich, Switzerland. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Pinsky, L (reprint author), Univ Houston, Houston, TX 77004 USA. EM pinsky@uh.edu RI sala, paola/E-2868-2013; Ballarini, Francesca/J-7293-2013; Zankl, Maria/M-7348-2014; Battistoni, Giuseppe/B-5264-2012 OI sala, paola/0000-0001-9859-5564; Ballarini, Francesca/0000-0002-6629-3382; Zankl, Maria/0000-0003-4743-970X; Battistoni, Giuseppe/0000-0003-3484-1724 NR 4 TC 7 Z9 7 U1 0 U2 7 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0144-8420 J9 RADIAT PROT DOSIM JI Radiat. Prot. Dosim. PD DEC 20 PY 2005 VL 116 IS 1-4 BP 113 EP 117 DI 10.1093/rpd/nci040 PG 5 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 004XA UT WOS:000234784800026 PM 16604609 ER PT J AU Atwell, W Townsend, L Miller, T Campbell, C AF Atwell, W Townsend, L Miller, T Campbell, C TI A reassessment of Galileo radiation exposures in the Jupiter magnetosphere SO RADIATION PROTECTION DOSIMETRY LA English DT Article DE cDNA microarray; dark-rearing; opioid-binding cell adhesion molecule; striate cortex ID PARTICLES AB Earlier particle experiments in the 1970s on Pioneer-10 and -11 and Voyager-1 and -2 provided Jupiter flyby particle data, which were used by Divine and Garrett to develop the first Jupiter trapped radiation environment model. This model was used to establish a baseline radiation effects design limit for the Galileo onboard electronics. Recently, Garrett et al. have developed an updated Galileo Interim Radiation Environment (GIRE) model based on Galileo electron data. In this paper, we have used the GIRE model to reassess the computed radiation exposures and dose effects for Galileo. The 34-orbit 'as flown' Galileo trajectory data and the updated GIRE model were used to compute the electron and proton spectra for each of the 34 orbits. The total ionisation doses of electrons and protons have been computed based on a parametric shielding configuration, and these results are compared with previously published results. C1 NASA Syst, Boeing Co, Houston, TX 77058 USA. Univ Tennessee, Dept Nucl Engn, Knoxville, TN 37996 USA. RP Atwell, W (reprint author), NASA Syst, Boeing Co, Houston, TX 77058 USA. EM bigshot@houston.rr.com NR 7 TC 0 Z9 0 U1 1 U2 2 PU OXFORD UNIV PRESS PI OXFORD PA GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND SN 0144-8420 J9 RADIAT PROT DOSIM JI Radiat. Prot. Dosim. PD DEC 20 PY 2005 VL 116 IS 1-4 BP 220 EP 223 DI 10.1093/rpd/nci009 PG 4 WC Environmental Sciences; Public, Environmental & Occupational Health; Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical Imaging SC Environmental Sciences & Ecology; Public, Environmental & Occupational Health; Nuclear Science & Technology; Radiology, Nuclear Medicine & Medical Imaging GA 004XA UT WOS:000234784800048 PM 16604631 ER PT J AU Blacksberg, J Hoenk, ME Elliott, ST Holland, SE Nikzad, S AF Blacksberg, J Hoenk, ME Elliott, ST Holland, SE Nikzad, S TI Enhanced quantum efficiency of high-purity silicon imaging detectors by ultralow temperature surface modification using Sb doping SO APPLIED PHYSICS LETTERS LA English DT Article ID HIGH-RESISTIVITY SILICON; P-CHANNEL CCDS; LAYER AB A low temperature process for Sb doping of silicon has been developed as a backsurface treatment for high-purity n-type imaging detectors. Molecular beam epitaxy (MBE) is used to achieve very high dopant incorporation in a thin, surface-confined layer. The growth temperature is kept below 450 degrees C for compatibility with Al-metallized devices. Imaging with MBE-modified 1kx1k charge coupled devices (CCDs) operated in full depletion has been demonstrated. Dark current is comparable to the state-of-the-art process, which requires a high temperature step. Quantum efficiency is improved, especially in the UV, for thin doped layers placed closer to the backsurface. Near 100% internal quantum efficiency has been demonstrated in the ultraviolet for a CCD with a 1.5 nm silicon cap layer. C1 CALTECH, Jet Propuls Lab, Pasadena, CA 91109 USA. Lawrence Berkeley Lab, Berkeley, CA 94720 USA. RP Blacksberg, J (reprint author), CALTECH, Jet Propuls Lab, Pasadena, CA 91109 USA. EM jordana.blacksberg@jpl.nasa.gov; shouleh.nikzad@jpl.nasa.gov NR 11 TC 10 Z9 10 U1 1 U2 4 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0003-6951 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD DEC 19 PY 2005 VL 87 IS 25 AR 254101 DI 10.1063/1.2149181 PG 3 WC Physics, Applied SC Physics GA 995QM UT WOS:000234118900106 ER PT J AU Kim, TH Gangopadhyay, AK Xing, LQ Lee, GW Shen, YT Kelton, KF Goldman, AI Hyers, RW Rogers, JR AF Kim, TH Gangopadhyay, AK Xing, LQ Lee, GW Shen, YT Kelton, KF Goldman, AI Hyers, RW Rogers, JR TI Role of Ti in the formation of Zr-Ti-Cu-Ni-Al glasses SO APPLIED PHYSICS LETTERS LA English DT Article ID SHORT-RANGE ORDER; QUASI-CRYSTALLINE PHASE; METALLIC GLASSES; ALLOYS; BEHAVIOR; OXYGEN AB It has been widely reported that glass formation improves in Zr62Cu20Ni8Al10 alloys when small amounts of Ti are substituted for Zr. Glasses containing greater than 3 at. % Ti crystallize to a metastable icosahedral phase, suggesting that Ti enhances icosahedral short-range order in the liquid/glass, making crystallization more difficult during cooling. However, based on containerless solidification and in situ high-energy synchrotron diffraction studies of electrostatically levitated supercooled liquids of these alloys, we demonstrate that Ti inhibits surface crystallization but neither increases the icosahedral short-range order nor improves glass formation. (c) 2005 American Institute of Physics. C1 Washington Univ, Dept Phys, St Louis, MO 63130 USA. US DOE, Ames Lab, Ames, IA 50011 USA. Iowa State Univ, Ames, IA 50011 USA. Univ Massachusetts, Amherst, MA 01003 USA. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Kim, TH (reprint author), Washington Univ, Dept Phys, St Louis, MO 63130 USA. EM thkim@hbar.wustl.edu RI Hyers, Robert/G-3755-2010 NR 19 TC 10 Z9 10 U1 2 U2 8 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0003-6951 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD DEC 19 PY 2005 VL 87 IS 25 AR 251924 DI 10.1063/1.2149368 PG 3 WC Physics, Applied SC Physics GA 995QM UT WOS:000234118900034 ER PT J AU Koswatta, SO Lundstrom, MS Anantram, MP Nikonov, DE AF Koswatta, SO Lundstrom, MS Anantram, MP Nikonov, DE TI Simulation of phonon-assisted band-to-band tunneling in carbon nanotube field-effect transistors SO APPLIED PHYSICS LETTERS LA English DT Article AB Electronic transport in a carbon nanotube metal-oxide-semiconductor field effect transistor (MOSFET) is simulated using the nonequilibrium Green's functions method with the account of electron-phonon scattering. For MOSFETs, ambipolar conduction is explained via phonon-assisted band-to-band (Landau-Zener) tunneling. In comparison to the ballistic case, we show that the phonon scattering shifts the onset of ambipolar conduction to more positive gate voltage (thereby increasing the off current). It is found that the subthreshold swing in ambipolar conduction can be made as steep as 40 mV/decade despite the effect of phonon scattering. C1 Purdue Univ, Sch Elect & Comp Engn, W Lafayette, IN 47907 USA. NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. Intel Corp, Technol & Mfg Grp, Santa Clara, CA 95052 USA. RP Koswatta, SO (reprint author), Purdue Univ, Sch Elect & Comp Engn, W Lafayette, IN 47907 USA. EM dmitri.e.nikonov@intel.com RI Nikonov, Dmitri/B-6502-2011 OI Nikonov, Dmitri/0000-0002-1436-1267 NR 17 TC 37 Z9 37 U1 0 U2 10 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0003-6951 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD DEC 19 PY 2005 VL 87 IS 25 AR 253107 DI 10.1063/1.2146065 PG 3 WC Physics, Applied SC Physics GA 995QM UT WOS:000234118900083 ER PT J AU Sokolow, A Pfannes, JMM Doney, RL Nakagawa, M Agui, JH Sen, S AF Sokolow, A Pfannes, JMM Doney, RL Nakagawa, M Agui, JH Sen, S TI Absorption of short duration pulses by small, scalable, tapered granular chains SO APPLIED PHYSICS LETTERS LA English DT Article ID IMPULSE PROPAGATION AB Making shock proof layers is an outstanding challenge. Elastic spheres are known to repel softer than springs when gently squeezed but develop strong repulsion upon compression and the forces between adjacent spheres lead to ballistic-like energy transfer between them. Here we demonstrate that a small alignment of progressively shrinking spheres of a strong, light-mass material, placed horizontally in an appropriate casing, can absorb similar to 80% (similar to 90%) of the incident force (energy) pulse. The system can be scaled down in size. Effects of varying the size, radius shrinkage and restitutive losses are shown via computed "dynamical phase diagrams." C1 SUNY Buffalo, Dept Phys, Buffalo, NY 14260 USA. Colorado Sch Mines, Dept Min Engn, Golden, CO 80401 USA. NASA Glenn Res Ctr, Cleveland, OH 44135 USA. RP Sen, S (reprint author), SUNY Buffalo, Dept Phys, Buffalo, NY 14260 USA. EM sen@dynamics.physics.buffalo.edu NR 17 TC 25 Z9 25 U1 0 U2 2 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0003-6951 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD DEC 19 PY 2005 VL 87 IS 25 AR 254104 DI 10.1063/1.2149218 PG 3 WC Physics, Applied SC Physics GA 995QM UT WOS:000234118900109 ER PT J AU Johnson, RE Liu, M Sittler, EC AF Johnson, RE Liu, M Sittler, EC TI Plasma-induced clearing and redistribution of material embedded in planetary magnetospheres SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID SATURNS MAGNETOSPHERE; TORUS; IONS; DYNAMICS; NITROGEN AB Charge exchange collisions between the ions trapped in a planetary magnetosphere and the ambient neutrals are a principal material loss process in evolving planetary systems (Johnson, 2004). Here we show that low energy charge exchange collisions, in which orbiting occurs, can drastically modify the redistribution and loss of materials in evolving planetary disks. Using Saturn as an example, these collisions can account for the fact that water products, produced primarily in the inner magnetosphere, are found to be the dominant ions throughout Saturn's magnetosphere. C1 Univ Virginia, Engn Phys Program, Charlottesville, VA 22904 USA. Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA. NYU, Dept Phys, New York, NY 10003 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Johnson, RE (reprint author), Univ Virginia, Engn Phys Program, Charlottesville, VA 22904 USA. EM rej@virginia.edu NR 21 TC 20 Z9 20 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 17 PY 2005 VL 32 IS 24 AR L24201 DI 10.1029/2005GL024275 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 998BN UT WOS:000234293000004 ER PT J AU Guest, A Smrekar, SE AF Guest, A Smrekar, SE TI Relaxation of the Martian dichotomy boundary: Faulting in the Ismenius Region and constraints on the early evolution of Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID VISCOUS RELAXATION; CRUSTAL DICHOTOMY; PLATE-TECTONICS; HEMISPHERIC DICHOTOMY; IMPACT BASINS; GIANT IMPACT; TOPOGRAPHY; THICKNESS; GRAVITY; ORIGIN AB The Martian dichotomy is a global feature separating the cratered southern highlands and smooth northern lowlands. Parts of the boundary are defined by steep slopes with elevation differences of 2-6 km. Here we use constraints from the well-preserved section of the dichotomy in the Ismenius Region. We study the relaxation of the boundary using both finite element and semianalytical techniques to better constrain the thermomechanical conditions in early Mars. We argue that the steep slopes are the product of faulting resulting from relaxation of the edge of the boundary by lower crustal flow. This relaxation requires that the lower crust must be at least 10 km thick and have a viscosity of similar to 10(21) Pa s during the first 100-300 Myr of relaxation. We show that a wet crustal rheology and a thermal gradient of similar to 15-20 K/km at 4 Ga allows for both the partial relaxation of the Martian dichotomy and preservation of long wavelength topography as observed on Mars. This result is generally consistent with a stagnant-lid model of cooling of Martian interior. The thermal gradient at 4 Ga is also consistent with the estimated elastic thickness on early Mars. Our modeling constrains the original slope of the boundary to approximately 2 degrees. We cannot constrain the crustal thickness more tightly than the current estimates of 50-100 km. On the basis of our semianalytical modeling, the relaxation of the boundary can contribute to the general north-south slope observed on Mars. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91106 USA. RP Guest, A (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 183-501, Pasadena, CA 91106 USA. EM alickaguest@yahoo.com; ssmrekar@jpl.nasa.gov NR 44 TC 8 Z9 8 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD DEC 17 PY 2005 VL 110 IS E12 AR E12S25 DI 10.1029/2005JE002504 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 998CJ UT WOS:000234295300001 ER PT J AU Considine, DB Bergmann, DJ Liu, H AF Considine, DB Bergmann, DJ Liu, H TI Sensitivity of Global Modeling Initiative chemistry and transport model simulations of radon-222 and lead-210 to input meteorological data SO ATMOSPHERIC CHEMISTRY AND PHYSICS LA English DT Article ID GENERAL-CIRCULATION MODEL; OBSERVED RADON PROFILES; ATMOSPHERIC TRANSPORT; 3-DIMENSIONAL SIMULATION; NATIONAL CENTER; WET DEPOSITION; DRY DEPOSITION; CLIMATE MODEL; PARAMETERIZATION; AEROSOLS AB We have used the Global Modeling Initiative chemistry and transport model to simulate the radionuclides radon-222 and lead-210 using three different sets of input meteorological information: 1. Output from the Goddard Space Flight Center Global Modeling and Assimilation Office GEOS-STRAT assimilation; 2. Output from the Goddard Institute for Space Studies GISS II' general circulation model; and 3. Output from the National Center for Atmospheric Research MACCM3 general circulation model. We intercompare these simulations with observations to determine the variability resulting from the different meteorological data used to drive the model, and to assess the agreement of the simulations with observations at the surface and in the upper troposphere/ lower stratosphere region. The observational datasets we use are primarily climatologies developed from multiple years of observations. In the upper troposphere/ lower stratosphere region, climatological distributions of lead-210 were constructed from similar to 25 years of aircraft and balloon observations compiled into the US Environmental Measurements Laboratory RANDAB database. Taken as a whole, no simulation stands out as superior to the others. However, the simulation driven by the NCARMACCM3 meteorological data compares better with lead-210 observations in the upper troposphere/ lower stratosphere region. Comparisons of simulations made with and without convection show that the role played by convective transport and scavenging in the three simulations differs substantially. These differences may have implications for evaluation of the importance of very short-lived halogen-containing species on stratospheric halogen budgets. C1 NASA, Langley Res Ctr, Hampton, VA 23665 USA. Lawrence Livermore Natl Lab, Livermore, CA USA. Natl Inst Aerosp, Hampton, VA USA. RP Considine, DB (reprint author), NASA, Langley Res Ctr, Hampton, VA 23665 USA. EM david.b.considine@nasa.gov RI Liu, Hongyu/A-5867-2008; Bergmann, Daniel/F-9801-2011 OI Bergmann, Daniel/0000-0003-4357-6301 NR 51 TC 26 Z9 26 U1 0 U2 11 PU COPERNICUS GESELLSCHAFT MBH PI GOTTINGEN PA BAHNHOFSALLEE 1E, GOTTINGEN, 37081, GERMANY SN 1680-7316 EI 1680-7324 J9 ATMOS CHEM PHYS JI Atmos. Chem. Phys. PD DEC 16 PY 2005 VL 5 BP 3389 EP 3406 PG 18 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 993ZR UT WOS:000233999600002 ER PT J AU Lillis, RJ Engel, JH Mitchell, DL Brain, DA Lin, RP Bougher, SW Acuna, MH AF Lillis, RJ Engel, JH Mitchell, DL Brain, DA Lin, RP Bougher, SW Acuna, MH TI Probing upper thermospheric neutral densities at Mars using electron reflectometry SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID CRUSTAL MAGNETIC-FIELD AB We present a new technique for inferring neutral densities in the Martian upper atmosphere from atmospheric absorption of magnetically reflected solar wind electrons. Using electron loss cone measurements from the Magnetometer/Electron Reflectometer (MAG/ER) experiment on board Mars Global Surveyor (MGS), we derive upper thermospheric (similar to 160-230 km altitude) densities in the southern hemisphere from 160\degrees to 200 degrees E at 2am local time, continuously from 1999 to 2005. We find a mean density of 0.027 kg/km(3) at 160 km and observe a latitude-dependent, repeatable seasonal variation of a factor of 1.8-4, with inter-annual differences and consistently lower winter densities at 50 degrees-55 degrees S, compared with 0 degrees-30 degrees S. The mean densities, overall seasonal variation and latitude dependence are in general agreement with the Mars Thermosphere Global Circulation Model (MTGCM). These measurements are important for improved understanding of the dynamics of Mars' upper atmosphere and for planning spacecraft aerobraking maneuvers. C1 Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA. Univ Michigan, Ann Arbor, MI 48109 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Lillis, RJ (reprint author), Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. EM rlillis@ssl.berkeley.edu RI Bougher, Stephen/C-1913-2013; Lillis, Robert/A-3281-2008 OI Bougher, Stephen/0000-0002-4178-2729; Lillis, Robert/0000-0003-0578-517X NR 20 TC 8 Z9 8 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 15 PY 2005 VL 32 IS 23 AR L23204 DI 10.1029/2005GL024337 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 998BJ UT WOS:000234292600003 ER PT J AU Stalport, F Coll, P Cabane, M Person, A Gonzalez, RN Raulin, F Vaulay, MJ Ausset, P McKay, CP Szopa, C Zarnecki, J AF Stalport, F Coll, P Cabane, M Person, A Gonzalez, RN Raulin, F Vaulay, MJ Ausset, P McKay, CP Szopa, C Zarnecki, J TI Search for past life on Mars: Physical and chemical characterization of minerals of biotic and abiotic origin: part 1 - Calcite SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID WET AB Several lines of evidence suggest that early Mars once had liquid water on its surface, a denser atmosphere and a mild climate. Similar environmental conditions led to the origin of life on the Earth more than 3.5 billion years ago; consequently, life might also have originated on Mars. The Viking landers searched for evidence of organic molecules on the surface of Mars, and found that the Martian soil is depleted in organics at ppb levels at the landing sites. We contend that inorganic compounds could give us interesting clues as to the existence of possible biological activity in future astrobiological missions to Mars. Consequently, we have investigated the physical and chemical properties of calcite, which could be expected on Mars because liquid water was certainly present on the surface of early Mars and carbon dioxide was abundant in its atmosphere. Calcite is interesting because on Earth this mineral is produced by abiotic processes as well as by biological activity. One may suppose that crystalline defects and trace element in the crystal lattice and the growth speed of biotic calcites must indicate a difference between them and pure abiotic calcites. We investigated twelve different terrestrial calcite samples from various origins: biotic, diagenetic and abiotic. The minerals were studied by X-ray diffraction and electron scanning microscopy to determine their mineralogical and chemical composition, and differential thermal analysis coupled to thermogravimetric analysis (DTA-TG) to determine their thermal behavior. Our results show that the thermal degradation of abiotic calcite starts at a temperature at least 40 degrees C higher than the degradation temperature of any biotic calcite investigated. Consequently, in the case of a Martian in-situ study or in a sample return mission, the analysis of Martian minerals by DTA-TG represents a promising approach to detect evidence of past biological activity on Mars. C1 Univ Paris 12, Lab Interuniv Syst Atmospher, F-94010 Creteil, France. Univ Paris 06, CNRS, Serv Aeron, SA IPSL, F-75005 Paris, France. Univ Paris 06, Lab Geol Sedimentaire, F-75005 Paris, France. Univ Nacl Autonoma Mexico, Lab Quim Plasmas & Estudios Planetarios, Mexico City 04510, DF, Mexico. Univ Paris 07, ITODYS, F-75005 Paris, France. NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. Open Univ, Planetary & Space Sci Res Inst, Milton Keynes MK15 0BT, Bucks, England. RP Stalport, F (reprint author), Univ Paris 12, Lab Interuniv Syst Atmospher, F-94010 Creteil, France. EM stalport@lisa.univ-paris12.fr RI Gonzalez, Rafael/D-1748-2009; szopa, cyril/C-6865-2015 OI szopa, cyril/0000-0002-0090-4056 NR 21 TC 21 Z9 22 U1 1 U2 10 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 15 PY 2005 VL 32 IS 23 AR L23205 DI 10.1029/2005GL023403 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 998BJ UT WOS:000234292600001 ER PT J AU Hubickyj, O Bodenheimer, P Lissauer, JJ AF Hubickyj, O Bodenheimer, P Lissauer, JJ TI Accretion of the gaseous envelope of Jupiter around a 5-10 Earth-mass core SO ICARUS LA English DT Article DE Jupiter, formation; Jupiter, interiors; accretion; origin of planetary systems ID GIANT PLANET FORMATION; ROSSELAND OPACITY TABLES; PROTOPLANETARY DISKS; SOLAR NEBULA; GRAVITATIONAL INSTABILITIES; EXTRASOLAR PLANETS; PROTOSTELLAR DISKS; THERMAL REGULATION; HOST STARS; EVOLUTION AB New numerical simulations of the formation and evolution of Jupiter are presented. The formation model assumes that first a solid core of several M circle plus accretes from the planetesimals in the protoplanetary disk, and then the core captures a massive gaseous envelope from the protoplanetary disk. Earlier studies of the core accretion-gas capture model [Pollack, J.B., Hubickyj, O., Bodenheimer, P., Lissauer, J.J., Podolak, M., Greenzweig, Y., 1996. Icarus 124, 62-85] demonstrated that it was possible for Jupiter to accrete with a solid core of 10-30 M circle plus in a total formation time comparable to the observed lifetime of protoplanetary disks. Recent interior models of Jupiter and Saturn that agree with all observational constraints suggest that Jupiter's core mass is 0-11 M circle plus and Saturn's is 9-22 M circle plus [Saumon, G., Guillot, T., 2004. Astrophys. J. 609, 1170-1180]. We have computed simulatons of the growth of Jupiter using various values for the opacity produced by grains in the protoplanet's atmosphere and for the initial planetesimal Surface density, sigma(init,Z), in the protoplanetary disk. We also explore the implications of halting the solid accretion at selected core mass values during the protoplanet's growth. Halting planetesimal accretion at low core mass Simulates the presence of a competing embryo, and decreasing the atmospheric opacity adjusting due to grains emulates the settling and coagulation of grains within the protoplanet's atmosphere. We examine the effects of ad these parameters to determine whether or not gas runaway can occur for small mass cores on a reasonable timescale. We compute four series Of Simulations with the latest version Of our code, which contains updated equation of state and opacity tables as well as other improvernents. Each series consists of a RIII without a cutoff in planetesimal accretion, plus up to three runs with a Cutoff at a particular core mass. The first series of runs is computed with an atmospheric opacity due to grains (hereafter referred to as 'grain opacity') that is 2% of the interstellar value and sigma(init),(Z) = 10 g/cm(2). Cutoff runs are computed for core masses of 10, 5, and 3 M circle plus. The second series of Jupiter models is computed with the grain opacity at the full interstellar Value and sigma(init,Z) = 10 g-/cm(2). Cutoff runs are computed for core masses of 10 and 5 M circle plus. The third series of runs is computed with the grain opacity at 2% of the interstellar value and sigma(init,Z) = 6 g/cm(2). One cutoff run is computed with core mass of 5 M circle plus. The final series consists of one run, without a Cutoff, which is computed with a temperature dependent grain opacity (i.e., 2% of the interstellar value for T < 350 K ramping LIP to the full interstellar value for T > 500 K) and sigma(init,Z) = 10 g/cm(2.) Our results demonstrate that reducing grain opacities results in formation times less than half of those for models computed with full interstellar grain opacity values. The reduction of opacity due to grains in the upper portion of the envelope with T < 500 K has the largest effect on the lowering of the formation time. If the accretion of planetesimals is not cut off prior to the accretion of gas, then decreasing the surface density of planetesimals lowers the final core mass of the protoplanet, but increases the formation timescale considerably. Finally, a core mass cutoff results in a reduction of the time needed for I protoplanet to evolve to thestage of runaway gas accretion, provided the cutoff mass is sufficiently large. The overall results indicate that, with reasonable parameters, it is possible that Jupiter formed at 5 AU via the core accretion process in I Myr with a core of 10 M circle plus or in 5 Myr with a core of 5 M circle plus. Published by Elsevier Inc. C1 Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA. NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. RP Hubickyj, O (reprint author), Univ Calif Santa Cruz, Dept Astron & Astrophys, UCO Lick Observ, Santa Cruz, CA 95064 USA. EM hubickyj@pollack.arc.nasa.gov NR 91 TC 258 Z9 259 U1 0 U2 7 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD DEC 15 PY 2005 VL 179 IS 2 BP 415 EP 431 DI 10.1016/j.icarus.2005.06.021 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 995HY UT WOS:000234092600009 ER PT J AU Matcheva, KI Conrath, BJ Gierasch, PJ Flasar, FM AF Matcheva, KI Conrath, BJ Gierasch, PJ Flasar, FM TI The cloud structure of the jovian atmosphere as seen by the Cassini/CIRS experiment SO ICARUS LA English DT Article DE Jupiter; Jupiter, atmosphere; atmospheres, structure ID NORTH EQUATORIAL BELT; LARGE PHASE ANGLES; GALILEO PROBE DATA; JUPITERS ATMOSPHERE; THERMAL STRUCTURE; UPPER TROPOSPHERE; ISOTOPIC RATIO; GIANT PLANETS; IMAGING DATA; WATER-VAPOR AB We analyze the thermal infrared spectra of Jupiter obtained by the Cassini-CIRS instrument during the 2000 flyby to infer temperature and cloud density in the jovian stratosphere and upper troposphere. We use an inversion technique to derive zonal mean vertical profiles of Cloud absorption coefficient and optical thickness from a narrow spectral window centered at 1392 cm(-1) (7.18 mu m). At this wavenumber atmospheric absorption due to ammonia gas is very weak and uncertainties in the ammonia abundance do not impact the cloud retrieval results. For cloud-free conditions the atmospheric transmission is limited by the absorption of molecular hydrogen and methane. The gaseous optical depth of the atmosphere is of order unity at about 1200 mbar. This allows us to probe the structure of the atmosphere through a layer where ammonia Cloud formation is expected. The results are presented as height vs latitude cross-sections of the zonal mean Cloud optical depth and cloud absorption coefficient. The cloud optical depth and the cloud base pressure exhibit a significant variability with latitude. In regions with thin Cloud cover (Cloud optical depth less than 2), the cloud absorption coefficient peaks at 1.1 +/- 0.05 bar, whereas in regions with thick clouds the peak Cloud absorption coefficient Occurs in the vicinity of 900 +/- 50 mbar. If the Cloud optical depth is too large the location of the Cloud peak cannot be identified. Based oil theoretical expectations for the ammonia condensation pressure we conclude that the detected clouds are probably a system of two different cloud layers: a top ammonia ice layer at about 900 mbar covering only limited latitudes and a second, deeper layer at 1100 mbar, possibly made of ammonium hydrosuffide. (c) 2005 Elsevier Inc. All rights reserved. C1 Cornell Univ, Dept Astron, Ithaca, NY 14853 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Matcheva, KI (reprint author), Univ Florida, Dept Phys, Gainesville, FL 32611 USA. EM katia@phys.ufl.edu RI Flasar, F Michael/C-8509-2012 NR 48 TC 28 Z9 28 U1 0 U2 3 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD DEC 15 PY 2005 VL 179 IS 2 BP 432 EP 448 DI 10.1016/j.icarus.2005.06.020 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 995HY UT WOS:000234092600010 ER PT J AU Bernstein, MP Cruikshank, DP Sandford, SA AF Bernstein, MP Cruikshank, DP Sandford, SA TI Near-infrared laboratory spectra of solid H2O/CO2 and CH3OH/CO2 ice mixtures SO ICARUS LA English DT Article DE ices, infrared observations; spectroscopy; surfaces, planets, satellites ID INTERSTELLAR GRAIN MANTLES; WATER-ICE; ASTROPHYSICAL IMPLICATIONS; PHYSICAL STATE; AMORPHOUS ICE; MU-M; CO2; SURFACE; ABSORPTION; TRITON AB We present near-IR spectra of solid CO2 in H2O and CH3OH, and find they are significantly different from that Of pure solid CO2. Peaks not present in either pure H2O Or pure CO2 spectra become evident when the two are mixed. First, the Putative theoretically forbidden CO? (2 nu(3)) overtone near 2.134 mu m (4685 cm(-1)), that is absent from Our Spectrum of pure solid CO2, is prominent in the spectra of H2O/CO2 = 5 and 25 Mixtures. Second, a 2.74-mu m (3650 cm(-1)) dangling OH feature of H2O (and a potentially related peak at 1.89 mu m) appear in the spectra of CO2-H2O ice Mixtures, but are probably not diagnostic of the presence of CO,). Other CO2 peaks display shifts in position and increased width because of intermolecular interactions with H2O. Warming causes some peak positions and profiles in the spectrum of a H2O/CO2 = 5 Mixture to take oil the appearance Of Pure CO2. Absolute strengths for absorptions of CO2 in solid H2O are estimated. similar results are observed for CO2 in solid CH3OH. Since the CO2 (2 nu(3)) overtone near 2.134 mu m (4685 cm(-1)) is not present in pure CO2 but prominent in Mixtures, it may be a good observational (spectral) indicator of whether solid CO2 is a pure material or intimately mixed with other Molecules. These observations may be applicable to Mars polar caps as well as Outer Solar System bodies. Published by Elsevier Inc. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Bernstein, MP (reprint author), NASA, Ames Res Ctr, MS 245-6, Moffett Field, CA 94035 USA. EM mbernstein@mail.arc.nasa.gov NR 35 TC 53 Z9 54 U1 1 U2 12 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD DEC 15 PY 2005 VL 179 IS 2 BP 527 EP 534 DI 10.1016/j.icarus.2005.07.009 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 995HY UT WOS:000234092600018 ER PT J AU Blacksberg, J Hoenk, ME Nikzad, S AF Blacksberg, J Hoenk, ME Nikzad, S TI Ultra-low-temperature homoepitaxial growth of Sb-doped silicon SO JOURNAL OF CRYSTAL GROWTH LA English DT Article DE delta doping; surfaces; surface segregation; molecular beam epitaxy; semiconducting silicon ID MOLECULAR-BEAM EPITAXY; SCANNING-TUNNELING-MICROSCOPY; SURFACE SEGREGATION; SI; SI(100); SI(001); PHOSPHORUS; ADSORPTION; DIFFUSION; LAYERS AB An ultra-low-temperature process for homoepitaxial growth of high-quality, surface-confined, Sb-doped silicon layers is presented. Non-equilibrium growth by molecular beam epitaxy (MBE) is used to achieve dopant incorporation in excess of 2 x 10(14) cm(-2) in a thin, surface-confined layer. Sb surface segregation larger than expected from theoretical models was observed, in agreement with other experimental works. Furthermore, this work details an entirely low-temperature process (< 450 degrees C) that can be applied to fully processed and aluminum-metallized silicon devices. One application of this process is the formation of a back-surface electrode for back-illuminated high-purity silicon imaging arrays. (c) 2005 Elsevier B.V. All rights reserved. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Blacksberg, J (reprint author), CALTECH, Jet Prop Lab, Mail Stop 302-306,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Jordana.Blacksberg@jpl.nasa.gov; Shouleh.Nikzad@jpl.nasa.gov NR 28 TC 13 Z9 13 U1 0 U2 3 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0022-0248 J9 J CRYST GROWTH JI J. Cryst. Growth PD DEC 15 PY 2005 VL 285 IS 4 BP 473 EP 480 DI 10.1016/j.jcrysgro.2005.09.005 PG 8 WC Crystallography; Materials Science, Multidisciplinary; Physics, Applied SC Crystallography; Materials Science; Physics GA 996HI UT WOS:000234164600005 ER PT J AU Liemohn, MW Ridley, AJ Brandt, PC Gallagher, DL Kozyra, JU Ober, DM Mitchell, DG Roelof, EC DeMajistre, R AF Liemohn, MW Ridley, AJ Brandt, PC Gallagher, DL Kozyra, JU Ober, DM Mitchell, DG Roelof, EC DeMajistre, R TI Parametric analysis of nightside conductance effects on inner magnetospheric dynamics for the 17 April 2002 storm SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID ASYMMETRIC RING CURRENT; ENERGETIC NEUTRAL ATOM; ELECTRIC-FIELD; GEOMAGNETIC STORMS; IMAGE MISSION; ENA OBSERVATIONS; MAGNETIC STORM; CURRENT IONS; MODEL; PROTON AB [1] Numerous simulations were conducted in order to quantify the influence of nightside conductance morphology and intensity on the storm-time ring current and plasmasphere. The study focused on the moderate magnetic storm of 17 April 2002. The simulation results were compared against measurements of the ring current and plasmasphere in order to assess the accuracy as a function of conductance parameter setting. In particular, three data sets were used: Dst*, plasmapause location as extracted from IMAGE EUV snapshots, and IMAGE HENA flux observations for the 39 - 60 keV energy range. While no single simulation conducted for this study proved itself to be the best overall match to the selected data sets, many things were learned from the simulations. The most important scientific finding is that there is an optimal conductance level for maximal ring current intensity. Too little conductance leads to large shielding potentials that effectively inhibit ring current growth, while too much conductance leads to continual flow-through of the hot ions with no significant hot ion accumulation in the inner magnetosphere. It was found that the poleward shift of the high conductance region of the auroral oval was the most important factor affecting the data-model comparisons. The peak intensity of the auroral oval conductance was also determined to be a significant factor affecting model accuracy. Tilting the dawnside location of the oval equatorward with respect to its duskside latitude had little effect on the results, as did the setting for the uniformly applied baseline conductance. The high-latitude boundary condition for the potential solution was also found to have little influence on the results. C1 Univ Michigan, Dept Atmospher Ocean & Space Sci, Ann Arbor, MI 48109 USA. Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. NASA, George C Marshall Space Flight Ctr, Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA. ATK Mission Res, Nashua, NH 03062 USA. RP Univ Michigan, Dept Atmospher Ocean & Space Sci, 2455 Hayward St, Ann Arbor, MI 48109 USA. EM liemohn@umich.edu RI Liemohn, Michael/H-8703-2012; Ridley, Aaron/F-3943-2011; Brandt, Pontus/N-1218-2016 OI Liemohn, Michael/0000-0002-7039-2631; Ridley, Aaron/0000-0001-6933-8534; Brandt, Pontus/0000-0002-4644-0306 NR 77 TC 39 Z9 39 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 15 PY 2005 VL 110 IS A12 AR A12S22 DI 10.1029/2005JA011109 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 998CR UT WOS:000234296100002 ER PT J AU Mandrake, L Wilson, B Wang, C Hajj, G Mannucci, A Pi, X AF Mandrake, L Wilson, B Wang, C Hajj, G Mannucci, A Pi, X TI A performance evaluation of the operational Jet Propulsion Laboratory/University of Southern California Global Assimilation Ionospheric Model (JPL/USC GAIM) SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID LOWER ATMOSPHERE; WEATHER; MIDDLE AB [1] The Jet Propulsion Laboratory/University of Southern California Global Assimilation Ionospheric Model (JPL/USCGAIM) uses two data assimilation techniques to optimally combine ionospheric measurements with the physics model: a sparse, traditional Kalman filter to estimate the three-dimensional density state, and a four-dimensional variational approach (4DVAR) to estimate ionospheric drivers such as the equatorial E x B drift or neutral winds. In this paper we study a specific implementation of the JPL/USC GAIM Kalman filter ( single ion, low-resolution, and input data from 200 ground GPS sites) and validate its global accuracy over 137 days by comparisons to independent GPS slant total electron content (TEC) observations ("missing site'' tests) and independent JASON vertical TEC observations. The assimilation accuracy is robust with a slant TEC spatial prediction RMS error of 4 TECU ( Total Electron Content Unit, 1 x 10(16) e-/m(2)) on average and a vertical TEC JASON RMS error of 7 TECU. Removing what appears to be a positive approximate to 4.4 TECU bias from the JASON observations, we obtain an improved performance of 5.3 TECU over the oceans. Comparisons with a single, thin shell global ionospheric map model and the International Reference Ionosphere and Bent ionospheric models are also provided. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ So Calif, Dept Math, Los Angeles, CA 90089 USA. RP Mandrake, L (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM lukas.mandrake@jpl.nasa.gov RI Mannucci, Anthony/A-1349-2007 OI Mannucci, Anthony/0000-0003-2391-8490 NR 32 TC 31 Z9 31 U1 1 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 15 PY 2005 VL 110 IS A12 AR A12306 DI 10.1029/2005JA011170 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 998CR UT WOS:000234296100004 ER PT J AU Mlynczak, MG Martin-Torres, FJ Crowley, G Kratz, DP Funke, B Lu, G Lopez-Puertas, M Russell, JM Kozyra, J Mertens, C Sharma, R Gordley, L Picard, R Winick, J Paxton, L AF Mlynczak, MG Martin-Torres, FJ Crowley, G Kratz, DP Funke, B Lu, G Lopez-Puertas, M Russell, JM Kozyra, J Mertens, C Sharma, R Gordley, L Picard, R Winick, J Paxton, L TI Energy transport in the thermosphere during the solar storms of April 2002 SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID 5.3 MU-M; TERRESTRIAL THERMOSPHERE; MIDDLE ATMOSPHERE; SABER EXPERIMENT; NUMERICAL-MODEL; ATOMIC OXYGEN; TEMPERATURE; IONOSPHERE; MESOSPHERE; ENERGETICS AB [1] The dramatic solar storm events of April 2002 deposited a large amount of energy into the Earth's upper atmosphere, substantially altering the thermal structure, the chemical composition, the dynamics, and the radiative environment. We examine the flow of energy within the thermosphere during this storm period from the perspective of infrared radiation transport and heat conduction. Observations from the SABER instrument on the TIMED satellite are coupled with computations based on the ASPEN thermospheric general circulation model to assess the energy flow. The dominant radiative response is associated with dramatically enhanced infrared emission from nitric oxide at 5.3 mu m from which a total of similar to 7.7 x 10(23) ergs of energy are radiated during the storm. Energy loss rates due to NO emission exceed 2200 Kelvin per day. In contrast, energy loss from carbon dioxide emission at 15 mm is only similar to 2.3% that of nitric oxide. Atomic oxygen emission at 63 mu m is essentially constant during the storm. Energy loss from molecular heat conduction may be as large as 3.8% of the NO emission. These results confirm the "natural thermostat'' effect of nitric oxide emission as the primary mechanism by which storm energy is lost from the thermosphere below 210 km. C1 NASA, Langley Res Ctr, Sci Directorate, Hampton, VA 23681 USA. AS & M Inc, Hampton, VA 23681 USA. SW Res Inst, San Antonio, TX 78228 USA. Inst Astrofis Andalucia, E-18080 Granada, Spain. Natl Ctr Atmospher Res, Boulder, CO 80307 USA. Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA. Univ Michigan, Ann Arbor, MI 48109 USA. USAF, Res Lab, Hanscom AFB, MA 01731 USA. G & A Tech Software, Newport News, VA 23606 USA. Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA. RP Mlynczak, MG (reprint author), NASA, Langley Res Ctr, Sci Directorate, 21 Langley Blvd,Mail Stop 420, Hampton, VA 23681 USA. EM m.g.mlynczak@nasa.gov RI Lu, Gang/A-6669-2011; Mlynczak, Martin/K-3396-2012; Lopez Puertas, Manuel/M-8219-2013; Funke, Bernd/C-2162-2008; Paxton, Larry/D-1934-2015; Martin-Torres, Francisco Javier/G-6329-2015 OI Lopez Puertas, Manuel/0000-0003-2941-7734; Funke, Bernd/0000-0003-0462-4702; Paxton, Larry/0000-0002-2597-347X; Martin-Torres, Francisco Javier/0000-0001-6479-2236 NR 31 TC 47 Z9 47 U1 0 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 15 PY 2005 VL 110 IS A12 AR A12S25 DI 10.1029/2005JA011141 PG 19 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 998CR UT WOS:000234296100003 ER PT J AU Tu, JN Song, P Reinisch, BW Huang, XQ Green, JL Frey, HU Reiff, PH AF Tu, JN Song, P Reinisch, BW Huang, XQ Green, JL Frey, HU Reiff, PH TI Electron density images of the middle- and high-latitude magnetosphere in response to the solar wind SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID CLEFT ION FOUNTAIN; PLASMA-DENSITY; POLAR-CAP; IONOSPHERIC ELECTRODYNAMICS; MODEL; FIELD; DEPENDENCE; ALTITUDE; SPACECRAFT; TROUGH AB [1] Electron density distributions and plasma dynamics in the middle- and high-latitude dayside magnetosphere are studied with observations from the IMAGE radio plasma imager. Remote measurements of the electron densities along magnetic field lines were made before and during a magnetic storm when the solar wind and interplanetary magnetic field ( IMF) impinging on the magnetopause varied considerably. Several regions of different density distribution characteristics, including plasmasphere, plasma trough, subauroral/auroral density depletion, density enhancements in the aurora/cusp, and polar cap, are identified in "two-dimensional images,''i.e., along the satellite orbit and field lines. The plasma dynamics, such as the plasma refilling in the outer plasmasphere and the plasma acceleration in the aurora/cusp region, are inferred from density gradients along the field lines. It is shown that the densities and locations of the plasma regions vary in accordance with the solar wind, particularly with the IMF variations for the case examined. In the partial recovery phase of the magnetic storm when the IMF was northward, the density depletion region expanded to wider latitude range and extended to lower altitudes, with much lower densities than those in the density depletion regions of the other RPI measurement periods. The density enhancements associated with the aurora/cusp region were not visible, possibly because of the diffusive nature of the dayside aurora and higher-latitude location of the cusp during this period. At the peak of the storm, characterized by a persistent southward IMF B-z, all plasma regions moved to lower L shells. The results imply that the solar wind/IMF effects should be included in any statistical study of the electron density distributions in these regions. C1 Univ Massachusetts, Ctr Atmospher Res, Lowell, MA 01854 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA. Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA. RP Tu, JN (reprint author), Univ Massachusetts, Ctr Atmospher Res, 600 Suffolk St, Lowell, MA 01854 USA. EM jiannan_tu@uml.edu RI Reiff, Patricia/D-2564-2014 OI Reiff, Patricia/0000-0002-8043-5682 NR 45 TC 9 Z9 9 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 15 PY 2005 VL 110 IS A12 AR A12210 DI 10.1029/2005JA011328 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 998CR UT WOS:000234296100007 ER PT J AU Khare, B Wilhite, P Tran, B Teixeira, E Fresquez, K Mvondo, DN Bauschlicher, C Meyyappan, M AF Khare, B Wilhite, P Tran, B Teixeira, E Fresquez, K Mvondo, DN Bauschlicher, C Meyyappan, M TI Functionalization of carbon nanotubes via nitrogen glow discharge SO JOURNAL OF PHYSICAL CHEMISTRY B LA English DT Article ID PLASMA; FLUORINATION AB We have exposed single-wall carbon nanotubes (SWCNTs) to microwave-generated N-2 plasma with the aim to functionalize the nanotubes. The results strongly depend on the distance between the discharge source and the sample, since nitrogen atoms generated can be lost due to recombination. No functionalization was observed when this distance was 7.0 cm. At intermediate distances (2.5 cm), the incorporation of nitrogen and oxygen onto the SWCNT was observed, while, at short distances (1 cm), products containing C&3bond; N were also observed. C1 NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. RP Khare, B (reprint author), NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. EM bkhare@mail.arc.nasa.gov NR 19 TC 54 Z9 55 U1 0 U2 10 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1520-6106 J9 J PHYS CHEM B JI J. Phys. Chem. B PD DEC 15 PY 2005 VL 109 IS 49 BP 23466 EP 23472 DI 10.1021/jp0537254 PG 7 WC Chemistry, Physical SC Chemistry GA 992DJ UT WOS:000233864300054 PM 16375320 ER PT J AU Sen, SY Ray, CS Reddy, RG AF Sen, SY Ray, CS Reddy, RG TI Processing of lunar soil simulant for space exploration applications SO MATERIALS SCIENCE AND ENGINEERING A-STRUCTURAL MATERIALS PROPERTIES MICROSTRUCTURE AND PROCESSING LA English DT Article; Proceedings Paper CT International Conference on Advances in Solidification Processes CY JUN 07-10, 2005 CL Stockholm, SWEDEN DE in situ resource utilization; regolith; simulant; extraction; purification; glass fabrication ID GLASSES AB NASA's long-term vision for space exploration includes developing human habitats and conducting scientific investigations on planetary bodies, especially on Moon and Mars. To reduce the level of upmass, processing and utilization of planetary in situ resources is recognized as an important element of this vision. Within this scope and context, we have undertaken a general effort aimed primarily at extracting and refining metals, developing glass, glass-ceramic or traditional ceramic type materials using lunar soil simulants. In this paper we will present the preliminary results on our effort on carbothermal reduction of oxides for elemental extraction and zone refining for obtaining high-purity metals. In addition, we will demonstrate the possibility of developing glasses from lunar soil simulant for fixing the nuclear waste from potential nuclear power generators on planetary bodies. Compositional analysis, X-ray diffraction patterns and differential thermal analysis (DTA) of processed samples are presented. (c) 2005 Elsevier B.V. All rights reserved. C1 NASA, George C Marshall Space Flight Ctr, BAE SYS, Huntsville, AL 35801 USA. Univ Alabama, Tuscaloosa, AL 35487 USA. RP Sen, SY (reprint author), NASA, George C Marshall Space Flight Ctr, BAE SYS, Huntsville, AL 35801 USA. EM s.sen@msfc.nasa.gov NR 17 TC 10 Z9 11 U1 1 U2 3 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0921-5093 J9 MAT SCI ENG A-STRUCT JI Mater. Sci. Eng. A-Struct. Mater. Prop. Microstruct. Process. PD DEC 15 PY 2005 VL 413 SI SI BP 592 EP 597 DI 10.1016/j.msea.2005.08.172 PG 6 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Science & Technology - Other Topics; Materials Science; Metallurgy & Metallurgical Engineering GA 996VI UT WOS:000234202900099 ER PT J AU Barthelmy, SD Chincarini, G Burrows, DN Gehrels, N Covino, S Moretti, A Romano, P O'Brien, PT Sarazin, CL Kouveliotou, C Goad, M Vaughan, S Tagliaferri, G Zhang, B Antonelli, LA Campana, S Cummings, JR D'Avanzo, P Davies, MB Giommi, P Grupe, D Kaneko, Y Kennea, JA King, A Kobayashi, S Melandri, A Meszaros, P Nousek, JA Patel, S Sakamoto, T Wijers, RAMJ AF Barthelmy, SD Chincarini, G Burrows, DN Gehrels, N Covino, S Moretti, A Romano, P O'Brien, PT Sarazin, CL Kouveliotou, C Goad, M Vaughan, S Tagliaferri, G Zhang, B Antonelli, LA Campana, S Cummings, JR D'Avanzo, P Davies, MB Giommi, P Grupe, D Kaneko, Y Kennea, JA King, A Kobayashi, S Melandri, A Meszaros, P Nousek, JA Patel, S Sakamoto, T Wijers, RAMJ TI An origin for short gamma-ray bursts unassociated with current star formation SO NATURE LA English DT Article ID GRB-050709; AFTERGLOW; SGR-1806-20; GALAXY; FLARE AB Two short (< 2 s) gamma-ray bursts (GRBs) have recently been localized(1-4) and fading afterglow counterparts detected(2-4). The combination of these two results left unclear the nature of the host galaxies of the bursts, because one was a star-forming dwarf, while the other was probably an elliptical galaxy. Here we report the X-ray localization of a short burst (GRB 050724) with unusual gamma-ray and X-ray properties. The X-ray afterglow lies off the centre of an elliptical galaxy at a redshift of z = 0.258 (ref. 5), coincident with the position determined by ground-based optical and radio observations(6-8). The low level of star formation typical for elliptical galaxies makes it unlikely that the burst originated in a supernova explosion. A supernova origin was also ruled out for GRB 050709 ( refs 3, 31), even though that burst took place in a galaxy with current star formation. The isotropic energy for the short bursts is 2 - 3 orders of magnitude lower than that for the long bursts. Our results therefore suggest that an alternative source of bursts - the coalescence of binary systems of neutron stars or a neutron star-black hole pair - are the progenitors of short bursts. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. INAF, Osservatorio Astron Brera, I-23807 Merate, Italy. Univ Studi Milano Bicocca, I-20126 Milan, Italy. Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. Univ Leicester, Dept Phys & Astron, Leicester LE1 7RH, Leics, England. Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. NASA, George C Marshall Space Flight Ctr, NSSTC, Huntsville, AL 35805 USA. Univ Nevada, Dept Phys, Las Vegas, NV 89154 USA. Osserv Astron Roma, I-00040 Monte Porzio Catone, Italy. CNR, Washington, DC 20418 USA. Univ Studi Insubria, Dipartimento Matemat & Fis, I-22100 Como, Italy. Lund Observ, SE-22100 Lund, Sweden. ASI Sci Data Ctr, I-00044 Frascati, Italy. NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, NSSTC, Huntsville, AL 35805 USA. Penn State Univ, Dept Phys, University Pk, PA 16802 USA. Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. RP Barthelmy, SD (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM scott@lheamail.gsfc.nasa.gov RI Gehrels, Neil/D-2971-2012; Barthelmy, Scott/D-2943-2012; OI Campana, Sergio/0000-0001-6278-1576; giommi, paolo/0000-0002-2265-5003; Wijers, Ralph/0000-0002-3101-1808; moretti, alberto/0000-0002-9770-0315 NR 30 TC 260 Z9 263 U1 0 U2 4 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD DEC 15 PY 2005 VL 438 IS 7070 BP 994 EP 996 DI 10.1038/nature04392 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 993EC UT WOS:000233934600061 PM 16355219 ER PT J AU Ksendzov, A Lin, Y AF Ksendzov, A Lin, Y TI Integrated optics ring-resonator sensors for protein detection SO OPTICS LETTERS LA English DT Article ID MICROCAVITY; COUPLERS AB Using an integrated optics ring-resonator biosensor, we have demonstrated the detection of protein in low concentrations. We detected 0.3 nM of avidin in a buffered saline solution; the calculated detection limit is 0.1 nM (6.8 ng/ml) for avidin, which compares favorably with those of other optical protein detection techniques. Further improvement is possible. Our ring resonator utilizes SixNy/SiO2 waveguides, which, owing to evanescent field interaction, change the effective refractive index when target molecules are immobilized on their surfaces. The selectivity of the sensor depends on the biotin surface coating, which causes the specific binding and immobilization of avidin. (c) 2005 Optical Society of America. 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. EM alexander.ksendzov@jpl.nasa.gov NR 11 TC 154 Z9 159 U1 1 U2 21 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 0146-9592 J9 OPT LETT JI Opt. Lett. PD DEC 15 PY 2005 VL 30 IS 24 BP 3344 EP 3346 DI 10.1364/OL.30.003344 PG 3 WC Optics SC Optics GA 991PX UT WOS:000233827000028 PM 16389826 ER PT J AU Pandey, RB Gettrust, JF AF Pandey, RB Gettrust, JF TI Flow response of a segregating mixture by interacting lattice gas simulation SO PHYSICA A-STATISTICAL MECHANICS AND ITS APPLICATIONS LA English DT Article DE lattice gas; mixture; segregation; non-equilibrium steady state; linear response ID PHASE-SEPARATION; HYDRATE; METHANE; FLUID AB Steady-state flow and structural profiles of immiscible components A and B (molecular weights M-A and M-B, M-A < M-B) in a non-conservative open system are studied by an interacting lattice gas Monte Carlo simulation. Concentration gradient and hydrostatic bias H drive the constituents (A,B) which are continuously released from the bottom with equal probability against gravity. At low bias, the segregation of A and B leading to a partial layering is enhanced toward the bottom. The longitudinal density profile with a high density in the bottom region and low toward the top shows linear, exponential, and power-law decays in different regions of depth or altitude which varies systematically with the pressure bias. The transverse density profiles show segregation with different domain sizes and layering depending on the bias. Response of their steady-state flux density j to the hydrostatic bias H is found to be linear at higher bias. The difference in response of the flux density of the two components becomes more pronounced at low bias and higher miscibility gap. Published by Elsevier B.V. C1 USN, Res Lab, Stennis Space Ctr, Stennis Space Ctr, MS 39529 USA. Univ So Mississippi, Dept Phys & Astron, Hattiesburg, MS 39406 USA. RP Pandey, RB (reprint author), USN, Res Lab, Stennis Space Ctr, Stennis Space Ctr, MS 39529 USA. EM ras.pandey@usm.edu NR 35 TC 3 Z9 3 U1 0 U2 0 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0378-4371 EI 1873-2119 J9 PHYSICA A JI Physica A PD DEC 15 PY 2005 VL 358 IS 2-4 BP 437 EP 446 DI 10.1016/j.physa.2005.03.060 PG 10 WC Physics, Multidisciplinary SC Physics GA 980BC UT WOS:000232987900015 ER PT J AU Kletetschka, G Connerney, JEP Acuna, MH Wasilewski, PJ Ness, NF AF Kletetschka, G Connerney, JEP Acuna, MH Wasilewski, PJ Ness, NF TI Reply to the comment on the paper "Grain size dependent potential for self generation of magnetic anomalies on Mars via thermoremanent magnetic acquisition and magnetic interaction of hematite and magnetite" by Gunther Kletetschka, Norman F. Ness, J.E.P. Connerney, M.H. Acuna, P.J. Wasilewski, Phys. Earth Planet. Inter. 148 (2005) 149-156, made by: Jafar Arkani-Hamed SO PHYSICS OF THE EARTH AND PLANETARY INTERIORS LA English DT Letter C1 Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. Acad Sci Czech Republ, Inst Geol, Prague, Czech Republic. NASA, Goddard Space Flight Ctr, Dept Extra Terr Phys, Greenbelt, MD 20771 USA. Univ Delaware, Bartol Res Inst, Newark, DE 19716 USA. RP Kletetschka, G (reprint author), Catholic Univ Amer, Dept Phys, Washington, DC 20064 USA. EM Gunther.Kletetschka@gsfc.nasa.gov RI Kletetschka, Gunther/C-9996-2011; connerney, john/I-5127-2013 OI Kletetschka, Gunther/0000-0002-0645-9037; NR 6 TC 0 Z9 0 U1 0 U2 8 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0031-9201 J9 PHYS EARTH PLANET IN JI Phys. Earth Planet. Inter. PD DEC 15 PY 2005 VL 153 IS 4 BP 238 EP 239 DI 10.1016/j.pepi.2005.05.004 PG 2 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 991TQ UT WOS:000233837300008 ER PT J AU Chandrasekhar, P Zay, BJ McQueeney, T Birur, GC Sitaram, V Menon, R Coviello, M Elsenbaumer, RL AF Chandrasekhar, P Zay, BJ McQueeney, T Birur, GC Sitaram, V Menon, R Coviello, M Elsenbaumer, RL TI Physical, chemical, theoretical aspects of conducting polymer electrochromics in the visible, IR and microwave regions SO SYNTHETIC METALS LA English DT Article; Proceedings Paper CT International Conference on Science and Technology of Synthetic Metals CY JUN 28-JUL 02, 2004 CL Wollongong, AUSTRALIA DE conducting; polymer; infrared; electrochromic; spacecraft AB Conducting polymers (CPs) display strong electrochromism across the visible, near-IR (NIR), IR and even microwave spectral regions. Applications range from military to space. However, a fundamental understanding of the phenomena behind this electrochromism, the charge carrier(s) responsible, and the relation of nanoscopic morphology and electrochemical properties to the electrochromism, still remains lacking. This paper takes a first step at such a correlation, mining a wealth of data accumulated over the course of many years by our group. Expected findings are that certain population states contribute predominantly to certain spectral regions (e.g. bipolaron states to the IR, the valence band to the visible and other mid-gap states to the microwave). Among more specific findings, a prominent 7 mu m (0.16 eV) peak in MR devices is ascribed to bipolarons, whilst a low-energy transition at 0.054 eV is ascribed to inter/intra-chain transitions. Other findings point to the potential design of very broad-band electrochromic systems encompassing the visible through microwave regions. (C) 2005 Elsevier B.V. All rights reserved. C1 Ashwin Ushas Corp Inc, Lakewood, NJ 08701 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Indian Inst Sci, Dept Phys, Bangalore 380001, Karnataka, India. Univ Texas, Dept Mat Sci & Engn, Arlington, TX 76019 USA. RP Chandrasekhar, P (reprint author), Ashwin Ushas Corp Inc, 500 James St,Ste 7, Lakewood, NJ 08701 USA. EM chandra.p@ashwin-ushas.com RI Sitaram, V/B-9340-2008 NR 6 TC 25 Z9 27 U1 0 U2 9 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0379-6779 J9 SYNTHETIC MET JI Synth. Met. PD DEC 15 PY 2005 VL 155 IS 3 BP 623 EP 627 DI 10.1016/j.synthemt.2005.08.015 PG 5 WC Materials Science, Multidisciplinary; Physics, Condensed Matter; Polymer Science SC Materials Science; Physics; Polymer Science GA 996PE UT WOS:000234185700031 ER PT J AU Tan, B Hu, JN Huang, D Yang, WZ Zhang, P Shabanov, NV Knyazikhin, Y Nemani, RR Myneni, RB AF Tan, B Hu, JN Huang, D Yang, WZ Zhang, P Shabanov, NV Knyazikhin, Y Nemani, RR Myneni, RB TI Assessment of the broadleaf crops leaf area index product from the Terra MODIS instrument SO AGRICULTURAL AND FOREST METEOROLOGY LA English DT Article DE broadleaf crops; leaf area index; terra MODIS instrument ID ABSORBED PAR; LAND-COVER; LAI; VALIDATION; ALGORITHM; FRACTION; KALAHARI; AFRICA AB The first significant processing of Terra MODIS data, called Collection 3, covered the period from November 2000 to December 2002. The Collection 3 leaf area index (LAI) and fraction vegetation absorbed photosynthetically active radiation (FPAR) products for broadleaf crops exhibited three anomalies (a) high LAI values during the peak growing season, (b) differences in LAI seasonality between the radiative transfer-based main algorithm and the vegetation index based back-up algorithm, and (c) too few retrievals from the main algorithm during the summer period when the crops are at full flush. The cause of these anomalies is a mismatch between reflectances modeled by the algorithm and MODIS measurements. Therefore, the Look-Up-Tables accompanying the algorithm were revised and implemented in Collection 4 processing. The main algorithm with the revised Look-Up-Tables generated retrievals for over 80% of the pixels with valid data. Retrievals from the back-up algorithm, although few, should be used with caution as they are generated from surface reflectances with high uncertainties. (c) 2005 Elsevier B.V. All rights reserved. C1 Boston Univ, Dept Geog, Boston, MA 02215 USA. NASA, Ames Res Ctr, Ecosyst Sci & Technol Branch, Moffett Field, CA 94035 USA. RP Tan, B (reprint author), Boston Univ, Dept Geog, Boston, MA 02215 USA. EM tanbin@crsa.bu.edu RI Yang, Wenze/B-8356-2012; Zhang, Ping/D-7257-2012; Tan, Bin/G-1331-2012; Huang, Dong/H-7318-2014; Myneni, Ranga/F-5129-2012 OI Yang, Wenze/0000-0001-8514-2742; Huang, Dong/0000-0001-9715-6922; NR 17 TC 35 Z9 35 U1 0 U2 6 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-1923 J9 AGR FOREST METEOROL JI Agric. For. Meteorol. PD DEC 14 PY 2005 VL 135 IS 1-4 BP 124 EP 134 DI 10.1016/j.agrformet.2005.10.008 PG 11 WC Agronomy; Forestry; Meteorology & Atmospheric Sciences SC Agriculture; Forestry; Meteorology & Atmospheric Sciences GA 021WY UT WOS:000236017800011 ER PT J AU Borak, JS Jasinski, MF Crago, RD AF Borak, JS Jasinski, MF Crago, RD TI Time series vegetation aerodynamic roughness fields estimated from modis observations SO AGRICULTURAL AND FOREST METEOROLOGY LA English DT Article DE aerodynamic roughness; MODIS; time series; southern great plains ID GENERAL-CIRCULATION MODELS; ZERO-PLANE DISPLACEMENT; COMMUNITY CLIMATE MODEL; SATELLITE DATA; AREA INDEX; LEAF-AREA; LAND; CANOPY; HEIGHT; LENGTH AB Most land surface models used today require estimates of aerodynamic roughness length in order to characterize momentum transfer between the surface and atmosphere. The most common method of prescribing roughness is through the use of empirical look-up tables based solely on land cover class. Theoretical approaches that employ satellite-based estimates of canopy density present an attractive alternative to current look-up table approaches based on vegetation cover type that do not account for within-class variability and are often times simplistic with respect to temporal variability. The current research applies Raupach's formulation of momentum aerodynamic roughness to MODIS data on a regional scale in order to estimate seasonally variable roughness and zero-plane displacement height fields using bulk land cover parameters estimated by [Jasinski, M.F., Borak, J., Crago, R., 2005. Bulk surface momentum parameters for satellite-derived vegetation fields. Agric. For. Meteorol. 133, 55-68]. Results indicate promising advances over look-up approaches with respect to characterization of vegetation roughness variability in land surface and atmospheric circulation models. (c) 2006 Published by Elsevier B.V. C1 NASA, Goddard Space Flight Ctr, SSAI, Hydrol Sci Branch, Greenbelt, MD 20771 USA. NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA. Bucknell Univ, Dept Civil & Environm Engn, Lewisburg, PA 17837 USA. RP Borak, JS (reprint author), NASA, Goddard Space Flight Ctr, SSAI, Hydrol Sci Branch, Code 614-3, Greenbelt, MD 20771 USA. EM borak@hsb.gsfc.nasa.gov; Michael.Flasinski.1@gsfc.nasa.gov; rcrago@bucknell.edu NR 29 TC 14 Z9 16 U1 1 U2 13 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-1923 J9 AGR FOREST METEOROL JI Agric. For. Meteorol. PD DEC 14 PY 2005 VL 135 IS 1-4 BP 252 EP 268 DI 10.1016/j.agroformet.2005.12.006 PG 17 WC Agronomy; Forestry; Meteorology & Atmospheric Sciences SC Agriculture; Forestry; Meteorology & Atmospheric Sciences GA 021WY UT WOS:000236017800022 ER PT J AU Sasai, T Ichii, K Yamaguchi, Y Nemani, R AF Sasai, Takahiro Ichii, Kazuhito Yamaguchi, Yasushi Nemani, Ramakrishna TI Simulating terrestrial carbon fluxes using the new biosphere model "biosphere model integrating eco-physiological and mechanistic approaches using satellite data" (BEAMS) SO JOURNAL OF GEOPHYSICAL RESEARCH-BIOGEOSCIENCES LA English DT Article ID NET PRIMARY PRODUCTION; PRIMARY PRODUCTIVITY NPP; COMPARING GLOBAL-MODELS; GAP FILLING STRATEGIES; LIGHT-USE EFFICIENCY; LEAF-AREA INDEX; INTERANNUAL VARIABILITY; STOMATAL CONDUCTANCE; ECOSYSTEM EXCHANGE; DECIDUOUS FOREST AB In this study we present a new biosphere model called the Biosphere model integrating Eco-physiological And Mechanistic approaches using Satellite data (BEAMS). BEAMS provides a new method of calculating the environmental stress affecting plant growth (Stress). Stress is calculated eco-physiologically using a photosynthesis model and stomatal conductance formulation, providing a more realistic result than previous models. Stress values are used to estimate Gross Primary Production (GPP) estimates via the light use efficiency concept. We used BEAMS, including our new Stress approach, to investigate global spatial and temporal patterns of net primary production (NPP) and net ecosystem production (NEP). BEAMS was run for the years 1982-2000 using global scale satellite and climate data. Comparison of model results with observational measurements at flux sites reveals that GPP values predicted by BEAMS agree with measured GPP. Obtained Stress values were compared with those of MOD17 and CASA; the three methods produce contrasting spatial patterns. Upon comparing predicted and observed NPP, the pattern of NPP for each plant functional type can be adequately estimated. In terms of trend analysis, NPP increased for the years 1982-2000 in most regions. Different NPP trends were observed in Europe, Russia, and northeast Canada than those proposed by Nemani et al. (2003); we attribute these differences to climate-related processes. Simulated interannual variations in global NEP are similar to results from inverse modeling. A sensitivity study of obtained NEP shows that the interannual variability in NEP is strongly controlled by air temperature, precipitation, CO(2), and the fraction of absorbed photosynthetically active radiation. C1 Nagoya Univ, Dept Earth & Environm Sci, Nagoya, Aichi, Japan. San Jose State Univ, Dept Geog, San Jose, CA 95192 USA. NASA, Ames Res Ctr, Moffett Field, CA USA. RP Sasai, T (reprint author), Nagoya Univ, Dept Earth & Environm Sci, Nagoya, Aichi, Japan. EM sasai@system.eps.nagoya-u.ac.jp; kichii@arc.nasa.gov; yasushi@nagoya-u.jp; ramakrishna.r.nemani@nasa.gov RI Ichii, Kazuhito/D-2392-2010; Sasai, Takahiro/E-6417-2011 OI Ichii, Kazuhito/0000-0002-8696-8084; NR 74 TC 29 Z9 32 U1 3 U2 11 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-BIOGEO JI J. Geophys. Res.-Biogeosci. PD DEC 14 PY 2005 VL 110 IS G2 AR G02014 DI 10.1029/2005JG000045 PG 18 WC Environmental Sciences; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Geology GA 090WS UT WOS:000240984900001 ER PT J AU Jiang, X Jones, DBA Shia, R Waliser, DE Yung, YL AF Jiang, X Jones, DBA Shia, R Waliser, DE Yung, YL TI Spatial patterns and mechanisms of the quasi-biennial oscillation - annual beat of ozone SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID NORTHERN-HEMISPHERE; EQUATORIAL STRATOSPHERE; TROPICAL STRATOSPHERE; 2-DIMENSIONAL MODEL; SOLAR-CYCLE; GLOBAL QBO; CIRCULATION; MODULATION; TRANSPORT; WINTER AB An idealized two-dimensional chemistry and transport model is used to investigate the spatial patterns of, and mechanism for, the quasi-biennial oscillation-annual beat (QBO-AB) signal in ozone in the tropics and subtropics. Principal component analysis is applied to the detrended, deseasonalized, and filtered total column ozone anomaly from the standard model. The first two empirical orthogonal functions (EOFs) capture over 98.5% of the total variance. The first EOF, accounting for 70.3% of the variance, displays a structure attributable to the approximately symmetric QBO with a period of 28 months. The second EOF, capturing 28.2% of the variance, is related to the QBO-AB around 20 months. An extended EOF analysis reveals the characteristic pattern of the downward propagation of QBO and upward propagation of QBO-AB. The model results are compared to those from the merged ozone data. Sensitivity experiments indicate that the QBO-AB is produced primarily as a result of the dynamical QBO-AB in the mean meridional circulation and by the interaction between the QBO and the annual cycle in transport, each contributing roughly equally to the forcing of QBO-AB. The interaction between the QBO in the transport fields and the annual cycle in chemistry plays a minor role. C1 CALTECH, Dept Environm Sci & Engn, Pasadena, CA 91125 USA. CALTECH, Div Geol & Planetary Sci, Pasadena, CA 91125 USA. Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada. CALTECH, Jet Prop Lab, Div Sci, Pasadena, CA 91109 USA. RP Jiang, X (reprint author), CALTECH, Dept Environm Sci & Engn, MS 150-21, Pasadena, CA 91125 USA. EM xun@gps.caltech.edu RI Jones, Dylan/O-2475-2014 OI Jones, Dylan/0000-0002-1935-3725 NR 38 TC 9 Z9 10 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 13 PY 2005 VL 110 IS D23 AR D23308 DI 10.1029/2005JD006055 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 998BU UT WOS:000234293700002 ER PT J AU Glazman, RE Golubev, YN AF Glazman, RE Golubev, YN TI Variability of the ocean-induced magnetic field predicted at sea surface and at satellite altitudes SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID ATLANTIC CIRCULATION MODELS; ELECTROMAGNETIC-FIELDS; TRANSPORT; VOLTAGES; SIGNALS; FLOW AB [1] Spatial and temporal variability of the magnetic field component induced by ocean circulation is investigated on the basis of a standard thin-shell approximation of electro- and magneto-static equations. Well-known difficulties of numerical solution of the governing equations are resolved by reducing the problem to an equation for the electric field potential, Phi, as opposed to a more conventional approach focused on the vertical jump, psi, of the magnetic field potential across a combined ocean/ marine-sediment-layer spherical shell. The present formulation permits using more realistic input data on ocean currents and ultimately yields much greater ( by at least an order of magnitude) values of the magnetic field at sea surface than predicted in earlier studies. Such large values are comparable to, and in some cases exceed, magnetic field variations caused by lithospheric and ionospheric sources on monthly to interannual timescales. At the 400-km altitude ( of CHAMP satellite), the field attains 6 nT. The model predictions show favorable comparisons with some in situ measurements as well as with Challenging Minisatellite Payload (CHAMP) satellite magnetometer data. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Raytheon ITSS, Pasadena, CA 91101 USA. RP Glazman, RE (reprint author), CALTECH, Jet Prop Lab, M-S 300-323,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM reg@pacific.jpl.nasa.gov NR 22 TC 5 Z9 5 U1 2 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD DEC 13 PY 2005 VL 110 IS C12 AR C12011 DI 10.1029/2005JC002926 PG 13 WC Oceanography SC Oceanography GA 998CF UT WOS:000234294900005 ER PT J AU Khazanov, GV Krivorutsky, E Sheldon, RB AF Khazanov, GV Krivorutsky, E Sheldon, RB TI Solid and grid sphere current collection in view of the tethered satellite system TSS 1 and TSS 1R mission results SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID ELECTRODES; PRESHEATH; ORBIT; PROBE AB Passive end body plasma contactors have been operationally validated in space and have been shown to provide a simple, effective, and robust means of current collection at the positive terminal of an electrodynamic tether system. A grid sphere has been suggested as a possible end body since it potentially has distinct advantages compared to a solid sphere, including a lower neutral dynamic drag and a higher current-to-mass ratio. This paper estimates the maximum current collected by a grid sphere, taking into account its orbital motion and ion production inside the grid sphere. We first review the data from the tethered satellite system (TSS 1) and the TSS 1R flights, formulate a model for current collection by a solid sphere, and suggest how to incorporate it into the grid sphere current collection estimate. Then we calculate the potential distribution inside the grid sphere and the potential distribution outside the solid sphere for the same system parameters. Finally, we estimate the maximum current collected by a grid sphere depending on its transparency. C1 NASA, Natl Space Sci & Technol Ctr, George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA. RP Khazanov, GV (reprint author), NASA, Natl Space Sci & Technol Ctr, George C Marshall Space Flight Ctr, Huntsville, AL 35805 USA. EM george.khazanov@msfc.nasa.gov NR 16 TC 3 Z9 3 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 13 PY 2005 VL 110 IS A12 AR A12304 DI 10.1029/2005JA011100 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 998CO UT WOS:000234295800003 ER PT J AU Bloemhof, EE AF Bloemhof, EE TI Achromatic four-quadrant phase mask (FQPM) coronagraphy using natural beam splitter phase shifts SO OPTICS EXPRESS LA English DT Article ID ADAPTIVE OPTICS; PERFORMANCE; DISPERSION; PLANETS AB The four-quadrant phase mask (FQPM) is an exciting new approach to coronagraphy, a classic astronomical technique for detecting faint companions very close to bright stars. Starlight rejection is potentially very high, and inner working distances are substantially smaller than those achieved with classical Lyot coronagraphy. The key component of the original FQPM scheme is a transparent mask divided into quadrants delivering relative phase shifts alternately 0/pi/0/pi, inserted in an intermediate focal plane of the telescope. Monochromatic masks of this kind have been successfully demonstrated in laboratory and telescope tests. Fabrication of masks with achromatic p phase shifts is challenging but of great interest for optimum astronomical sensitivity. In this paper I present a novel concept for achromatic FQPM operation that utilizes intrinsic phase relationships between transmitted and reflected beams in a dielectric beam splitter. (c) 2005 Optical Society of America. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91101 USA. RP Bloemhof, EE (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91101 USA. EM Eric.E.Bloemhof@jpl.nasa.gov NR 20 TC 5 Z9 5 U1 0 U2 1 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1094-4087 J9 OPT EXPRESS JI Opt. Express PD DEC 12 PY 2005 VL 13 IS 25 BP 10055 EP 10060 DI 10.1364/OPEX.13.010055 PG 6 WC Optics SC Optics GA 993RB UT WOS:000233971500013 PM 19503217 ER PT J AU Ward-Thompson, D Ade, PAR Araujo, H Coulson, I Cox, J Davis, GR Evans, R Griffin, MJ Gear, WK Hargrave, P Hargreaves, P Hayton, D Kiernan, BJ Leeks, SJ Mauskopf, P Naylor, D Potter, N Rinehart, SA Sudiwala, R Tucker, CR Walker, RJ Watkin, SL AF Ward-Thompson, D Ade, PAR Araujo, H Coulson, I Cox, J Davis, GR Evans, R Griffin, MJ Gear, WK Hargrave, P Hargreaves, P Hayton, D Kiernan, BJ Leeks, SJ Mauskopf, P Naylor, D Potter, N Rinehart, SA Sudiwala, R Tucker, CR Walker, RJ Watkin, SL TI First ground-based 200-mu m observing with THUMPER on JCMT - sky characterization and planet maps SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE instrumentation : photometers; techniques : photometric; infrared : solar system; submillimetre ID FOURIER-TRANSFORM SPECTROMETER; WAVE ATMOSPHERIC OPACITY; GROUND-BASED ASTRONOMY; PAMPA LA BOLA; MILLIMETER OBSERVATIONS; FTS MEASUREMENTS; SOUTH-POLE; SUBMILLIMETER; PHOTOMETER; TELESCOPE AB We present observations that were carried out with the Two HUndred Micron PhotometER (THUMPER) mounted on the James Clerk Maxwell Telescope (JCMT) in Hawaii, at a wavelength of 200 mu m (frequency 1.5 THz). The observations utilize a small atmospheric window that opens up at this wavelength under very dry conditions at high-altitude observing sites. The atmosphere was calibrated using the sky-dipping method and a relation was established between the optical depth, tau, at 1.5 THz and that at 225 GHz: tau(1.5 THz)= (95 +/- 10) x tau(225 GHz). Mars and Jupiter were mapped from the ground at this wavelength for the first time, and the system characteristics measured. A noise-equivalent flux density (NEFD) of similar to 65 +/- 10 Jy (1 sigma 1s) was measured for the THUMPER-JCMT combination, consistent with predictions based upon our laboratory measurements. The main beam resolution of 14 arcsec was confirmed and an extended error beam detected at roughly two-thirds of the magnitude of the main beam. Measurements of the Sun allow us to estimate that the fraction of the power in the main beam is similar to 15 per cent, consistent with predictions based on modelling the dish surface accuracy. It is therefore shown that the sky over Mauna Kea is suitable for astronomy at this wavelength under the best conditions. However, higher or drier sites should have a larger number of useable nights per year. C1 Cardiff Univ, Dept Phys & Astron, Cardiff CF24 3YB, Wales. Univ London Imperial Coll Sci & Technol, Blackett Lab, London SW7 2BW, England. Joint Astron Ctr, Hilo, HI 96720 USA. Univ Glamorgan, Pontypridd CF37 1DL, M Glam, Wales. European Space Astron Ctr, Madrid 28080, Spain. Univ Lethbridge, Dept Phys, Lethbridge, AB T1K 3M4, Canada. Goddard Space Flight Ctr, Astron & Solar Phys Lab, Washington, DC USA. RP Ward-Thompson, D (reprint author), Cardiff Univ, Dept Phys & Astron, 5 The Parade, Cardiff CF24 3YB, Wales. EM Derek.Ward-Thompson@astro.cf.ac.uk OI Araujo, Henrique/0000-0002-5972-2783 NR 25 TC 4 Z9 4 U1 0 U2 0 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC 11 PY 2005 VL 364 IS 3 BP 843 EP 848 DI 10.1111/j.1365-2966.2005.09625.x PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 987PR UT WOS:000233530300009 ER PT J AU Lyapustin, A Wang, YJ AF Lyapustin, A Wang, YJ TI Parameterized code SHARM-3D for radiative transfer over inhomogeneous surfaces SO APPLIED OPTICS LA English DT Article ID ATMOSPHERE; REFLECTION; ALBEDO; SYSTEM; BRDF AB The code SHARM-3D, developed for fast and accurate simulations of the monochromatic radiance at the top of the atmosphere over spatially variable surfaces with Lambertian or anisotropic reflectance, is described. The atmosphere is assumed to be laterally uniform across the image and to consist of two layers with aerosols contained in the bottom layer. The SHARM-3D code performs simultaneous calculations for all specified incidence-view geometries and multiple wavelengths in one run. The numerical efficiency of the current version of code is close to its potential limit and is achieved by means of two innovations. The first is the development of a comprehensive precomputed lookup table of the three-dimensional atmospheric optical transfer function for various atmospheric conditions. The second is the use of a linear kernel model of the land surface bidirectional reflectance factor (BRF) in our algorithm that has led to a fully parameterized solution in terms of the surface BRF parameters. The code is also able to model inland lakes and rivers. The water pixels are described with the Nakajima-Tanaka BRF model of wind-roughened water surface with a Lambertian offset, which is designed to model approximately the reflectance of suspended matter and of a shallow lake or river bottom. (c) 2005 Optical Society of America. C1 Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol, Baltimore, MD 21228 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Lyapustin, A (reprint author), Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol, Baltimore, MD 21228 USA. EM alyapust@pop900.gsfc.nasa.gov RI Lyapustin, Alexei/H-9924-2014 OI Lyapustin, Alexei/0000-0003-1105-5739 NR 18 TC 13 Z9 13 U1 3 U2 4 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 DEC 10 PY 2005 VL 44 IS 35 BP 7602 EP 7610 DI 10.1364/AO.44.007602 PG 9 WC Optics SC Optics GA 994EC UT WOS:000234012400013 PM 16363785 ER PT J AU Markowitz, A AF Markowitz, A TI X-ray variability characteristics of the Seyfert 1 galaxy NGC 3783 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (NGC 3783); galaxies : Seyfert; X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; BLACK-HOLE CANDIDATES; QUASI-PERIODIC OSCILLATIONS; CYGNUS X-1; SPECTRAL VARIABILITY; XMM-NEWTON; TIME-LAGS; GX 339-4; APERIODIC VARIABILITY; ACCRETION DISCS AB We have characterized the energy-dependent X-ray variability properties of the Seyfert 1 galaxy NGC 3783 using archival XMM-Newton and Rossi X-Ray Timing Explorer data. The high-frequency fluctuation power spectral density function (PSD) slope is consistent with flattening toward higher energies. Light-curve cross-correlation functions yield no significant lags, but peak coefficients generally decrease as energy separation of the bands increases on both short and long timescales. We have measured the coherence between various X-ray bands over the temporal frequency range of 6; 10(-8) -1; 10(-4) Hz; this range includes the temporal frequency of the low-frequency PSD break tentatively detected by Markowitz et al. and includes the lowest temporal frequency over which coherence has been measured in any active galactic nucleus to date. Coherence is generally near unity at these temporal frequencies, although it decreases slightly as energy separation of the bands increases. Temporal frequency-dependent phase lags are detected on short timescales; phase lags are consistent with increasing as energy separation increases or as temporal frequency decreases. All of these results are similar to those obtained previously for several Seyfert galaxies and stellar mass black hole systems. Qualitatively, these results are consistent with the variability models of Kotov et al. and Lyubarskii, wherein the X-ray variability is due to inwardly propagating variations in the local mass accretion rate. C1 NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Greenbelt, MD 20771 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 NR 70 TC 17 Z9 17 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 DEC 10 PY 2005 VL 635 IS 1 BP 180 EP 197 DI 10.1086/497261 PN 1 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993CF UT WOS:000233929600016 ER PT J AU Ebisawa, K Tsujimoto, M Paizis, A Hamaguchi, K Bamba, A Cutri, R Kaneda, H Maeda, Y Sato, G Senda, A Ueno, M Yamauchi, S Beckmann, V Courvoisier, TJL Dubath, P Nishihara, E AF Ebisawa, K Tsujimoto, M Paizis, A Hamaguchi, K Bamba, A Cutri, R Kaneda, H Maeda, Y Sato, G Senda, A Ueno, M Yamauchi, S Beckmann, V Courvoisier, TJL Dubath, P Nishihara, E TI Chandra deep X-ray observation of a typical galactic plane region and near-infrared identification SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; Galaxy : structure; X-rays : stars ID CCD IMAGING SPECTROMETER; ALL-SKY SURVEY; CATACLYSMIC VARIABLES; IRON LINE; INTERSTELLAR-MEDIUM; MOLECULAR CLOUDS; AX J1843.8-0352; INNER GALAXY; MILKY-WAY; EMISSION AB Using the Chandra Advanced CCD Imaging Spectrometer Imaging array (ACIS-I), we have carried out a deep hard X-ray observation of the Galactic plane region at (l, b) approximate to (28 degrees.5, 0 degrees.0), where no discrete X-ray source had been reported previously. We have detected 274 new point X-ray sources ( 4 sigma confidence), as well as strong Galactic diffuse emission within two partially overlapping ACIS-I fields (similar to 250 arcmin(2) in total). The point-source sensitivity was similar to 3 x 10(-15) ergs s(-1) cm(-2) in the hard X-ray band (2-10 keV) and similar to 2 x 10(-16) ergs s(-1) cm(-2) in the soft band (0.5-2 keV). The sum of all the detected point-source fluxes accounts for only similar to 10% of the total X- ray flux in the field of view. Even hypothesizing a new population of much dimmer and numerous Galactic point sources, the total observed X- ray flux cannot be explained. Therefore, we conclude that X- ray emission from the Galactic plane has a truly diffuse origin. Removing point sources brighter than similar to 3 x 10(-15) ergs s(-1) cm(-2) (2-10 keV), we have determined the Galactic diffuse X-ray flux to be 6.5 x 10(-11) ergs s(-1) cm(-2) deg(-2) (2-10 keV). Only 26 point sources were detected in both the soft and hard bands, indicating that there are two distinct classes of X- ray sources distinguished by their spectral hardness ratios. The surface number density of the hard sources is only slightly higher than that measured at the high Galactic latitude regions, indicating that the majority of the hard sources are background AGNs. Following up the Chandra observation, we have performed a near-infrared (NIR) survey with SofI at ESO/NTT. Almost all the soft X- ray sources have been identified in the NIR, and their spectral types are consistent with main-sequence stars, suggesting that most of them are nearby X- ray-active stars. On the other hand, only 22% of the hard sources had NIR counterparts, which are presumably Galactic. From X- ray and NIR spectral study, they are most likely to be quiescent cataclysmic variables. Our observation suggests a population of greater than or similar to 10(4) cataclysmic variables in the entire Galactic plane fainter than similar to 2 x 10(33) ergs s(-1). We have carried out a precise spectral study of the Galactic diffuse X- ray emission excluding the point sources. Confirming previous results, we have detected prominent emission lines from highly ionized heavy elements in the diffuse emission. In particular, the central energy of the iron emission line was determined to be 6.52(-0.14)(+0.08) keV ( 90% confidence), which is significantly lower than what is expected from a plasma in thermal equilibrium. The downward shift of the iron line center energy suggests nonequilibrium ionization states of the plasma or the presence of a nonthermal process to produce 6.4 keV fluorescent lines. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland. Penn State Univ, Dept Astron & Astrophys, University Pk, PA 16802 USA. IASF, Sez Milano, I-20133 Milan, Italy. RIKEN, Inst Phys & Chem Res, Cosm Radiat Lab, Wako, Saitama 3510198, Japan. CALTECH, IPAC, Pasadena, CA 91125 USA. JAXA, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan. Kyoto Univ, Dept Phys, Sakyo Ku, Kyoto 6068502, Japan. Iwate Univ, Fac Humanities & Social Sci, Iwate 0208550, Japan. Observ Geneva, CH-1290 Sauverny, Switzerland. Gunma Astron Observ, Takayama, Gunma 3770702, Japan. RP Ebisawa, K (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA. EM ebisawa@milkyway.gsfc.nasa.gov OI Paizis, Adamantia/0000-0001-5067-0377 NR 58 TC 77 Z9 77 U1 0 U2 2 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 DEC 10 PY 2005 VL 635 IS 1 BP 214 EP 242 DI 10.1086/497284 PN 1 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993CF UT WOS:000233929600018 ER PT J AU Brandl, BR Clark, DM Eikenberry, SS Wilson, JC Henderson, CP Barry, DJ Houck, JR Carson, JC Hayward, TL AF Brandl, BR Clark, DM Eikenberry, SS Wilson, JC Henderson, CP Barry, DJ Houck, JR Carson, JC Hayward, TL TI Deep near-infrared imaging and photometry of the Antennae galaxies with WIRC SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (NGC 4038, NGC 4039); galaxies : interactions ID YOUNG STAR-CLUSTERS; LUMINOSITY FUNCTION; NGC 4038/4039; NGC-4038/4039; TELESCOPE AB We present deep near-infrared images of the Antennae galaxies, taken with the Palomar Wide-Field Infrared Camera (WIRC). The images cover a 4.'33 x 4.'33 ( 24.7 x 24.7 kpc) area around the galaxy interaction zone. We derive J- and K-S-band photometric fluxes for 172 infrared star clusters and discuss details of the two galactic nuclei and the overlap region. We also discuss the properties of a subset of 27 sources that have been detected with WIRC, HST, and the VLA. The sources in common are young clusters of less than 10 Myr, which show no correlation between their infrared colors and 6 cm radio properties. These clusters cover a wide range in infrared color due to extinction and evolution. The average extinction is about A(V) similar to 2 mag, while the reddest clusters may be reddened by up to 10 mag. C1 Leiden Observ, NL-2300 RA Leiden, Netherlands. Univ Florida, Dept Astron, Gainesville, FL 32611 USA. Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. Cornell Univ, Ctr Radiophys & Space Res, Ithaca, NY 14853 USA. CALTECH, Pasadena, CA 91125 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Gemini Observ, So Operat Ctr, La Serena, Chile. RP Brandl, BR (reprint author), Leiden Observ, POB 9513, NL-2300 RA Leiden, Netherlands. EM brandl@strw.leidenuniv.nl NR 21 TC 19 Z9 19 U1 0 U2 1 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 DEC 10 PY 2005 VL 635 IS 1 BP 280 EP 289 DI 10.1086/497357 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993CF UT WOS:000233929600021 ER PT J AU O'Connell, RW Martin, JR Crane, JD Burstein, D Bohlin, RC Landsman, WB Freedman, I Rood, RT AF O'Connell, RW Martin, JR Crane, JD Burstein, D Bohlin, RC Landsman, WB Freedman, I Rood, RT TI Uv/optical nuclear activity in the gE galaxy NGC 1399 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : elliptical and lenticular, cD; ultraviolet : galaxies ID DOMINATED ACCRETION FLOWS; HUBBLE-SPACE-TELESCOPE; SUPERMASSIVE BLACK-HOLES; GIANT ELLIPTIC GALAXIES; X-RAY-EMISSION; NEARBY GALAXIES; FORNAX CLUSTER; GLOBULAR-CLUSTER; TIDAL DISRUPTION; GALACTIC NUCLEI AB Using HST STIS, we have detected far-ultraviolet nuclear activity in the giant elliptical galaxy NGC 1399, the central and brightest galaxy in the Fornax I cluster. The source reached a maximum observed far-UV luminosity of similar to 1.2 x 10(39) ergs s(-1) in 1999 January. It was detectable in earlier HST archival images in 1996 ( B band) but not in 1991 ( V band) or 1993 ( UV). It faded by a factor of similar to 4 by mid-2000. The source is almost certainly associated with the low-luminosity AGN responsible for the radio emission in NGC 1399. The properties of the outburst are remarkably similar to the UV-bright nuclear transient discovered earlier in NGC 4552 by Renzini and coworkers. The source is much fainter than expected from its Bondi accretion rate ( estimated from Chandra high-resolution X-ray images), even in the context of "radiatively inefficient accretion flow'' models, and its variability also appears inconsistent with such models. High spatial resolution UV monitoring is a valuable means to study activity in nearby LLAGNs. C1 Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. Arizona State Univ, Dept Phys & Astron, Tempe, AZ 85287 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. NASA, Goddard Space Flight Ctr, Sci Syst & Applicat Inc, Greenbelt, MD 20771 USA. RP O'Connell, RW (reprint author), Univ Virginia, Dept Astron, POB 3818, Charlottesville, VA 22903 USA. NR 63 TC 11 Z9 11 U1 0 U2 1 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 DEC 10 PY 2005 VL 635 IS 1 BP 305 EP 310 DI 10.1086/497678 PN 1 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993CF UT WOS:000233929600023 ER PT J AU Hwang, U Flanagan, KA Petre, R AF Hwang, U Flanagan, KA Petre, R TI Chandra X-ray observation of a mature cloud-shock interaction in the bright eastern knot region of Puppis A SO ASTROPHYSICAL JOURNAL LA English DT Article DE instabilities; ISM : clouds; supernova remnants; X-rays : individual (Puppis A) ID LOOP SUPERNOVA REMNANT; STAR RX J0822-4300; CYGNUS-LOOP; NEUTRAL HYDROGEN; INTERSTELLAR CLOUDS; VLA OBSERVATIONS; RADIO; SPECTROSCOPY; SPECTRUM; OBJECTS AB We present Chandra X-ray images and spectra of the most prominent cloud-shock interaction region in the Puppis A supernova remnant. The bright eastern knot (BEK) has two main morphological components: (1) a bright compact knot that lies directly behind the apex of an indentation in the eastern X-ray boundary; and (2) lying 10 westward behind the shock, a curved vertical structure (bar) that is separated from a smaller bright cloud (cap) by faint diffuse emission. Based on hardness images and spectra, we identify the bar and cap as a single shocked interstellar cloud. Its morphology strongly resembles the "voided sphere'' structures seen at late times in Klein and coworkers' experimental simulations of cloud-shock interactions, when the crushing of the cloud by shear instabilities is well underway. We infer an interaction time of roughly 3 cloud-crushing timescales, which translates to 2000-4000 yr, based on the X-ray temperature, physical size, and estimated expansion of the shocked cloud. This is the first X-ray identified example of a cloud-shock interaction in this advanced phase. Closer to the shock front, the X-ray emission of the compact knot in the eastern part of the BEK region implies a recent interaction with relatively denser gas, some of which lies in front of the remnant. The complex spatial relationship of the X-ray emission of the compact knot to optical [O III] emission suggests that there are multiple cloud interactions occurring along the line of sight. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. RP Hwang, U (reprint author), NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA. EM hwang@milkyway.gsfc.nasa.gov NR 37 TC 38 Z9 38 U1 0 U2 1 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 DEC 10 PY 2005 VL 635 IS 1 BP 355 EP 364 DI 10.1086/497298 PN 1 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993CF UT WOS:000233929600028 ER PT J AU Djuric, N Lozano, JA Smith, SJ Chutjian, A AF Djuric, N Lozano, JA Smith, SJ Chutjian, A TI Surface charging and X-ray emission from insulator surfaces induced by collisions with highly charged ions: Relevance to cometary and planetary spectroscopy SO ASTROPHYSICAL JOURNAL LA English DT Article DE atomic processes; comets : general; X-rays : general ID CROSS-SECTIONS; SIO2; OLIVINE; IMPACT; HE+; H+ AB Characteristic X-ray emission lines are detected from simulants of comet surfaces as they undergo collisions with highly charged ions (HCIs). The HCI projectiles are O+2-O+7. Ion energies are varied in the range (2-7) q keV, where q is the ion charge state. The targets are the insulator minerals olivine, augite, and quartz. It is found that the emission of characteristic K-L, K-M X-rays appears to proceed during positive charging of the surface by the HCI beam. When one uses low-energy, flood-gun electrons to neutralize the surface charge, the X-ray emission is eliminated or greatly reduced, depending on the flood-gun current. Acceleration of background electrons onto the charged surface results in excitation of elemental transitions, including the K-L-2 and K-L-3 target X-ray emission lines of Mg and Si located spectroscopically at 1253.6 and 1739.4 eV, respectively. Also observed are emission lines from O, Na, Ca, Al, and Fe atoms in the target and charge-exchange lines via surface extraction of electrons by the O+q electric field. Good agreement is found in the ratio of the measured X-ray yields for Mg and Si relative to the ratio of their electron-impact K-shell ionization cross sections. The present study may serve as a guide to astronomers as to specific observing X-ray energies indicative of solar/stellar wind or magnetospheric ion interactions with a comet, planetary surface, or circumstellar dust. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Djuric, N (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. NR 32 TC 10 Z9 10 U1 0 U2 4 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 DEC 10 PY 2005 VL 635 IS 1 BP 718 EP 722 DI 10.1086/497105 PN 1 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993CF UT WOS:000233929600060 ER PT J AU Chary, RR Stern, D Eisenhardt, P AF Chary, RR Stern, D Eisenhardt, P TI Spitzer constraints on the z =6.56 galaxy lensed by Abell 370 SO ASTROPHYSICAL JOURNAL LA English DT Article DE cosmology : observations; early universe; galaxies : evolution; galaxies : formation; galaxies : high-redshift; galaxies : individual (HCM 6A) ID QUASAR LUMINOSITY FUNCTION; LY-ALPHA EMITTERS; ULTRA-DEEP-FIELD; SPACE-TELESCOPE; STAR-FORMATION; DROP GALAXIES; HUBBLE; Z-APPROXIMATE-TO-6; REIONIZATION; REDSHIFT AB We report on Spitzer IRAC observations of the spectroscopically confirmed z = 6.56 lensed Lya emitting source HCM 6A that was found behind the cluster Abell 370. Detection of the source at 3.6 and 4.5 mu m, corresponding to rest-frame optical emission, allows us to study the stellar population of this primeval galaxy. The broadband flux density at 4.5 mm is enhanced compared to the continuum at other wavelengths, likely due to the presence of strong Ha in emission. The derived Ha line flux corresponds to a star formation rate of greater than or similar to 140 M-circle dot yr(-1), more than an order of magnitude larger than estimates from the ultraviolet continuum and Lya emission line. The dust extinction required to explain the discrepancy is A(v) similar to 1 mag. The inference of dust at such high redshifts is surprising and implies that the first epoch of star formation in this galaxy occurred at z similar to 20 C1 CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Chary, RR (reprint author), CALTECH, Spitzer Sci Ctr, Mail Stop 220-6, Pasadena, CA 91125 USA. EM rchary@caltech.edu NR 30 TC 69 Z9 69 U1 0 U2 4 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 DEC 10 PY 2005 VL 635 IS 1 BP L5 EP L8 DI 10.1086/499205 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993CG UT WOS:000233929700002 ER PT J AU Dominik, C Ceccarelli, C Hollenbach, D Kaufman, M AF Dominik, C Ceccarelli, C Hollenbach, D Kaufman, M TI Gas-phase water in the surface layer of protoplanetary disks SO ASTROPHYSICAL JOURNAL LA English DT Article DE planetary systems : protoplanetary disks; stars : formation; stars : pre-main-sequence; ISM : molecules ID INTERSTELLAR; PHOTODESORPTION; ENVELOPE; GRAINS; ICE; HDO AB Recent observations of the ground-state transition of HDO at 464 GHz toward the protoplanetary disk of DM Tau have detected the presence of water vapor in the regions just above the outer disk midplane (Ceccarelli et al.). In the absence of nonthermal desorption processes, water should be almost entirely frozen onto the grain mantles, and HDO undetectable. In this Letter we present a chemical model that explores the possibility that the icy mantles are photodesorbed by FUV ( 6 eV <= hv <= 13.6 eV) photons. We show that the average interstellar FUV field is enough to create a layer of water vapor above the disk midplane over the entire disk. Assuming a photodesorption yield of 10(-3), the water abundance in this layer is predicted to be similar to 3 x 10(-7), and the average H2O column density is similar to 1.6 x 10(15) cm(-2). The predictions are very weakly dependent on the details of the model, like the incident FUV radiation field, and on the gas density in the disk. Based on this model, we predict a gaseous HDO/H2O ratio in DM Tau of similar to 1%. In addition, we predict the ground-state transition of water at 557 GHz to be undetectable with Odin and/or with the Herschel Space Observatory Heterodyne Instrument for the Far Infrared (HIFI). C1 Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. Observ Grenoble, Astrophys Lab, F-38041 Grenoble, France. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. San Jose State Univ, Dept Phys, San Jose, CA 95192 USA. RP Dominik, C (reprint author), Univ Amsterdam, Astron Inst Anton Pannekoek, Kruislaan 403, NL-1098 SJ Amsterdam, Netherlands. EM dominik@science.uva.nl; cecilia.ceccarelli@obs.ujf-grenoble.fr; hollenbach@ism.arc.nasa.gov; kaufman@ism.arc.nasa.gov NR 16 TC 54 Z9 54 U1 1 U2 4 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 DEC 10 PY 2005 VL 635 IS 1 BP L85 EP L88 DI 10.1086/498942 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993CG UT WOS:000233929700022 ER PT J AU Hicks, AK Mushotzky, R AF Hicks, AK Mushotzky, R TI Star formation rates in cooling flow clusters: A UV pilot study with archival XMM-Newton optical monitor data SO ASTROPHYSICAL JOURNAL LA English DT Article DE cooling flows; galaxies : clusters : general; galaxies : elliptical and lenticular, cD; galaxies : stellar content; stars : formation; ultraviolet : stars ID FAINT OBJECT SPECTROGRAPH; ULTRAVIOLET OBSERVATIONS; CD-GALAXY; EMISSION; SPECTRA; NEBULAE; ABELL-1795; MODELS AB We have analyzed XMM-Newton Optical Monitor UV (180 - 400 nm) data for a sample of 33 galaxies. Thirty are cluster member galaxies, and nine are central cluster galaxies (CCGs) in cooling flow clusters having mass deposition rates between 8 and 525 M-circle dot yr(-1). By comparing the ratio of UV to 2MASS J-band fluxes, we find a significant UV excess in many, but not all, cooling flow CCGs, consistent with several previous studies based on optical imaging data (McNamara & O'Connell; Cardiel et al.; Crawford et al.). This UV excess is a direct indication of the presence of young massive stars and, therefore, recent star formation. Using the Starburst99 model of continuous star formation over a 900 Myr period, we derive star formation rates of 0.2-219 M-circle dot yr(-1) for the cooling flow sample. For two-thirds of this sample, it is possible to equate Chandra/XMM cooling flow mass deposition rates with UV-inferred star formation rates, for a combination of starburst lifetime and IMF slope. This is a pilot study of the well-populated XMM UV cluster archive, and a more extensive follow-up study is currently underway. C1 Univ Virginia, Dept Astron, Charlottesville, VA 22903 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Hicks, AK (reprint author), Univ Virginia, Dept Astron, POB 3818, Charlottesville, VA 22903 USA. EM ahicks@alum.mit.edu; richard@milkyway.gsfc.nasa.gov NR 26 TC 66 Z9 67 U1 0 U2 1 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 DEC 10 PY 2005 VL 635 IS 1 BP L9 EP L12 DI 10.1086/499123 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993CG UT WOS:000233929700003 ER PT J AU Temi, P Brighenti, F Mathews, WG AF Temi, P Brighenti, F Mathews, WG TI Mid-infrared emission from elliptical galaxies: Sensitivity to stellar age SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : elliptical and lenticular, cD; galaxies : ISM; infrared : galaxies; infrared : ISM ID GROTH STRIP SURVEY; INTERMEDIATE-AGE; POPULATION HISTORIES; SPACE-TELESCOPE; DUST; PARAMETERS; EVOLUTION; SHELLS; STARS AB Mid-infrared observations (3.6-24 mu m) of normal giant elliptical galaxies with the Spitzer Space Telescope are consistent with pure populations of very old stars with no evidence of younger stars. Most of the stars in giant elliptical galaxies are old, but the mean stellar age determined from Balmer absorption in optical spectra can appear much younger due to a small admixture of younger stars. The mean stellar age can also be determined from the spectral energy distribution in the mid-infrared, which decreases with time relative to the optical emission and shifts to shorter wavelengths. The observed flux ratios F-8 mu m/F-3.6 mu m and F-24 mu m/F(3.6 mu m)for elliptical galaxies with the oldest Balmer line ages are lower than predicted by recent models of single stellar populations. For elliptical galaxies with the youngest Balmer line ages in our sample, 3-5 Gyr, the flux ratios F-24 mu m/F-3.6 mu m are identical to those of the oldest stars. When theoretical mid-IR spectra of old ( 12 Gyr) and young stellar populations are combined, errors in the F-24 mu m/F-3.6 mu m observations are formally inconsistent with a mass fraction of young stars 24 mm 3.6 mm that exceeds similar to 1%. This is less than the fraction of young stars expected in discussions of recent surveys of elliptical galaxies at higher redshifts. However, this inconsistency between Balmer line ages and those inferred from mid-IR observations must be regarded as provisional until more accurate observations and theoretical spectra become available. Finally, there is no evidence to date that central disks or patches of dust commonly visible in optical images of elliptical galaxies contribute sensibly to the mid-IR spectrum. C1 NASA, Ames Res Ctr, Astrophys Branch, Moffett Field, CA 94035 USA. SETI Inst, Mountain View, CA 94043 USA. Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Board Studies Astron & Astrophys, Santa Cruz, CA 95064 USA. Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy. RP Temi, P (reprint author), NASA, Ames Res Ctr, Astrophys Branch, MS 245-6, Moffett Field, CA 94035 USA. NR 22 TC 17 Z9 17 U1 0 U2 1 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 DEC 10 PY 2005 VL 635 IS 1 BP L25 EP L28 DI 10.1086/499239 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993CG UT WOS:000233929700007 ER PT J AU Arola, A Kazadzis, S Krotkov, N Bais, A Grobner, J Herman, JR AF Arola, A Kazadzis, S Krotkov, N Bais, A Grobner, J Herman, JR TI Assessment of TOMS UV bias due to absorbing aerosols SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID SINGLE SCATTERING ALBEDO; OPTICAL-PROPERTIES; ULTRAVIOLET IRRADIANCE; BREWER SPECTRORADIOMETER; TROPOSPHERIC AEROSOLS; SPECTRAL MEASUREMENTS; SATELLITE RETRIEVALS; GROUND MEASUREMENTS; SURFACE; RADIATION AB [1] We compared NASA Total Ozone Mapping Spectrometer ( TOMS) overpass irradiances against ground-based Brewer measurements at Ispra, Italy, and Thessaloniki, Greece, with the main objective of evaluating the effect of absorbing aerosols on TOMS UV bias using direct measurements of aerosol optical properties. Dependence of the TOMS/Brewer bias on aerosol absorption optical depth is significant. Our study demonstrates that the bias between TOMS and measured Brewer 324 nm irradiances increases with increasing aerosol absorption optical depth tau(abs). The correlation coefficients between the ratio TOMS/Brewer and tau(abs) at Ispra and Thessaloniki are similar to 0.7 or more and similar to 0.8 or more, respectively, depending on the range of solar zenith angle values selected for the analysis. We found that the correlation with single-scattering albedo omega or aerosol optical depth is significantly smaller than with tau(abs). If measurements or climatology of tau(abs) are available in the UVB range, the TOMS UV product can be postcorrected for absorbing aerosols using similar site-dependent regressions as established in our study. If no correction is applied, the mean positive biases between TOMS and Brewer 324 nm irradiances in Thessaloniki and Ispra are 19.2% and 29.7%, respectively, while the standard deviations are 8.9% and 16.5%. Depending on the level of correction, the mean positive bias can be essentially removed, and the standard deviations can be reduced down to similar to 6% and similar to 10%, respectively. C1 Finnish Meteorol Inst, FIN-70211 Kuopio, Finland. Aristotle Univ Thessaloniki, Lab Atmospher Phys, GR-54124 Thessaloniki, Greece. Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. NASA, Atmospheres Lab, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Commiss European Communities, Joint Res Ctr, Inst Hlth & Consumer Protect, I-21020 Ispra, Italy. RP Arola, A (reprint author), Finnish Meteorol Inst, POB 1627, FIN-70211 Kuopio, Finland. EM antti.arola@fmi.fi RI Kazadzis, Stelios/A-5628-2011; Kazadzis, Stelios/F-8667-2011; Bais, Alkiviadis/D-2230-2009; Krotkov, Nickolay/E-1541-2012; OI Bais, Alkiviadis/0000-0003-3899-2001; Krotkov, Nickolay/0000-0001-6170-6750; Kazadzis, Stelios/0000-0002-8624-8247; Herman, Jay/0000-0002-9146-1632; Arola, Antti/0000-0002-9220-0194 NR 30 TC 37 Z9 37 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 10 PY 2005 VL 110 IS D23 AR D23211 DI 10.1029/2005JD005913 PG 7 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 997LY UT WOS:000234248200002 ER PT J AU Matsoukas, C Banks, AC Hatzianastassiou, N Pavlakis, KG Hatzidimitriou, D Drakakis, E Stackhouse, PW Vardavas, I AF Matsoukas, C Banks, AC Hatzianastassiou, N Pavlakis, KG Hatzidimitriou, D Drakakis, E Stackhouse, PW Vardavas, I TI Seasonal heat budget of the Mediterranean Sea SO JOURNAL OF GEOPHYSICAL RESEARCH-OCEANS LA English DT Article ID LONGWAVE RADIATION BUDGET; FRESH-WATER BUDGETS; NORTHERN-HEMISPHERE; CLIMATOLOGICAL DATA; GLOBAL DISTRIBUTION; OCEAN SURFACE; MODEL; CLIMATE; FLUX; PARAMETERIZATION AB [1] We calculate the monthly components of the Mediterranean Sea heat budget, namely the net shortwave, net longwave, latent, sensible heat fluxes, and heat storage change, for years 1984 - 2000. The radiative components of the seasonal heat budget are derived by a radiation transfer model, while in most other studies bulk formulae are used. A variety of data are required to run the model, among which are cloud data from International Satellite Cloud Climatology Project ( ISCCP) D2 data set, aerosol data from Global Aerosol Data Set ( GADS), temperature and humidity from National Center for Environmental Prediction/National Center for Atmospheric Research (NCEP/ NCAR) and European Centre for Medium-range Weather Forecasts (ECMWF) Re-Analysis (ERA-40), and oceanographical data from Mediterranean Data Archaeology and Rescue (MEDAR) MEDATLAS database and the World Ocean Atlas 2001. We compare two methods for the estimation of the monthly latent heat flux and evaporation: the bulk aerodynamic and the heat balance. The average annual evaporation rate for the Mediterranean Sea, based on the heat balance method, is estimated at 1500 +/- 190 mm yr(-1). The bulk aerodynamic method produces estimates of the annual evaporation rate in the range 1060 1280 mm yr(-1), depending on the source of the input data. The analysis of the heat content shows that the solar heat absorbed by the sea during summer is redistributed to winter evaporation via heat storage by the sea. Thus the peak evaporation occurs in winter and is mainly driven by energy released (100 - 150 Wm(-2)) from sea heat storage. C1 Fdn Res & Technol Hellas, Inst Elect Struct & Laser, GR-71110 Iraklion, Greece. Univ Crete, Dept Phys, Iraklion, Greece. Hellen Ctr Marine Res, Attika, Greece. Univ Ioannina, Dept Phys, GR-45110 Ioannina, Greece. Technol Educ Inst Crete, Dept Gen Appl Sci, Iraklion, Greece. Technol Educ Inst Crete, Dept Elect Engn, Iraklion, Greece. NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Fdn Res & Technol Hellas, Inst Elect Struct & Laser, POB 1527, GR-71110 Iraklion, Greece. EM matsoukas@iesl.forth.gr RI Drakakis, Emmanuel/D-7396-2012; Vardavas, Ilias/G-7310-2011; Hatzidimitriou, Despina/A-3732-2015 NR 56 TC 16 Z9 16 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9275 EI 2169-9291 J9 J GEOPHYS RES-OCEANS JI J. Geophys. Res.-Oceans PD DEC 9 PY 2005 VL 110 IS C12 AR C12008 DI 10.1029/2004JC002566 PG 15 WC Oceanography SC Oceanography GA 997MG UT WOS:000234249000001 ER PT J AU Lebreton, JP Witasse, O Sollazzo, C Blancquaert, T Couzin, P Schipper, AM Jones, JB Matson, DL Gurvits, LI Atkinson, DH Kazeminejad, B Perez-Ayucar, M AF Lebreton, JP Witasse, O Sollazzo, C Blancquaert, T Couzin, P Schipper, AM Jones, JB Matson, DL Gurvits, LI Atkinson, DH Kazeminejad, B Perez-Ayucar, M TI An overview of the descent and landing of the Huygens probe on Titan SO NATURE LA English DT Article ID SURFACE; ENTRY; TELESCOPE; MISSION; SCIENCE; SYSTEM AB Titan, Saturn's largest moon, is the only Solar System planetary body other than Earth with a thick nitrogen atmosphere. The Voyager spacecraft confirmed that methane was the second-most abundant atmospheric constituent in Titan's atmosphere, and revealed a rich organic chemistry, but its cameras could not see through the thick organic haze. After a seven-year interplanetary journey on board the Cassini orbiter, the Huygens probe was released on 25 December 2004. It reached the upper layer of Titan's atmosphere on 14 January and landed softly after a parachute descent of almost 2.5 hours. Here we report an overview of the Huygens mission, which enabled studies of the atmosphere and surface, including in situ sampling of the organic chemistry, and revealed an Earth-like landscape. The probe descended over the boundary between a bright icy terrain eroded by fluvial activity - probably due to methane - and a darker area that looked like a river- or lake-bed. Post-landing images showed centimetre-sized surface details. C1 European Space Agcy, Estec, Sci Directorate, Res & Sci Support Dept, NL-2200 AG Noordwijk, Netherlands. European Space Agcy, Estec, Sci Directorate, Sci Project Dept, NL-2200 AG Noordwijk, Netherlands. ESOC, ESA Operat Directorate, D-64293 Darmstadt, Germany. Alcatel Alenia Space, F-06156 Cannes La Bocca, France. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Joint Inst VLBI Europe, NL-7990 AA Dwingeloo, Netherlands. Univ Idaho, Dept Elect & Comp Engn, Moscow, ID 83844 USA. Austrian Acad Sci, Space Res Inst, A-8042 Graz, Austria. RP European Space Agcy, Estec, Sci Directorate, Res & Sci Support Dept, NL-2200 AG Noordwijk, Netherlands. EM jean-pierre.lebreton@esa.int NR 24 TC 112 Z9 113 U1 3 U2 24 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD DEC 8 PY 2005 VL 438 IS 7069 BP 758 EP 764 DI 10.1038/nature04347 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 990XX UT WOS:000233777800036 PM 16319826 ER PT J AU Tomasko, MG Archinal, B Becker, T Bezard, B Bushroe, M Combes, M Cook, D Coustenis, A de Bergh, C Dafoe, LE Doose, L Doute, S Eibl, A Engel, S Gliem, F Grieger, B Holso, K Howington-Kraus, E Karkoschka, E Keller, HU Kirk, R Kramm, R Kuppers, M Lanagan, P Lellouch, E Lemmon, M Lunine, J McFarlane, E Moores, J Prout, GM Rizk, B Rosiek, M Rueffer, P Schroder, SE Schmitt, B See, C Smith, P Soderblom, L Thomas, N West, R AF Tomasko, MG Archinal, B Becker, T Bezard, B Bushroe, M Combes, M Cook, D Coustenis, A de Bergh, C Dafoe, LE Doose, L Doute, S Eibl, A Engel, S Gliem, F Grieger, B Holso, K Howington-Kraus, E Karkoschka, E Keller, HU Kirk, R Kramm, R Kuppers, M Lanagan, P Lellouch, E Lemmon, M Lunine, J McFarlane, E Moores, J Prout, GM Rizk, B Rosiek, M Rueffer, P Schroder, SE Schmitt, B See, C Smith, P Soderblom, L Thomas, N West, R TI Rain, winds and haze during the Huygens probe's descent to Titan's surface SO NATURE LA English DT Article ID AGGREGATE PARTICLES; ATMOSPHERE; AEROSOLS; SIMULATION; AMMONIA; ENTRY; MODEL; ICE AB The irreversible conversion of methane into higher hydrocarbons in Titan's stratosphere implies a surface or subsurface methane reservoir. Recent measurements from the cameras aboard the Cassini orbiter fail to see a global reservoir, but the methane and smog in Titan's atmosphere impedes the search for hydrocarbons on the surface. Here we report spectra and high-resolution images obtained by the Huygens Probe Descent Imager/Spectral Radiometer instrument in Titan's atmosphere. Although these images do not show liquid hydrocarbon pools on the surface, they do reveal the traces of once flowing liquid. Surprisingly like Earth, the brighter highland regions show complex systems draining into flat, dark lowlands. Images taken after landing are of a dry riverbed. The infrared reflectance spectrum measured for the surface is unlike any other in the Solar System; there is a red slope in the optical range that is consistent with an organic material such as tholins, and absorption from water ice is seen. However, a blue slope in the near-infrared suggests another, unknown constituent. The number density of haze particles increases by a factor of just a few from an altitude of 150 km to the surface, with no clear space below the tropopause. The methane relative humidity near the surface is 50 per cent. C1 Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. US Geol Survey, Flagstaff, AZ 86001 USA. Observ Paris, LESIA, F-92195 Meudon, France. Univ Grenoble 1, CNRS, Lab Planetol Grenoble, F-38041 Grenoble, France. Tech Univ Carolo Wilhelmina Braunschweig, D-38106 Braunschweig, Germany. Max Planck Inst Solar Syst Res, D-37191 Katlenburg Lindau, Germany. Texas A&M Univ, Dept Phys, College Stn, TX 77843 USA. Ist Fis Spazio Interplanetario, Ist Nazl Astrofis, ARTOV, I-00133 Rome, Italy. Univ Bern, Dept Phys, CH-3012 Bern, Switzerland. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP See, C (reprint author), Univ Arizona, Lunar & Planetary Lab, 1629 E Univ Blvd, Tucson, AZ 85721 USA. EM csee@lpl.arizona.edu RI Lemmon, Mark/E-9983-2010; Schmitt, Bernard/A-1064-2009; Schroder, Stefan/D-9709-2013 OI Lemmon, Mark/0000-0002-4504-5136; Schmitt, Bernard/0000-0002-1230-6627; Schroder, Stefan/0000-0003-0323-8324 NR 31 TC 330 Z9 332 U1 7 U2 61 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD DEC 8 PY 2005 VL 438 IS 7069 BP 765 EP 778 DI 10.1038/nature04126 PG 14 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 990XX UT WOS:000233777800037 PM 16319829 ER PT J AU Niemann, HB Atreya, SK Bauer, SJ Carignan, GR Demick, JE Frost, RL Gautier, D Haberman, JA Harpold, DN Hunten, DM Israel, G Lunine, JI Kasprzak, WT Owen, TC Paulkovich, M Raulin, F Raaen, E Way, SH AF Niemann, HB Atreya, SK Bauer, SJ Carignan, GR Demick, JE Frost, RL Gautier, D Haberman, JA Harpold, DN Hunten, DM Israel, G Lunine, JI Kasprzak, WT Owen, TC Paulkovich, M Raulin, F Raaen, E Way, SH TI The abundances of constituents of Titan's atmosphere from the GCMS instrument on the Huygens probe SO NATURE LA English DT Article ID MASS-SPECTROMETER; HETERODYNE OBSERVATIONS; SOLAR-SYSTEM; NITROGEN; METHANE; ORIGIN; EVOLUTION; MODEL; RATIO; PHOTOCHEMISTRY AB Saturn's largest moon, Titan, remains an enigma, explored only by remote sensing from Earth, and by the Voyager and Cassini spacecraft. The most puzzling aspects include the origin of the molecular nitrogen and methane in its atmosphere, and the mechanism(s) by which methane is maintained in the face of rapid destruction by photolysis. The Huygens probe, launched from the Cassini spacecraft, has made the first direct observations of the satellite's surface and lower atmosphere. Here we report direct atmospheric measurements from the Gas Chromatograph Mass Spectrometer (GCMS), including altitude profiles of the constituents, isotopic ratios and trace species ( including organic compounds). The primary constituents were confirmed to be nitrogen and methane. Noble gases other than argon were not detected. The argon includes primordial Ar-36, and the radiogenic isotope Ar-40, providing an important constraint on the outgassing history of Titan. Trace organic species, including cyanogen and ethane, were found in surface measurements. C1 NASA, Greenbelt, MD 20771 USA. Univ Michigan, Ann Arbor, MI 48109 USA. Graz Univ, Inst Meteorol & Geophys, A-8010 Graz, Austria. Observ Paris, LESIA, F-92195 Meudon, France. Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85716 USA. CNRS, Serv Aeron, F-91371 Verrieres Le Buisson, France. Univ Alabama Birmingham, CMC, Birmingham, AL 35205 USA. Univ Hawaii, Honolulu, HI 96822 USA. Univ Paris 12, Lab Interuniv Syst Atmospher, F-94010 Creteil, France. Univ Paris 07, F-94010 Creteil, France. RP NASA, Greenbelt, MD 20771 USA. EM Hasso.B.Niemann@nasa.gov RI Harpold, Dan/I-3345-2013; OI Bauer, Siegfried/0000-0003-4213-2047 NR 46 TC 545 Z9 550 U1 11 U2 117 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 EI 1476-4687 J9 NATURE JI Nature PD DEC 8 PY 2005 VL 438 IS 7069 BP 779 EP 784 DI 10.1038/nature04122 PG 6 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 990XX UT WOS:000233777800038 PM 16319830 ER PT J AU Fulchignoni, M Ferri, F Angrilli, F Ball, AJ Bar-Nun, A Barucci, MA Bettanini, C Bianchini, G Borucki, W Colombatti, G Coradini, M Coustenis, A Debei, S Falkner, P Fanti, G Flamini, E Gaborit, V Grard, R Hamelin, M Harri, AM Hathi, B Jernej, I Leese, MR Lehto, A Stoppato, PFL Lopez-Moreno, JJ Makinen, T McDonnell, JAM McKay, CP Molina-Cuberos, G Neubauer, FM Pirronello, V Rodrigo, R Saggin, B Schwingenschuh, K Seiff, A Simoes, F Svedhem, H Tokano, T Towner, MC Trautner, R Withers, P Zarnecki, JC AF Fulchignoni, M Ferri, F Angrilli, F Ball, AJ Bar-Nun, A Barucci, MA Bettanini, C Bianchini, G Borucki, W Colombatti, G Coradini, M Coustenis, A Debei, S Falkner, P Fanti, G Flamini, E Gaborit, V Grard, R Hamelin, M Harri, AM Hathi, B Jernej, I Leese, MR Lehto, A Stoppato, PFL Lopez-Moreno, JJ Makinen, T McDonnell, JAM McKay, CP Molina-Cuberos, G Neubauer, FM Pirronello, V Rodrigo, R Saggin, B Schwingenschuh, K Seiff, A Simoes, F Svedhem, H Tokano, T Towner, MC Trautner, R Withers, P Zarnecki, JC TI In situ measurements of the physical characteristics of Titan's environment SO NATURE LA English DT Article ID VOYAGER-1 RADIO-OCCULTATION; HUYGENS PROBE; ELECTRICAL-CONDUCTIVITY; ELECTROMAGNETIC-WAVES; UPPER-ATMOSPHERE; GRAVITY-WAVES; PWA-HASI; SURFACE; TEMPERATURES; PROPAGATION AB On the basis of previous ground-based and fly-by information, we knew that Titan's atmosphere was mainly nitrogen, with some methane, but its temperature and pressure profiles were poorly constrained because of uncertainties in the detailed composition. The extent of atmospheric electricity ('lightning') was also hitherto unknown. Here we report the temperature and density profiles, as determined by the Huygens Atmospheric Structure Instrument (HASI), from an altitude of 1,400 km down to the surface. In the upper part of the atmosphere, the temperature and density were both higher than expected. There is a lower ionospheric layer between 140 km and 40 km, with electrical conductivity peaking near 60 km. We may also have seen the signature of lightning. At the surface, the temperature was 93.65 +/- 0.25 K, and the pressure was 1,467 +/- 1 hPa. C1 Univ Padua, CISAS G Colombo, I-35131 Padua, Italy. Observ Paris, LESIA, F-92195 Meudon, France. Univ Denis Diderot Paris 7, UFR Phys, F-75006 Paris, France. Open Univ, PSSRI, Milton Keynes MK7 6AA, Bucks, England. Tel Aviv Univ, Dept Geophys & Planetary Sci, IL-69978 Tel Aviv, Israel. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. ESA Headquarters, Sci Directorate, F-75015 Paris, France. European Space Agcy, Estec, ESA, NL-2200 AG Noordwijk, Netherlands. Agenzia Spaziale Italiana, I-00198 Rome, Italy. CETP IPSL, F-94107 St Maur, France. CNRS, LPCE, F-45071 Orleans, France. Finnish Meteorol Inst, Helsinki 00100, Finland. Austrian Acad Sci IWF, Space Res Inst, A-8042 Graz, Austria. CSIC, Inst Astrofis Andalucia, E-18080 Granada, Spain. Univ Murcia, Dept Phys, Appl Electromagnet Grp, E-30100 Murcia, Spain. Univ Cologne, Inst Geophys & Meteorol, D-50923 Cologne, Germany. Univ Catania, DMFCI, I-95125 Catania, Italy. Politecn Milan, Dipartimento Meccan, I-20133 Milan, Italy. Boston Univ, Ctr Space Phys, Boston, MA 02215 USA. RP Ferri, F (reprint author), Univ Padua, CISAS G Colombo, Via Venezia 15, I-35131 Padua, Italy. EM francesca.ferri@unipd.it RI Simoes, Fernando/D-7731-2012; Withers, Paul/H-2241-2014; Molina-Cuberos, Gregorio /K-7522-2014; Lopez-Moreno, Jose Juan/C-7976-2011; Harri, Ari-Matti/C-7142-2012; Ball, Andrew/B-6747-2009; OI Molina-Cuberos, Gregorio /0000-0002-5664-7028; Harri, Ari-Matti/0000-0001-8541-2802; Ball, Andrew/0000-0003-1593-3279; Lopez-Moreno, Jose Juan/0000-0002-7946-2624; saggin, bortolino/0000-0002-4033-3585 NR 45 TC 375 Z9 380 U1 3 U2 60 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD DEC 8 PY 2005 VL 438 IS 7069 BP 785 EP 791 DI 10.1038/nature04314 PG 7 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 990XX UT WOS:000233777800039 PM 16319827 ER PT J AU Israel, G Szopa, C Raulin, F Cabane, M Niemann, HB Atreya, SK Bauer, SJ Brun, JF Chassefiere, E Coll, P Conde, E Coscia, D Hauchecorne, A Millian, P Nguyen, MJ Owen, T Riedler, W Samuelson, RE Siguier, JM Steller, M Sternberg, R Vidal-Madjar, C AF Israel, G Szopa, C Raulin, F Cabane, M Niemann, HB Atreya, SK Bauer, SJ Brun, JF Chassefiere, E Coll, P Conde, E Coscia, D Hauchecorne, A Millian, P Nguyen, MJ Owen, T Riedler, W Samuelson, RE Siguier, JM Steller, M Sternberg, R Vidal-Madjar, C TI Complex organic matter in Titan's atmospheric aerosols from in situ pyrolysis and analysis SO NATURE LA English DT Article ID OPTICAL-PROPERTIES; HYDROGEN-CYANIDE; HAZE; ACETYLENE; PLASMA; CLOUDS AB Aerosols in Titan's atmosphere play an important role in determining its thermal structure(1-3). They also serve as sinks for organic vapours(4) and can act as condensation nuclei for the formation of clouds(5,6), where the condensation efficiency will depend on the chemical composition of the aerosols(5,7). So far, however, no direct information has been available on the chemical composition of these particles. Here we report an in situ chemical analysis of Titan's aerosols by pyrolysis at 600 degrees C. Ammonia (NH3) and hydrogen cyanide (HCN) have been identified as the main pyrolysis products. This clearly shows that the aerosol particles include a solid organic refractory core. NH3 and HCN are gaseous chemical fingerprints of the complex organics that constitute this core, and their presence demonstrates that carbon and nitrogen are in the aerosols. C1 Univ Paris 06, CNRS, UMR 7620, Serv Aeron, F-91371 Verrieres Le Buisson, France. Univ Versailles St Quentin, F-91371 Verrieres Le Buisson, France. Univ Paris 12, CNRS, UMR 7583, Lab Interuniv Syst Atmospher, F-94010 Creteil, France. Univ Paris 07, F-94010 Creteil, France. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Michigan, Ann Arbor, MI 48109 USA. Graz Univ, Inst Meteorol & Geophys, A-8010 Graz, Austria. Ctr Natl Etud Spatiales, F-31401 Toulouse, France. Off Natl Etud & Rech Aerosp, F-31055 Toulouse, France. Univ Hawaii Manoa, Inst Astron, Honolulu, HI 96822 USA. Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. Austrian Acad Sci, Inst Weltraumforsch, A-8042 Graz, Austria. CNRS, UMR 7581, Lab Rech Polymeres, F-94320 Thiais, France. RP Israel, G (reprint author), Univ Paris 06, CNRS, UMR 7620, Serv Aeron, F-91371 Verrieres Le Buisson, France. EM Guy.israel@aerov.jussieu.fr RI Hauchecorne, Alain/A-8489-2013; szopa, cyril/C-6865-2015; OI szopa, cyril/0000-0002-0090-4056; Bauer, Siegfried/0000-0003-4213-2047; Siguier, Jean-Michel/0000-0003-3568-9816; Hauchecorne, Alain/0000-0001-9888-6994 NR 24 TC 114 Z9 115 U1 2 U2 26 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD DEC 8 PY 2005 VL 438 IS 7069 BP 796 EP 799 DI 10.1038/nature04349 PG 4 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 990XX UT WOS:000233777800041 PM 16319825 ER PT J AU Bird, MK Allison, M Asmar, SW Atkinson, DH Avruch, IM Dutta-Roy, R Dzierma, Y Edenhofer, P Folkner, WM Gurvits, LI Johnston, DV Plettemeier, D Pogrebenko, SV Preston, RA Tyler, GL AF Bird, MK Allison, M Asmar, SW Atkinson, DH Avruch, IM Dutta-Roy, R Dzierma, Y Edenhofer, P Folkner, WM Gurvits, LI Johnston, DV Plettemeier, D Pogrebenko, SV Preston, RA Tyler, GL TI The vertical profile of winds on Titan SO NATURE LA English DT Article ID GENERAL-CIRCULATION; RADIO SCIENCE; SATURN SYSTEM; ATMOSPHERE; SUPERROTATION; TEMPERATURES; OCCULTATION; VOYAGER-1; DYNAMICS; VENUS AB One of Titan's most intriguing attributes is its copious but featureless atmosphere. The Voyager 1 fly-by and occultation in 1980 provided the first radial survey of Titan's atmospheric pressure and temperature(1,2) and evidence for the presence of strong zonal winds(3). It was realized that the motion of an atmospheric probe could be used to study the winds, which led to the inclusion of the Doppler Wind Experiment(4) on the Huygens probe(5). Here we report a high resolution vertical profile of Titan's winds, with an estimated accuracy of better than 1 m s(-1). The zonal winds were prograde during most of the atmospheric descent, providing in situ confirmation of superrotation on Titan. A layer with surprisingly slow wind, where the velocity decreased to near zero, was detected at altitudes between 60 and 100 km. Generally weak winds (similar to 1 m s(-1)) were seen in the lowest 5 km of descent. C1 Univ Bonn, Inst Radioastron, D-53125 Bonn, Germany. NASA, Goddard Inst Space Studies, New York, NY 10025 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Idaho, Dept Elect & Comp Engn, Moscow, ID 83844 USA. Joint Inst VLBI Europe, NL-7990 AA Dwingeloo, Netherlands. Ruhr Univ Bochum, Inst HF Tech, D-44780 Bochum, Germany. Tech Univ Dresden, Elektrotech Inst, D-01062 Dresden, Germany. Stanford Univ, Ctr Radar Astron, Stanford, CA 94305 USA. RP Bird, MK (reprint author), Univ Bonn, Inst Radioastron, Auf Hugel 71, D-53125 Bonn, Germany. EM mbird@astro.uni-bonn.de NR 25 TC 105 Z9 106 U1 1 U2 4 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0028-0836 J9 NATURE JI Nature PD DEC 8 PY 2005 VL 438 IS 7069 BP 800 EP 802 DI 10.1038/nature04060 PG 3 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 990XX UT WOS:000233777800042 PM 16319831 ER PT J AU Palo, SE Forbes, JM Zhang, X Russell, JM Mertens, CJ Mlynczak, MG Burns, GB Espy, PJ Kawahara, TD AF Palo, SE Forbes, JM Zhang, X Russell, JM Mertens, CJ Mlynczak, MG Burns, GB Espy, PJ Kawahara, TD TI Planetary wave coupling from the stratosphere to the thermosphere during the 2002 Southern Hemisphere pre-stratwarm period SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID ROTATIONAL TEMPERATURES; STATION 69-DEGREES-S; 39-DEGREES-E; 78-DEGREES-E; ANTARCTICA AB Temperature observations between 20 and 120 km from the SABER instrument on the TIMED spacecraft are used to investigate the nature of planetary wave activity during the 60 days prior to the midwinter stratospheric warming that commenced on 26 September, 2002 in the Southern Hemisphere. The primary wave components consist of eastward-propagating quasi-10-day waves with zonal wave numbers s = 1 and s = 2, and a stationary planetary wave with s = 1. The waves are found to extend from the lower stratosphere to the 100 - 120 km height region with surprisingly little amplitude attenuation, although wave amplitudes oscillate with altitude like a standing wave pattern. Time evolution of the waves is also addressed with emphasis on 86 km altitude, where temperature observations from three Antarctic stations at Davis (69 degrees S, 78 degrees W), Rothera ( 68 degrees S, 68 degrees W) and Syowa (69 degrees S, 40 degrees E) are available during the same period. We demonstrate that the temporal evolution of temperature obtained by superposition of the waves derived from SABER measurements accounts for nearly all the temperature variability observed at the longitudes of the three Antarctic stations. C1 Univ Colorado, Dept Aerosp Engn Sci, Boulder, CO 80309 USA. Hampton Univ, Ctr Atmospher Sci, Hampton, VA 23668 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. Shinshu Univ, Nagano, Japan. Australian Antarctic Div, Kingston, Tas 7050, Australia. British Antarctic Survey, Cambridge CB3 OET, England. RP Palo, SE (reprint author), Univ Colorado, Dept Aerosp Engn Sci, Campus Box 429, Boulder, CO 80309 USA. EM scott.palo@colorado.edu RI Mlynczak, Martin/K-3396-2012; ZHANG, Xiao-Ye/C-8707-2012 OI FORBES, JEFFREY/0000-0001-6937-0796; PALO, SCOTT/0000-0002-4729-4929; ZHANG, Xiao-Ye/0000-0003-1802-3385 NR 17 TC 24 Z9 26 U1 0 U2 1 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 7 PY 2005 VL 32 IS 23 AR L23809 DI 10.1029/2005GL024298 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 997LL UT WOS:000234246800006 ER PT J AU Bridges, NT Phoreman, J White, BR Greeley, R Eddlemon, EE Wilson, GR Meyer, CJ AF Bridges, NT Phoreman, J White, BR Greeley, R Eddlemon, EE Wilson, GR Meyer, CJ TI Trajectories and energy transfer of saltating particles onto rock surfaces: Application to abrasion and ventifact formation on Earth and Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID PATHFINDER LANDING SITE; WIND-DRIVEN SAND; MERIDIANI-PLANUM; GLOBAL SURVEYOR; ORBITER CAMERA; GUSEV CRATER; SEDIMENT-TRANSPORT; OPPORTUNITY ROVER; COACHELLA VALLEY; SPIRIT ROVER AB [1] The interaction between saltating sand grains and rock surfaces is assessed to gauge relative abrasion potential as a function of rock shape, wind speed, grain size, and planetary environment. Many kinetic energy height profiles for impacts exhibit a distinctive increase, or kink, a few centimeters above the surface, consistent with previous field, wind tunnel, and theoretical investigations. The height of the kink observed in natural and wind tunnel settings is greater than predictions by a factor of 2 or more, probably because of enhanced bouncing off hard ground surfaces. Rebounded grains increase the effective flux and relative kinetic energy for intermediate slope angles. Whether abrasion occurs, as opposed to simple grain impact with little or no mass lost from the rock, depends on whether the grain kinetic energy (E-G) exceeds a critical value (E-C), as well as the flux of grains with energies above E-C. The magnitude of abrasion and the shape change of the rock over time depends on this flux and the value of E-G > E-C. Considering the potential range of particle sizes and wind speeds, the predicted kinetic energies of saltating sand hitting rocks overlap on Earth and Mars. However, when limited to the most likely grain sizes and threshold conditions, our results agree with previous work and show that kinetic energies are about an order of magnitude greater on Mars. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Arizona State Univ, NASA, Ames Res Ctr, Dept Geol Sci, Moffett Field, CA 94035 USA. Univ Calif Davis, Dept Mech Engn, Davis, CA 95616 USA. Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. Ohio Univ, Dept Geol Sci, Athens, OH 45701 USA. RP Bridges, NT (reprint author), CALTECH, Jet Prop Lab, MS 183-501,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM nathan.bridges@jpl.nasa.gov RI Bridges, Nathan/D-6341-2016 NR 75 TC 10 Z9 10 U1 0 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD DEC 7 PY 2005 VL 110 IS E12 AR E12004 DI 10.1029/2004JE002388 PG 24 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 997MH UT WOS:000234249100002 ER PT J AU Rao, MN Sutton, SR McKay, DS Dreibus, G AF Rao, MN Sutton, SR McKay, DS Dreibus, G TI Clues to Martian brines based on halogens in salts from nakhlites and MER samples SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID X-RAY SPECTROMETER; AQUEOUS ALTERATION; MERIDIANI-PLANUM; GUSEV CRATER; EARLY MARS; METEORITE; WATER; ROCKS; LAFAYETTE; CHEMISTRY AB [1] Chlorine and Br abundances in fracture-filling secondary salts in Nakhla veins determined in this study by Synchrotron X-ray Microprobe ( Br) and Electron Microprobe (Cl) techniques compare well to the halogens determined recently by APXS instruments in soils and rock rinds at the Gusev and Meridiani sites. The salts in these Mars rocks arise from Martian brines that have undergone evaporative or freezing concentration. The halogen abundances in these salts are corrected for "dilution effect'' ( because of mixing with halogen- poor phases) to obtain their "true'' abundances, which seem to be close to the halogen abundances in terrestrial sea brines. Consistent with the petrographic evidence for evaporative salt deposition sequence of carbonate-sulfate-halite in nakhlite meteorites, Nakhla veins yield high Br ( similar to 250 ppm) and low Cl/Br ratios ( similar to 10 - 50), suggesting possible salt deposition from concentrated brines, whereas Lafayette iddingsite, with low Br (11 ppm) and high Cl/ Br ratios ( similar to 250 - 300), indicates salt deposition from dilute brines on Mars. The low Cl/ Br ratios ( similar to 20 to 80) in salts from Gusev and Meridiani rock rinds indicate that they presumably originate from concentrated subsurface Martian brines. The high Cl/ Br ratio ( similar to 270) in salts deposited by dilute solutions in Lafayette and Adirondack is similar to the chondritic Cl/ Br ratio, which seems to characterize the dilute brines on Mars ( prior to halite precipitation) including "Early Mars Waters'' (Noachian or earlier). Our results seem to be consistent with the Burt-Knauth model involving density stratification during evaporation/freezing of brine solutions in Martian regolith. C1 NASA, Lyndon B Johnson Space Ctr, Jacobs ESC Grp, Houston, TX 77058 USA. Univ Chicago, Dept Geophys Sci, Chicago, IL 60637 USA. Univ Chicago, CARS, Chicago, IL 60637 USA. NASA, Lyndon B Johnson Space Ctr, ARES, Houston, TX 77058 USA. Max Planck Inst Chem, D-55020 Mainz, Germany. RP Rao, MN (reprint author), NASA, Lyndon B Johnson Space Ctr, Jacobs ESC Grp, Bay Area Blvd, Houston, TX 77058 USA. EM sitarao@sbcglobal.net; sutton@cars.uchicago.edu; david.s.mckay@jsc.nasa.gov; dreibus@mpch-mainz.mpg.de NR 59 TC 15 Z9 15 U1 1 U2 7 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD DEC 7 PY 2005 VL 110 IS E12 AR E12S06 DI 10.1029/2005JE002470 PG 12 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 997MH UT WOS:000234249100003 ER PT J AU Walsh, BM Grew, GW Barnes, NP AF Walsh, BM Grew, GW Barnes, NP TI Energy levels and intensity parameters of Ho3+ ions in GdLiF4, YLiF4 and LuLiF4 SO JOURNAL OF PHYSICS-CONDENSED MATTER LA English DT Article ID RARE-EARTH IONS; CRYSTAL-FIELD ANALYSIS; END-PUMPING TECHNIQUE; SINGLE-CRYSTALS; LANTHANUM TRIFLUORIDE; OPTICAL APPLICATIONS; ROOM-TEMPERATURE; LASER; GROWTH; TM AB While the energy levels in Ho:YLF have been measured previously, they have not been as thoroughly investigated in the isomorphs, Ho:LuLF and Ho:GdLF. We report here the measurement of the energy levels of the trivalent lanthanide Ho3+ in GdLiF4 (GdLF), YLiF4 (YLF), and LuLiF4 (LuLF). The measurement of the energy levels of Ho:YLF, although they have been measured before, are repeated here for self-consistent comparison to Ho:LuLF and Ho:GdLF The Stark split levels for the first ten Ho manifolds in these materials have been measured, and the results have been fitted to a free-ion plus crystal-field Hamiltonian to generate a theoretical set of energy levels. Crystal-field parameters were varied to determine the best fit between experimental and theoretical energy levels. The energy levels of Ho:GdLF and Ho:LuLF are seen to be very similar to those in Ho:YLF. However, subtle changes resulting from replacing Y3+ with Gd3+ or Lu3+ in the fluoride crystal YLiF4 result in shorter transition wavelengths in GdLF and longer transition wavelengths in LuLF. This has implications for Ho I-5(7) -> I-5(8) lasers operating at similar to 2.0 mu m. The energy levels for Ho:GdLF and Ho:LuLF determined here indicate that Ho:GdLF will have a larger lower laser level thermal population than Ho:YLF, while Ho:LuLF lasers will have a smaller lower laser level thermal population than Ho:YLF. This is consistent with the larger Stark splitting associated with the larger host ions that Ho Substitutes for in these lithium fluoride materials. The intensity parameters are also determined from a Judd-Ofelt analysis and used to calculate radiative lifetimes and branching ratios for the first ten manifolds in Ho:GdLF, Ho:YLF and Ho:LuLF C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Walsh, BM (reprint author), NASA, Langley Res Ctr, Hampton, VA 23681 USA. NR 26 TC 34 Z9 34 U1 1 U2 13 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0953-8984 J9 J PHYS-CONDENS MAT JI J. Phys.-Condes. Matter PD DEC 7 PY 2005 VL 17 IS 48 BP 7643 EP 7665 DI 10.1088/0953-8984/17/48/016 PG 23 WC Physics, Condensed Matter SC Physics GA 997SR UT WOS:000234268600018 ER PT J AU Martin, A Eskridge, R AF Martin, A Eskridge, R TI Electrical coupling efficiency of inductive plasma accelerators SO JOURNAL OF PHYSICS D-APPLIED PHYSICS LA English DT Article ID LAUNCHER AB A single-stage pulsed inductive plasma accelerator was modelled as an inductive mass-driver, with the plasma treated as a rigid slug that acts as the armature. We derive a set of coupled dynamic-circuit equations, with dimensionless coefficients. The functional form of the mutual inductance profile, M(z), was calculated using the magnetic field solver QuickField; an exponential form for M(z) was found to be accurate for a variety of coil-slug geometries. A parametric study of the solutions to the equations was performed in order to determine the conditions that yield high coupling efficiency. High inductance, multi-turn drive-coils yield the highest efficiency for a single-stage device. Using inductive recapture, coupling efficiencies in excess of 90% are possible; without it, the peak efficiency is much lower, eta <= 55%. We conclude that inductive recapture will be required in order to achieve the high efficiency required of an electric thruster. The efficiency scales favourably with increasing power, although this does not preclude operation at lower power with acceptable efficiency. The presence of an imbedded bias flux in the slug improves the dynamic efficiency for devices without inductive recapture, but offers little improvement when used with inductive recapture. C1 NASA, George C Marshall Space Flight Ctr, Prop Res Ctr, Sci & Technol Directorate, Huntsville, AL 35812 USA. RP Martin, A (reprint author), NASA, George C Marshall Space Flight Ctr, Prop Res Ctr, Sci & Technol Directorate, XD22, Huntsville, AL 35812 USA. NR 23 TC 7 Z9 7 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA DIRAC HOUSE, TEMPLE BACK, BRISTOL BS1 6BE, ENGLAND SN 0022-3727 J9 J PHYS D APPL PHYS JI J. Phys. D-Appl. Phys. PD DEC 7 PY 2005 VL 38 IS 23 BP 4168 EP 4179 DI 10.1088/0022-3727/38/23/005 PG 12 WC Physics, Applied SC Physics GA 996OH UT WOS:000234183000006 ER PT J AU Kleinbohl, A Toon, GC Sen, B Blavier, JFL Weisenstein, DK Wennberg, PO AF Kleinbohl, A Toon, GC Sen, B Blavier, JFL Weisenstein, DK Wennberg, PO TI Infrared measurements of atmospheric CH3CN SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID METHYL CYANIDE; ACETONITRILE; TROPOSPHERE; SINKS; OCEAN; HCN AB For the first time CH3CN has been measured in the Earth's atmosphere by means of infrared remote sensing. Vertical profiles of volume mixing ratio were retrieved from 12 solar occultation measurements by the balloon-borne JPL MkIV interferometer between 1993 and 2004. Profile retrieval is possible in an altitude range between 12 and 30 km with a precision of similar to 20 ppt in the Arctic and similar to 30 ppt at mid-latitudes. The retrieved CH3CN profiles show mixing ratios of 100 - 150 ppt a few kilometers above the tropopause that decrease to values below 40 ppt at altitudes between 22 and 30 km. The CH3CN mixing ratios show a reasonably compact correlation with the stratospheric tracers CH3Cl and CH4. The CH3CN altitude profiles and tracer correlations are well reproduced by a 2-dimensional model, suggesting that CH3CN is long-lived in the lower stratosphere and that previously-proposed ion-molecule reactions do not play a major role as loss processes of CH3CN. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Atmospher & Environm Res Inc, Lexington, MA 02421 USA. CALTECH, Div Engn & Appl Sci, Pasadena, CA 91125 USA. RP CALTECH, Jet Prop Lab, MS 183-501,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM armin.kleinboehl@jpl.nasa.gov RI Wennberg, Paul/A-5460-2012 NR 22 TC 9 Z9 9 U1 0 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 6 PY 2005 VL 32 IS 23 AR L23807 DI 10.1029/2005GL024283 PG 5 WC Geosciences, Multidisciplinary SC Geology GA 997LJ UT WOS:000234246600006 ER PT J AU Ominami, Y Ngo, Q Austin, AJ Yoong, H Yang, CY Cassell, AM Cruden, BA Li, J Meyyappan, M AF Ominami, Y Ngo, Q Austin, AJ Yoong, H Yang, CY Cassell, AM Cruden, BA Li, J Meyyappan, M TI Structural characteristics of carbon nanofibers for on-chip interconnect applications SO APPLIED PHYSICS LETTERS LA English DT Article ID CHEMICAL-VAPOR-DEPOSITION; FIELD-EFFECT TRANSISTORS; NANOTUBES; GROWTH; TRANSPORT; PALLADIUM; REACTOR AB In this letter, we compare the structures of plasma-enhanced chemical vapor deposition of Ni-catalyzed and Pd-catalyzed carbon nanofibers (CNFs) synthesized for on-chip interconnect applications with scanning transmission electron microscopy (STEM). The Ni-catalyzed CNF has a conventional fiberlike structure and many graphitic layers that are almost parallel to the substrate at the CNF base. In contrast, the Pd-catalyzed CNF has a multiwall nanotubelike structure on the sidewall spanning the entire CNF. The microstructure observed in the Pd-catalyzed fibers at the CNF-metal interface has the potential to lower contact resistance significantly, as our electrical measurements using current-sensing atomic force microscopy indicate. A structural model is presented based on STEM image analysis. (c) 2005 American Institute of Physics. C1 Santa Clara Univ, Ctr Nanostruct, Santa Clara, CA 95139 USA. NASA, Ames Res Ctr, Ctr Nanotechnol, Moffett Field, CA 94035 USA. RP Ominami, Y (reprint author), Santa Clara Univ, Ctr Nanostruct, 500 El Camino Real, Santa Clara, CA 95139 USA. EM yominami@scu.edu RI Li, Jun/H-7771-2013 OI Li, Jun/0000-0002-3689-8946 NR 22 TC 29 Z9 29 U1 1 U2 3 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0003-6951 J9 APPL PHYS LETT JI Appl. Phys. Lett. PD DEC 5 PY 2005 VL 87 IS 23 AR 233105 DI 10.1063/1.2137873 PG 3 WC Physics, Applied SC Physics GA 990DK UT WOS:000233723200066 ER PT J AU Singh, M Shpargel, TP Morscher, GN Asthana, R AF Singh, M Shpargel, TP Morscher, GN Asthana, R TI Active metal brazing and characterization of brazed joints in titanium to carbon-carbon composites SO MATERIALS SCIENCE AND ENGINEERING A-STRUCTURAL MATERIALS PROPERTIES MICROSTRUCTURE AND PROCESSING LA English DT Article; Proceedings Paper CT International Conference on Recent Advances in Composite Materials (ICRACM 2004) CY DEC 17-19, 2004 CL Banaras Hindu Univ, Varanasi, INDIA HO Banaras Hindu Univ ID ALUMINA; ALLOYS AB The Ti-metal/C-C composite joints were formed by reactive brazing with three commercial brazes, namely, Cu-ABA, TiCuNi, and TiCuSil. The joint microstructures were examined using optical microscopy and scanning electron microscopy Coupled with energy dispersive X-ray spectrometry. The results of the microstructure analysis indicate Solute redistribution across the joint and possible metallurgical bond formation via interdiffusion, which led to good wetting and spreading. A tube-on-plate tensile test was used to evaluate joint strength of Ti-tube/C-C composite joints. The load-carrying ability was greatest for the Cu-ABA brazejoint structures. This system appeared to have the best braze spreading which resulted in a larger braze/C-C composite bonded area compared to the other two braze materials. Also, joint load-carrying ability was found to be higher for joint structures where the fiber tows in the Outer ply of the C-C composite were aligned perpendicular to the tube axis when compared to the case where fiber tows were aligned parallel to the tube axis. (c) 2005 Elsevier B.V. All rights reserved. C1 NASA, Glenn Res Ctr, QSS Grp Inc, Cleveland, OH 44135 USA. NASA, Glenn Res Ctr, Ohio Aerosp Inst, Cleveland, OH 44135 USA. Univ Wisconsin Stout, Dept Technol, Menomonie, WI 54751 USA. RP Singh, M (reprint author), NASA, Glenn Res Ctr, QSS Grp Inc, 21000 Brookpath Rd,MS 106-5, Cleveland, OH 44135 USA. EM msingh@grc.nasa.gov NR 21 TC 70 Z9 76 U1 4 U2 24 PU ELSEVIER SCIENCE SA PI LAUSANNE PA PO BOX 564, 1001 LAUSANNE, SWITZERLAND SN 0921-5093 J9 MAT SCI ENG A-STRUCT JI Mater. Sci. Eng. A-Struct. Mater. Prop. Microstruct. Process. PD DEC 5 PY 2005 VL 412 IS 1-2 SI SI BP 123 EP 128 DI 10.1016/j.msea.2005.08.179 PG 6 WC Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering SC Science & Technology - Other Topics; Materials Science; Metallurgy & Metallurgical Engineering GA 994MY UT WOS:000234037100022 ER PT J AU Waliser, DE Murtugudde, R Strutton, P Li, JL AF Waliser, DE Murtugudde, R Strutton, P Li, JL TI Subseasonal organization of ocean chlorophyll: Prospects for prediction based on the Madden-Julian Oscillation SO GEOPHYSICAL RESEARCH LETTERS LA English DT Article ID NINO-SOUTHERN-OSCILLATION; SEA-SURFACE TEMPERATURES; CENTRAL ARABIAN SEA; EQUATORIAL PACIFIC; EL-NINO; INTRASEASONAL OSCILLATION; PRIMARY PRODUCTIVITY; INFECTIOUS-DISEASE; MIXED-LAYER; VARIABILITY AB Analysis of satellite ocean color and rainfall data shows that the Madden-Julian Oscillation (MJO) produces systematic and significant variations in ocean surface Chlorophyll (Chl) in a number of regions across the tropical Indian and Pacific Oceans, including the northern Indian Ocean, a broad expanse of the northwestern tropical Pacific Ocean, and a number of near-coastal areas in the far eastern Pacific Ocean. Potential mechanisms for this modulation are examined with the result that wind-induced vertical entrainment at the base of the ocean mixed layer appears to play an important role. Given evidence that the MJO is predictable with 2-3 week lead-times, surface Chl may also be predictable at similar lead times with implications for the fishing industry and public health sectors concerned with cholera epidemics. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Maryland, Earth Syst Sci Interdisciplinary Ctr, College Pk, MD 20742 USA. Oregon State Univ, Coll Ocean & Atmospher Sci, Corvallis, OR 97331 USA. RP Waliser, DE (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr,MS 183-501, Pasadena, CA 91109 USA. EM duane.waliser@jpl.nasa.gov RI Strutton, Peter/C-4466-2011 OI Strutton, Peter/0000-0002-2395-9471 NR 30 TC 41 Z9 41 U1 0 U2 11 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0094-8276 EI 1944-8007 J9 GEOPHYS RES LETT JI Geophys. Res. Lett. PD DEC 3 PY 2005 VL 32 IS 23 AR L23602 DI 10.1029/2005GL024300 PG 4 WC Geosciences, Multidisciplinary SC Geology GA 993EJ UT WOS:000233936000005 ER PT J AU Geogdzhayev, IV Mishchenko, MI Terez, EI Terez, GA Gushchin, GK AF Geogdzhayev, IV Mishchenko, MI Terez, EI Terez, GA Gushchin, GK TI Regional advanced very high resolution radiometer-derived climatology of aerosol optical thickness and size SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID RETRIEVALS; OCEAN; DEPTH; RADIANCES; SPACE; MODEL; SIMULATIONS; SENSITIVITY; VALIDATION; ALGORITHM AB We have used the NASA Global Energy and Water Cycle Experiment (GEWEX) Global Aerosol Climatology Project data set of retrieved aerosol optical thickness and Angstrom exponent to construct and analyze regional aerosol climatologies for a number of areas affected by different aerosol types (such as dust, biomass burning, anthropogenic, or clear maritime aerosols) that exemplify the range of natural aerosol variation. We have found that variations in the number of individual pixels used to calculate monthly means associated with short- and long-term satellite orbit changes and instrument degradation have little effect on global and hemispherical values of the aerosol optical thickness and Angstrom exponent. Aerosol loads are found to be higher, and aerosol particles smaller, over the northern Atlantic Ocean off the coast of Europe and the eastern United States, rather than off the west coast, thereby indicating a significant impact of anthropogenic aerosols. The smallest background levels of maritime aerosols are found in the southern Pacific Ocean, with seasonal mean optical thicknesses as low as 0.1. We analyze time series of the aerosol optical thickness in the regions affected by dust outflows from the Sahara and Asian deserts and by biomass burning. An influence of anthropogenic aerosols associated with the high regional industrial activity is apparent in the eastern China Sea. Two distinct periods are identified in satellite and Sun photometer aerosol time series over the Black Sea with transition time around 1993. During the first period the aerosol loads in the region significantly exceeded the hemispherical mean, whereas in the second period they became very close. This change is linked to the reduction of the industrial output in that region. C1 Columbia Univ, NASA, Goddard Inst Space Studies, New York, NY 10025 USA. Crimean Astrophys Observ, UA-95000 Simferopol, Ukraine. Natl Taurida Vernadsky Univ, UA-95000 Simferopol, Ukraine. Karadag Res Geophys Observ, UA-98188 Feodosiya, Ukraine. RP Columbia Univ, NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM igor@giss.nasa.gov RI Mishchenko, Michael/D-4426-2012 NR 26 TC 28 Z9 30 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 3 PY 2005 VL 110 IS D23 AR D23205 DI 10.1029/2005JD006170 PG 12 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 993EN UT WOS:000233936600005 ER PT J AU Holzer, M Hall, TM Stull, RB AF Holzer, M Hall, TM Stull, RB TI Seasonality and weather-driven variability of transpacific transport SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID AIR-POLLUTION TRANSPORT; LONG-RANGE TRANSPORT; ASIAN DUST EVENT; APRIL 1998; NORTHEAST PACIFIC; UNITED-STATES; TRANSIT-TIME; OZONE; PERSPECTIVE; EMISSIONS AB We quantify transport from the industrialized regions of E Asia using the transit-time probability density function, G, to isolate the role of transport from any other factors, such as chemistry and deposition. Using the offline transport model MATCH driven by NCEP reanalyses, we calculate G, which is the mass fraction of air that had its last contact with the E-Asian source region during a given day, for each day of a three-year period. Ensemble means of G establish the climatological seasonal-mean transport from E Asia. Export from the source region is most efficient in spring, with nearly all E-Asian air involved in transpacific transport. In summer, E-Asian air is transported aloft across the Pacific and, in nearly equal measure, west over SE Asia to the Middle East. Winter transport is similar to that of spring, except winter has low-level transport to SE Asia. Fall transport is intermediate between that of summer and winter. For all seasons, the most probable transit times to N America are 6-8 days in the mid-to-upper troposphere and approximately one week (two for summer) longer at the surface. The surface signal of E-Asian air over N America is strongest in spring. Daily variability of transpacific transport is quantified in terms of the transit-time partitioned burden of E-Asian air over western N America. The standard deviation of the transit-time partitioned fluctuations has a nearly universal dependence on the corresponding seasonal-mean burden. The standard deviation peaks several days before the burden at a transit time of similar to 7 days. Lagged event and nonevent composites, based on the western N-American burden of E-Asian air, reveal that transport events are associated with dipolar wind perturbations over the eastern Pacific that are positioned and phased to receive enhanced Asian outflow. Surface-pressure correlations are consistent with an associated strengthened Pacific High and weakened Aleutian Low. C1 NASA, Goddard Inst Space Studies, New York, NY 10025 USA. Univ British Columbia, Dept Earth & Ocean Sci, Atmospher Sci Program, Vancouver, BC V6T 1Z4, Canada. Columbia Univ, Dept Appl Phys & Appl Math, New York, NY USA. Langara Coll, Dept Phys, Vancouver, BC, Canada. RP NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM mholzer@eos.ubc.ca; thall@giss.nasa.gov; rstull@eos.ubc.ca NR 38 TC 29 Z9 29 U1 1 U2 4 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 3 PY 2005 VL 110 IS D23 AR D23103 DI 10.1029/2005JD006261 PG 22 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 993EN UT WOS:000233936600006 ER PT J AU Minnis, P Yi, YH Huang, JP Ayers, K AF Minnis, P Yi, YH Huang, JP Ayers, K TI Relationships between radiosonde and RUC-2 meteorological conditions and cloud occurrence determined from ARM data SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID UPPER-AIR OBSERVATIONS; SOUTHERN GREAT-PLAINS; RELATIVE-HUMIDITY; VERTICAL STRUCTURE; TROPOPAUSE REGION; DISTRIBUTION LAW; CLIMATE; CIRRUS; RADAR; SURFACE AB Relationships between modeled and measured meteorological state parameters and cloudy and cloud-free conditions are examined using data taken over the ARM (Atmospheric Radiation Measurement) Southern Great Plains Central Facility between 1 March 2000 and 28 February 2001. Cloud vertical layering was determined from the Active Remotely Sensed Cloud Location product based on the ARM active sensor measurements. Both temperature and relative humidity (RH) observations from balloon-borne Vaisala RS80-15LH radiosonde (SONDE) and the Rapid Update Cycle (RUC) 40-km resolution model are highly correlated, but the SONDE RHs generally exceed those from RUC. Inside cloudy layers, the RH from SONDE is 2-14% higher than the RH from RUC at all pressure levels. Although the layer mean RH within clouds is much greater than the layer mean RH outside clouds or in clear skies, RH thresholds chosen as a function of temperature can more accurately diagnose cloud occurrence for either data set than a fixed RH threshold. For overcast clouds (cloud amount greater than or equal to 90%), it was found that the 50% probability RH threshold for diagnosing a cloud, within a given upper tropospheric layer, is roughly 90% for the SONDE and 80% for RUC data. For partial cloud cover (cloud amount is less than 90%), the SONDE RH thresholds are close to those for RUC at a given probability in upper tropospheric layers. Cloud probability was found to be only minimally dependent on vertical velocity. In the upper troposphere, SONDE ice-supersaturated air occurred in 8 and 35% of the clear and cloudy layers, respectively. The RH was distributed exponentially in the ice supersaturated layers as found in previous studies. The occurrence of high-altitude, ice-supersaturated layers in the RUC data was roughly half of that in the SONDE data. Optimal thresholds were derived as functions of temperature to define the best RH thresholds for accurately determining the mean cloud cover. For warm clouds the typical SONDE threshold exceeds 87%, while the RH thresholds for cold clouds are typically less than 80% and greater than 90% with respect to liquid and ice water, respectively. Preliminary comparisons with satellite data suggest that the relationships between cloudiness and RH and T determined here could be useful for improving the characterization of cloud vertical structure from satellite data by providing information about low-level clouds that were obscured by high-level clouds viewed by the satellite. The results have potential for improving computations of atmospheric heating rate profiles and estimates of aircraft icing conditions. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP NASA, Langley Res Ctr, Hampton, VA 23681 USA. EM p.minnis@larc.nasa.gov RI Minnis, Patrick/G-1902-2010 OI Minnis, Patrick/0000-0002-4733-6148 NR 45 TC 19 Z9 22 U1 0 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 3 PY 2005 VL 110 IS D23 AR D23204 DI 10.1029/2005JD006005 PG 19 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 993EN UT WOS:000233936600002 ER PT J AU Shindell, DT Faluvegi, G Emmons, LK AF Shindell, DT Faluvegi, G Emmons, LK TI Inferring carbon monoxide pollution changes from space-based observations SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID GENERAL-CIRCULATION MODEL; GLOBAL DISTRIBUTION; TROPOSPHERIC OZONE; GODDARD-INSTITUTE; OCTOBER 1994; MOPITT; EMISSIONS; APRIL; VALIDATION; INSTRUMENT AB We compare space-based measurements of carbon monoxide ( CO) during April 1994 and October 1984 and 1994 from the early MAPS instrument with those during 2000-2004 from the MOPITT instrument. We show that a three-dimensional global composition model can be used to account for differences in retrieval sensitivity between the two instruments and between the different years of MOPITT data. This allows direct comparison of CO amounts over most of the globe at different times. These types of changes in short-lived constituents cannot be assessed with local measurements. Though the existing space-based data are too sparse both temporally and geographically to allow trend estimates, we find substantial variations in midtropospheric CO between the different years in many continental-scale regions. During April, average CO is similar to 12-18 ppbv (similar to 10-20%) greater during 2000-2004 than during 1994 over North America, southeast Asia and North Africa though the global mean value is nearly the same. During October 1994, observations show CO enhancements of 15-20 ppbv relative to 1984 or 2000-2004 over South America and a similar, though slightly smaller (9-19 ppbv), enhancement globally. Southeast Asia, Europe and North America all show similar October CO levels in 1994 and 2000-2004, with both times showing substantially more pollution (13-29 ppbv) than 1984. Variations over Europe and Africa are consistent in both seasons, while changes elsewhere are not. Changes over southeast Asia and North Africa are substantially in excess of interannual variability, while those over North and South America and southern Africa are only marginally so. Model sensitivity studies examining the response to changes in emissions indicate probable causes of the CO changes over different regions. Over southeast Asia and North America, CO is most sensitive to industrial and biomass burning emissions, implying that changes in these sources likely account for the 13-29 ppbv increases seen there between 2000-2004 and earlier years. Over North Africa, CO is strongly influenced by numerous sources as well as meteorology, precluding attribution of increases to particular factors. Over South America and southern Africa, variations in both biomass burning and isoprene emissions likely contributed to the similar to 10-20 ppbv changes. C1 NASA, Goddard Inst Space Studies, New York, NY 10025 USA. Columbia Univ, Ctr Climate Syst Res, New York, NY 10027 USA. Natl Ctr Atmospher Res, Boulder, CO 80307 USA. RP Shindell, DT (reprint author), NASA, Goddard Inst Space Studies, New York, NY 10025 USA. EM dshindell@giss.nasa.gov RI Shindell, Drew/D-4636-2012; Emmons, Louisa/R-8922-2016 OI Emmons, Louisa/0000-0003-2325-6212 NR 25 TC 13 Z9 14 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 3 PY 2005 VL 110 IS D23 AR D23303 DI 10.1029/2005JD006132 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 993EN UT WOS:000233936600004 ER PT J AU Huddleston, MM Chappell, CR Delcourt, DC Moore, TE Giles, BL Chandler, MO AF Huddleston, MM Chappell, CR Delcourt, DC Moore, TE Giles, BL Chandler, MO TI An examination of the process and magnitude of ionospheric plasma supply to the magnetosphere SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID MASS-SPECTROMETER OBSERVATIONS; POLAR WIND; ION OUTFLOW; EARTHS MAGNETOTAIL; MAGNETIC ACTIVITY; O+ IONS; SHEET; DYNAMICS; DISTRIBUTIONS; ACCELERATION AB [1] The contribution of ionospheric plasma to the Earth's magnetosphere has been recognized for more than 3 decades. The magnitude of this contribution has become more evident over that same time period with the observed magnitude of the low-energy ionospheric supply increasing as the measurement techniques improved. Estimates based on Dynamics Explorer measurements in the mid-1980s suggested that the ionospheric plasma supply is sufficient to populate the plasmasphere, plasma trough, plasma sheet, and magnetotail lobes. Recent measurements from the Thermal Ion Dynamics Experiment on the Polar spacecraft have been used in conjunction with an ion trajectory model to reexamine the process and magnitude of the ionospheric supply of magnetospheric plasma. These measurements reveal the energy, pitch angle, and flux characteristics of the upward flowing polar wind over broad regions of the high-latitude ionosphere. Onboard measurement of spacecraft potential is found to be a fundamental element in interpreting the measured ion outflow. Newly derived polar wind fluxes are determined to be near 6.0 x 10(7) ions cm(-2) s(-1) at 5000 km altitude during local winter and magnetically quiet conditions. Using the measured ionospheric source characteristics in combination with the trajectory code reveals the nature of the ionospheric/ magnetosphere filling process and shows that the ionospheric source is sufficient to supply the observed densities and energies of the plasma sheet and magnetotail lobes. Many of the ionospheric particles are further transformed to ring current energies and locations after circulation through the plasma sheet. This measurement/ calculation approach is able to show which regions of the high-latitude ionosphere are important for plasma sheet/ring current filling. The ionospheric sources used in the calculations include the dominant polar wind, the cleft ion fountain, and the auroral zone. C1 Harpeth Hall Sch, Nashville, TN 37215 USA. Vanderbilt Univ, Nashville, TN 37235 USA. CNRS, IPSL, Observ St Maur, Ctr Etud Environm Terr & Planetaires, F-94107 St Maur des Fosses, France. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Harpeth Hall Sch, 3801 Hobbs Rd, Nashville, TN 37215 USA. EM huddleston@harpethhall.org RI Moore, Thomas/D-4675-2012 OI Moore, Thomas/0000-0002-3150-1137 NR 61 TC 44 Z9 44 U1 1 U2 6 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9380 EI 2169-9402 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 3 PY 2005 VL 110 IS A12 AR A12202 DI 10.1029/2004JA010401 PG 29 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993OS UT WOS:000233964000001 ER PT J AU Taguchi, S Chen, SH Collier, MR Moore, TE Fok, MC Hosokawa, K Nakao, A AF Taguchi, S Chen, SH Collier, MR Moore, TE Fok, MC Hosokawa, K Nakao, A TI Monitoring the high-altitude cusp with the Low Energy Neutral Atom imager: Simultaneous observations from IMAGE and Polar SO JOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICS LA English DT Article ID INTERPLANETARY MAGNETIC-FIELD; SOLAR-WIND CONDITIONS; AURORAL ACTIVITY; TIME-VARIATION; B-Z; MAGNETOSPHERE; CLEFT; DEPENDENCE; LATITUDE; EROSION AB [1] The Low Energy Neutral Atom (LENA) imager on the IMAGE spacecraft in the dayside magnetosphere can detect neutral particles that are emitted in the magnetosheath flow. During a period of dynamic pressure of 4 - 6 nPa and interplanetary magnetic field (IMF) B-z of - 5 to 3 nT on 12 April 2001, LENA on IMAGE at (X-GSM, Y-GSM, Z(GSM)) similar to (4 R-E, 0 R-E, 6 R-E) observed significant emission in the direction of the high-latitude magnetosheath. Detailed analyses have revealed that the high-latitude sheath emission consists of two parts: the stable emission at the higher latitudes and the lower-latitude emission that occurs on and off. During the interval of this event, the Polar spacecraft was located at somewhat lower latitudes than IMAGE in similar noon meridian, and the plasma observations with the Thermal Ions Dynamic Experiment showed that the entry of the cusp ions happens in concurrence with the appearance of the lower-latitude LENA emission. This coincidence strongly suggests that the cusp ions flowing earthward charge exchange with the hydrogen exosphere. For the higher-latitude emission, its stability suggests that the source is associated with the structure persistently existing, which is consistent with the recent result showing that the sheath flow in the cusp indentation can create neutral atom emissions. Comparison of the LENA emission and ACE solar wind suggests that the lower-latitude LENA emission occurs during the southward tilting of dawnward IMF, indicating that this emission is associated with the earthward ion flux along the newly reconnected field lines. Hence this unique event for the simultaneous observations strongly suggests that LENA monitors the entry of the ions in the cusp, which is triggered by the southward tilting of the IMF, and that the significant flux of the cusp ion entry occurs equatorward of and separately from the cusp indentation. C1 Univ Electrocommun, Dept Informat & Commun Engn, Tokyo 1828585, Japan. NASA, Goddard Space Flight Ctr, Univ Space Res Assoc, Greenbelt, MD 20771 USA. RP Taguchi, S (reprint author), Univ Electrocommun, Dept Informat & Commun Engn, Tokyo 1828585, Japan. EM taguchi@ice.uec.ac.jp RI Moore, Thomas/D-4675-2012; Fok, Mei-Ching/D-1626-2012; Collier, Michael/I-4864-2013 OI Moore, Thomas/0000-0002-3150-1137; Collier, Michael/0000-0001-9658-6605 NR 34 TC 12 Z9 12 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-SPACE JI J. Geophys. Res-Space Phys. PD DEC 3 PY 2005 VL 110 IS A12 AR A12204 DI 10.1029/2005JA011075 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993OS UT WOS:000233964000003 ER PT J AU Golden, DC Ming, DW Morris, RV Mertzman, SA AF Golden, DC Ming, DW Morris, RV Mertzman, SA TI Laboratory-simulated acid-sulfate weathering of basaltic materials: Implications for formation of sulfates at Meridiani Planum and Gusev crater, Mars SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Article ID X-RAY SPECTROMETER; OMEGA/MARS EXPRESS; SPIRIT ROVER; MOSSBAUER SPECTROMETER; ROCKS; SOILS; HEMATITE; MINERALOGY; CHEMISTRY; JAROSITE AB [1] Acid-sulfate weathering of basaltic materials is a candidate formation process for the sulfate-rich outcrops and rocks at the MER rover Opportunity and Spirit landing sites. To determine the style of acid-sulfate weathering on Mars, we weathered basaltic materials (olivine-rich glassy basaltic sand and plagioclase feldspar-rich basaltic tephra) in the laboratory under different oxidative, acid-sulfate conditions and characterized the alteration products. We investigated alteration by ( 1) sulfuric-acid vapor ( acid fog), ( 2) three-step hydrothermal leaching treatment approximating an "open system,'' and ( 3) single-step hydrothermal batch treatment approximating a "closed system.'' In acid fog experiments, Al-, Fe-, and Ca-sulfates and amorphous silica formed from plagioclase-rich tephra, and Mg- and Ca-sulfates and amorphous silica formed from the olivine-rich sands. In three-step leaching experiments, only amorphous Si formed from the plagioclase-rich basaltic tephra, and jarosite, Mg-, and Ca-sulfates and amorphous silica formed from olivine-rich basaltic sand. Amorphous silica formed under single-step experiments for both starting materials. On the basis of our experiments, jarosite formation in Meridiani outcrop is potential evidence for an open system acid-sulfate weathering regime. Waters rich in sulfuric acid percolated through basaltic sediment, dissolving basaltic phases (e.g., olivine) and forming jarosite, other sulfates, and iron oxides. Aqueous alteration of outcrops and rocks on the West Spur of the Columbia Hills may have occurred when vapors rich in SO(2) from volcanic sources reacted with basaltic materials. Soluble ions from the host rock (e.g., olivine) reacted with S to form Ca-, Mg-, and other sulfates along with iron oxides and oxyhydroxides. C1 ESCG UTC HS, Houston, TX 77058 USA. NASA, Lyndon B Johnson Space Ctr, Astromat Res & Explorat Sci Directorate, Houston, TX 77058 USA. Franklin & Marshall Coll, Dept Geosci, Lancaster, PA 17604 USA. RP Golden, DC (reprint author), ESCG UTC HS, Mail Code JE 23,2224 Bay Area Blvd,Box 7, Houston, TX 77058 USA. EM douglas.w.ming@nasa.gov NR 44 TC 47 Z9 47 U1 3 U2 16 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 0148-0227 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD DEC 2 PY 2005 VL 110 IS E12 AR E12S07 DI 10.1029/2005JE002451 PG 15 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 993OM UT WOS:000233963400003 ER PT J AU Irwin, RP Howard, AD Craddock, RA Moore, JM AF Irwin, RP Howard, AD Craddock, RA Moore, JM TI An intense terminal epoch of widespread fluvial activity on early Mars: 2. Increased runoff and paleolake development SO JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS LA English DT Review ID MARGARITIFER SINUS; MARTIAN HIGHLANDS; VALLEY NETWORKS; GALE-CRATER; AQUEOUS SEDIMENTATION; DRAINAGE BASINS; FRETTED TERRAIN; IMPACT CRATERS; SUN PARADOX; YOUNG SUN AB [1] To explain the much higher denudation rates and valley network development on early Mars (> similar to 3.6 Gyr ago), most investigators have invoked either steady state warm/wet (Earthlike) or cold/dry ( modern Mars) end-member paleoclimates. Here we discuss evidence that highland gradation was prolonged, but generally slow and possibly ephemeral during the Noachian Period, and that the immature valley networks entrenched during a brief terminal epoch of more erosive fluvial activity in the late Noachian to early Hesperian. Observational support for this interpretation includes ( 1) late-stage breaching of some enclosed basins that had previously been extensively modified, but only by internal erosion and deposition; ( 2) deposition of pristine deltas and fans during a late stage of contributing valley entrenchment; ( 3) a brief, erosive response to base level decline ( which was imparted as fretted terrain developed by a suite of processes unrelated to surface runoff) in fluvial valleys that crosscut the highland-lowland boundary scarp; and ( 4) width/contributing area relationships of interior channels within valley networks, which record significant late-stage runoff production with no evidence of recovery to lower-flow conditions. This erosion appears to have ended abruptly, as depositional landforms generally were not entrenched with declining base level in crater lakes. A possible planetwide synchronicity and common cause to the late-stage fluvial activity are possible but remain uncertain. This increased activity of valley networks is offered as a possible explanation for diverse features of highland drainage basins, which were previously cited to support competing warm, wet and cold, dry paleoclimate scenarios. C1 Smithsonian Inst, Ctr Earth & Planetary Studies, Natl Air & Space Museum, Washington, DC 20013 USA. Univ Virginia, Dept Environm Sci, Charlottesville, VA 22904 USA. NASA, Ames Res Ctr, Div Space Sci, Moffett Field, CA 94035 USA. RP Smithsonian Inst, Ctr Earth & Planetary Studies, Natl Air & Space Museum, 6th St & Independence Ave SW, Washington, DC 20013 USA. EM irwinr@si.edu; ah6p@virginia.edu; jeff.moore@nasa.gov RI Craddock, Robert/B-3884-2013; OI Howard, Alan/0000-0002-5423-1600 NR 114 TC 103 Z9 104 U1 0 U2 0 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-9097 EI 2169-9100 J9 J GEOPHYS RES-PLANET JI J. Geophys. Res.-Planets PD DEC 2 PY 2005 VL 110 IS E12 AR E12S15 DI 10.1029/2005JE002460 PG 38 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 993OM UT WOS:000233963400005 ER PT J AU Jakosky, BM Haberle, RM Arvidson, RE AF Jakosky, BM Haberle, RM Arvidson, RE TI The changing picture of volatiles and climate on Mars SO SCIENCE LA English DT Editorial Material ID GROUND ICE; MERIDIANI; CAP C1 Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. Univ Colorado, Dept Geol Sci, Boulder, CO 80309 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Washington Univ, Dept Earth & Planetary Sci, St Louis, MO 63130 USA. RP Jakosky, BM (reprint author), Univ Colorado, Atmospher & Space Phys Lab, Boulder, CO 80309 USA. EM bruce.jakosky@lasp.colorado.edu NR 17 TC 11 Z9 11 U1 0 U2 3 PU AMER ASSOC ADVANCEMENT SCIENCE PI WASHINGTON PA 1200 NEW YORK AVE, NW, WASHINGTON, DC 20005 USA SN 0036-8075 J9 SCIENCE JI Science PD DEC 2 PY 2005 VL 310 IS 5753 BP 1439 EP 1440 DI 10.1126/science.1118031 PG 2 WC Multidisciplinary Sciences SC Science & Technology - Other Topics GA 990PU UT WOS:000233756500028 PM 16322442 ER PT J AU Lind, R Prazenica, RJ Brenner, MJ Baldelli, DH AF Lind, R Prazenica, RJ Brenner, MJ Baldelli, DH TI Identifying parameter-dependent Volterra kernels to predict aeroelastic instabilities SO AIAA JOURNAL LA English DT Article; Proceedings Paper CT AIAA/ASME/ASCE/AHS/ASC 45th Structures, Structural Dynamics and Materials Conference CY APR 19-22, 2004 CL Palm Springs, CA SP Amer Inst Aeronaut & Astronaut, ASME, ASCE, AHS, ASC ID ROBUST FLUTTER ANALYSIS; REDUCED-ORDER MODELS AB Flight testing for envelope expansion remains dangerous and costly because of difficulties inaccurately predicting the onset of flutter. Approaches have been developed that are able to identify optimal models of the acroelastic dynamics based on flight data but are not able to predict the responses at all airspeeds. Those previous approaches are extended to include parameter variations in the optimal models. Specifically, parameter-varying models of Volterra kernels are identified for inclusion with theoretical models in aeroelastic analysis. The new approach is applied to a pitch-plunge system to demonstrate the accuracy achieved in predicting the onset of flutter by analyzing data obtained at lower airspeeds. C1 Univ Florida, Dept Mech & Aerosp Engn, Gainesville, FL 32611 USA. NASA, Dryden Flight Res Ctr, Aerostruct Branch, Edwards AFB, CA 93523 USA. ZONA Technol, Scottsdale, AZ 85251 USA. RP Lind, R (reprint author), Univ Florida, Dept Mech & Aerosp Engn, 231 Aerosp Bldg, Gainesville, FL 32611 USA. EM ricklind@ufl.edu; chad.prazenica@dfrc.nasa.gov; martin.j.brenner@nasa.gov; dario@zonatech.com NR 18 TC 11 Z9 13 U1 0 U2 3 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 J9 AIAA J JI AIAA J. PD DEC PY 2005 VL 43 IS 12 BP 2496 EP 2502 DI 10.2514/1.12042 PG 7 WC Engineering, Aerospace SC Engineering GA 991YL UT WOS:000233850700005 ER PT J AU Wright, MJ Bose, D Palmer, GE Levin, E AF Wright, MJ Bose, D Palmer, GE Levin, E TI Recommended collision integrals for transport property computations, part 1: Air species SO AIAA JOURNAL LA English DT Article ID ENERGY-ELECTRON-SCATTERING; VISCOSITY CROSS-SECTIONS; ION-NEUTRAL INTERACTIONS; IONIZED-GASES; ELASTIC-SCATTERING; MOLECULAR NITROGEN; ATOMIC NITROGEN; OXYGEN; COEFFICIENTS; ARGON AB A review of the best-available data for calculating a complete set of binary collision integral data for the computation of the mixture transport properties (viscosity, thermal conductivity, and ordinary and thermal diffusion) of 13-species weakly ionized air is presented. Although the fidelity of the data varies, all collision integrals presented herein, except for electron-neutral interactions, are estimated to be accurate to within 25% over the temperature range of interest (300-15,000 K) for reentry and laboratory plasmas. In addition, most of the dominant atom-atom and atom-ion interactions for dissociated weakly ionized air were derived from ab initio methods that are estimated to be accurate to within 10%. The accuracy and valid temperature range for electron-neutral interactions vary because of scarcity of the required cross-sectional data. C1 NASA, Ames Res Ctr, Reacting Flow Environm Branch, Moffett Field, CA 94035 USA. NASA, Ames Res Ctr, Eloret Corp, Moffett Field, CA 94035 USA. RP NASA, Ames Res Ctr, Reacting Flow Environm Branch, MS 230-2, Moffett Field, CA 94035 USA. NR 53 TC 76 Z9 77 U1 2 U2 9 PU AMER INST AERONAUTICS ASTRONAUTICS PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 EI 1533-385X J9 AIAA J JI AIAA J. PD DEC PY 2005 VL 43 IS 12 BP 2558 EP 2564 DI 10.2514/1.16713 PG 7 WC Engineering, Aerospace SC Engineering GA 991YL UT WOS:000233850700011 ER PT J AU Moss, JN Bird, GA AF Moss, JN Bird, GA TI Direct simulation Monte Carlo Simulations of hypersonic flows with shock interactions SO AIAA JOURNAL LA English DT Article; Proceedings Paper CT AIAA 37th Thermophysics Conference CY JUN 28-JUL 01, 2004 CL Portland, OR SP AIAA AB The capabilities of a relatively new direct simulation Monte Carlo (DSMC) code are examined for the problem of hypersonic laminar shock/shock and shock/boundary-layer interactions, where boundary-layer separation is an important feature of the How. Flow about two model configurations is considered, where both configurations (a biconic and a hollow cylinder-Hare) have recent published experimental measurements. The computations are made using the DS2V code of Bird, a general two-dimensional/axisymmetric time-accurate code. The current focus is on flows produced in ground-based facilities at Mach 12 and 16 test conditions with nitrogen as the test gas and the test models at zero incidence. The freestream Knudsen numbers, with the characteristic length equal to the test model diameter, range from 0.0008 to 0.0004, consequently demanding computations for DSMC simulations. Results presented highlight the sensitivity of the calculations to grid resolution, sensitivity to physical modeling parameters, and comparison with experimental measurements. Information is provided concerning the flow structure and surface results for the extent of separation, heating, pressure, and skin friction. C1 NASA, Langley Res Ctr, Aerothermodynam Branch, Hampton, VA 23681 USA. GAB Consulting Pty Ltd, Sydney, NSW 2000, Australia. Univ Sydney, Sch Aerosp Mech & Mechatron Engn, Sydney, NSW 2006, Australia. RP Bird, GA (reprint author), NASA, Langley Res Ctr, Aerothermodynam Branch, MS 408A, Hampton, VA 23681 USA. EM j.n.moss@larc.nasa.gov; gabird@compuserve.com NR 19 TC 25 Z9 27 U1 2 U2 7 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 J9 AIAA J JI AIAA J. PD DEC PY 2005 VL 43 IS 12 BP 2565 EP 2573 DI 10.2514/1.12532 PG 9 WC Engineering, Aerospace SC Engineering GA 991YL UT WOS:000233850700012 ER PT J AU Guo, B Holder, DW Tester, JT AF Guo, B Holder, DW Tester, JT TI Two-phase oxidizing flow in volatile removal assembly reactor under microgravity conditions SO AIAA JOURNAL LA English DT Article ID PERCOLATION; LIQUID AB Volatile removal assembly (VRA) is a module installed in the International Space Station for removing contaminants (volatile organics) in the wastewater produced by the crew. The VRA contains a slim pack-bed reactor to perform catalyst oxidation of the wastewater at elevated pressure and temperature under microgravity conditions. Optimal design of the reactor requires a thorough understanding about how the reactor performs under microgravity conditions. The efficiency of catalyst oxidation is controlled by catalyst oxidation kinetics and oxygen gas distribution in the reactor. The process involves bubbly flow in porous media with chemical reactions in microgravity environment, which has not been previously studied. We have developed and used a mathematical model in this study to simulate the organics oxidation process in the VRA reactor. We conclude that 1) the remaining oxygen gas in the VRA reactor should decline exponentially with reactor length; 2) the minimum reactor length required to achieve a complete oxygen utilization is directly proportional to bubble size, oxygen density, and bubble velocity, and inversely proportional to rate of oxidation per unit area and bubble sphericity; 3) gravity affects oxygen utilization through changing several parameters including oxygen bubble size; and 4) the example VRA design is very conservative. C1 Univ Louisiana, Dept Petr Engn, Lafayette, LA 70504 USA. NASA, George C Marshall Space Flight Ctr, Flight Project Directorate, Huntsville, AL 35812 USA. No Arizona Univ, Dept Mech Engn, Flagstaff, AZ 86011 USA. RP Guo, B (reprint author), Univ Louisiana, Dept Petr Engn, POB 44690, Lafayette, LA 70504 USA. EM boyun.guo@louisiana.edu; donald.w.holder@nasa.gov; john.tester@nau.edu NR 12 TC 1 Z9 1 U1 1 U2 4 PU AMER INST AERONAUT ASTRONAUT PI RESTON PA 1801 ALEXANDER BELL DRIVE, STE 500, RESTON, VA 22091-4344 USA SN 0001-1452 J9 AIAA J JI AIAA J. PD DEC PY 2005 VL 43 IS 12 BP 2586 EP 2592 DI 10.2514/1.12267 PG 7 WC Engineering, Aerospace SC Engineering GA 991YL UT WOS:000233850700014 ER PT J AU Kiang, RK Adimi, F Zollner, GE Coleman, RE AF Kiang, Richard K. Adimi, Farida Zollner, Gabriela E. Coleman, Russell E. TI Dynamic modeling of malaria transmissions with applications to a study site in western Thailand SO AMERICAN JOURNAL OF TROPICAL MEDICINE AND HYGIENE LA English DT Meeting Abstract C1 [Kiang, Richard K.; Adimi, Farida] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. [Zollner, Gabriela E.; Coleman, Russell E.] Walter Reed Army Inst Res, Silver Spring, MD USA. NR 0 TC 0 Z9 0 U1 1 U2 1 PU AMER SOC TROP MED & HYGIENE PI MCLEAN PA 8000 WESTPARK DR, STE 130, MCLEAN, VA 22101 USA SN 0002-9637 J9 AM J TROP MED HYG JI Am. J. Trop. Med. Hyg. PD DEC PY 2005 VL 73 IS 6 SU S MA 64 BP 22 EP 22 PG 1 WC Public, Environmental & Occupational Health; Tropical Medicine SC Public, Environmental & Occupational Health; Tropical Medicine GA V44GA UT WOS:000202990000065 ER PT J AU Kiang, RK Adimi, F Soilka, V Nigro, JD AF Kiang, Richard K. Adimi, Farida Soilka, Valerii Nigro, Joseph D. TI Assessing malaria risks in Thailand using meteorological and environmental parameters SO AMERICAN JOURNAL OF TROPICAL MEDICINE AND HYGIENE LA English DT Meeting Abstract C1 [Kiang, Richard K.; Adimi, Farida; Nigro, Joseph D.] NASA Goddard Space Flight Ctr, Greenbelt, MD USA. [Soilka, Valerii] Sci Syst & Applicat Inc, Landover, MD USA. NR 0 TC 0 Z9 0 U1 0 U2 0 PU AMER SOC TROP MED & HYGIENE PI MCLEAN PA 8000 WESTPARK DR, STE 130, MCLEAN, VA 22101 USA SN 0002-9637 J9 AM J TROP MED HYG JI Am. J. Trop. Med. Hyg. PD DEC PY 2005 VL 73 IS 6 SU S MA 847 BP 279 EP 279 PG 1 WC Public, Environmental & Occupational Health; Tropical Medicine SC Public, Environmental & Occupational Health; Tropical Medicine GA V44GA UT WOS:000202990001270 ER PT J AU Einstein, DR Freed, AD Stander, N Fata, B Vesely, I AF Einstein, DR Freed, AD Stander, N Fata, B Vesely, I TI Inverse parameter fitting of biological tissues: A response surface approach SO ANNALS OF BIOMEDICAL ENGINEERING LA English DT Article; Proceedings Paper CT International Biofluids Mechanics Symposium CY DEC 12-14, 2003 CL Pasadena, CA SP US Natl Comm Biomech, Biomed Engn Soc, Int Federat Med & Biol Engn DE LS-OPT; nonlinear continuum mechanics; finite element analysis ID FINITE-ELEMENT CHARACTERIZATION; SOFT-TISSUES; OPTIMIZATION AB In this paper, we present the application of a semiglobal inverse method for determining material parameters of biological tissues. The approach is based on the successive response surface method, and is illustrated by fitting constitutive parameters to two nonlinear anisotropic constitutive equations, one for aortic sinus and aorticwall, the other for aortic valve tissue. Material test data for the aortic sinus consisted of two independent orthogonal uniaxial tests. Material test data for the aortic valve was obtained from a dynamic inflation test. In each case, a numerical simulation of the experiment was performed and predictions were compared to the real data. For the uniaxial test simulation, the experimental targets were force at a measured displacement. For the inflation test, the experimental targets were the three-dimensional coordinates of material markers at a given pressure. For both sets of tissues, predictions with converged parameters showed excellent agreement with the data, and we found that the method was able to consistently identify model parameters. We believe the method will find wide application in biomedical material characterization and in diagnostic imaging. C1 Pacific NW Normal Lab, Richland, WA 99354 USA. NASA, John H Glenn Res Ctr, Biosci & Technol Branch, Cleveland, OH USA. Livermore Software Technol Corp, Livermore, CA USA. Univ So Calif, Dept Biomed Engn, Los Angeles, CA 90089 USA. Univ So Calif, Keck Sch Med, Los Angeles, CA USA. Childrens Hosp Los Angeles, Los Angeles, CA 90027 USA. RP Pacific NW Normal Lab, 790 6th St,MS P7-56, Richland, WA 99354 USA. EM daniel.einstein@pnl.gov OI Freed, Alan/0000-0002-3492-0628 NR 21 TC 18 Z9 18 U1 1 U2 3 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 0090-6964 EI 1573-9686 J9 ANN BIOMED ENG JI Ann. Biomed. Eng. PD DEC PY 2005 VL 33 IS 12 BP 1819 EP 1830 DI 10.1007/s10439-005-8338-3 PG 12 WC Engineering, Biomedical SC Engineering GA 999NC UT WOS:000234395300020 PM 16389530 ER PT J AU Ivins, ER James, TS AF Ivins, ER James, TS TI Antarctic glacial isostatic adjustment: a new assessment SO ANTARCTIC SCIENCE LA English DT Article; Proceedings Paper CT 2004 SCAR Open Science Conference CY JUL, 2004 CL Bremen, GERMANY SP SCAR DE Antarctica; glacial isostasy; global geodesy; GRACE satellites; mantle viscosity ID SEA-LEVEL CHANGE; SUBSEQUENT RETREAT HISTORY; WESTERN ROSS-SEA; MARIE-BYRD-LAND; ICE-SHEET; LATE-PLEISTOCENE; EAST ANTARCTICA; MASS-BALANCE; HOLOCENE DEGLACIATION; COSMOGENIC NUCLIDES AB The prediction of crustal motions and gravity change driven by glacial isostatic adjustment (GIA) in Antarctica is critically dependent on the reconstruction of the configuration and thickness of the ice sheet during the Late Pleistocene and Holocene. The collection and analysis of field data to improve the reconstruction has occurred at an accelerated pace during the past decade. At the same time, space-based imaging and altimetry, combined with on-ice velocity measurements using Global Positioning System (GPS) geodesy, has provided better assessments of the present-day mass balance of the Antarctic ice sheet. Present-day mass change appears to be dominated by deglaciation that is, in large part, a continuation of late-Holocene evolution. Here a new ice load model is constructed, based on a synthesis of the current constraints on past ice history and present-day mass balance. The load is used to predict GIA crustal motion and geoid change. Compared to existing glacioisostatic models, the new ice history model is significantly improved in four aspects: (i) the timing of volume losses in the region ranging from the Ross Sea sector to the Antarctic Peninsula, (ii) the maximum ice heights in parts of the Ellsworth and Transantarctic Mountains, (iii) maximum grounding line position in Pine Island Bay, the Antarctic Peninsula, and in the Ross Sea, (iv) incorporation of present-day net mass balance estimates. The predicted present-day GIA uplift rates peak at 14-18 min yr(-1) and geoid rates peak at 4-5 mm yr(-1) for two contrasting viscosity models. If the asthenosphere underlying West Antarctica has a low viscosity then the predictions could change substantially due to the extreme sensitivity to recent (past two millennia) ice mass variability. Future observations of crustal motion and gravity change will substantially improve the understanding of sub-Antarctic lithospheric and mantle theology. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Geol Survey Canada, Sidney, BC V8L 4B2, Canada. RP Ivins, ER (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM eri@fryxell.jpl.nasa.gov RI James, Thomas/D-9301-2013 OI James, Thomas/0000-0001-7321-047X NR 91 TC 131 Z9 138 U1 3 U2 25 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 32 AVENUE OF THE AMERICAS, NEW YORK, NY 10013-2473 USA SN 0954-1020 J9 ANTARCT SCI JI Antarct. Sci. PD DEC PY 2005 VL 17 IS 4 BP 541 EP 553 DI 10.1017/S0954102005002968 PG 13 WC Environmental Sciences; Geography, Physical; Geosciences, Multidisciplinary SC Environmental Sciences & Ecology; Physical Geography; Geology GA 990FE UT WOS:000233727800008 ER PT J AU Newcombe, DA Schuerger, AC Benardini, JN Dickinson, D Tanner, R Venkateswaran, K AF Newcombe, DA Schuerger, AC Benardini, JN Dickinson, D Tanner, R Venkateswaran, K TI Survival of spacecraft-associated microorganisms under simulated Martian UV irradiation SO APPLIED AND ENVIRONMENTAL MICROBIOLOGY LA English DT Article ID BACILLUS-SUBTILIS SPORES; MARS ODYSSEY SPACECRAFT; ATMOSPHERIC-PRESSURE; ASSEMBLY FACILITY; HYDROGEN-PEROXIDE; BACTERIAL-SPORES; SOLAR-RADIATION; SP NOV.; ENVIRONMENT; RESISTANCE AB Spore-forming microbes recovered from spacecraft surfaces and assembly facilities were exposed to simulated Martian UV irradiation. The effects of UVA (315 to 400 nm), UVA+B (280 to 400 nm), and the full UV spectrum (200 to 400 nm) on the survival of microorganisms were studied at UV intensities expected to strike the surfaces of Mars. Microbial species isolated from the surfaces of several spacecraft, including Mars Odyssey, X-2000 (avionics), and the International Space Station, and their assembly facilities were identified using 16S rRNA gene sequencing. Forty-three Bacillus spore lines were screened, and 19 isolates showed resistance to UVC irradiation (200 to 280 nm) after exposure to 1,000 J m(-2) of UVC irradiation at 254 nm using a low-pressure mercury lamp. Spores of Bacillus species isolated from spacecraft-associated surfaces were more resistant than a standard dosimetric strain, Bacillus subtilis 168. In addition, the exposure time required for UVA+B irradiation to reduce the viable spore numbers by 90% was 35-fold longer than the exposure time required for the full UV spectrum to do this, confirming that UVC is the primary biocidal bandwidth. Among the Bacillus species tested, spores of a Bacillus pumilus strain showed the greatest resistance to all three UV bandwidths, as well as the total spectrum. The resistance to simulated Mars UV irradiation was strain specific; B. pumilus SAFR-032 exhibited greater resistance than all other strains tested. The isolation of organisms like B. pumilus SAFR-032 and the greater survival of this organism (sixfold) than of the standard dosimetric strains should be considered when the sanitation capabilities of UV irradiation are determined. C1 CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, Pasadena, CA 91109 USA. Univ Florida, Dept Plant Pathol, Space Life Sci Lab, Kennedy Space Ctr, Kennedy Space Ctr, FL 32899 USA. Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. RP Venkateswaran, K (reprint author), CALTECH, Jet Prop Lab, Biotechnol & Planetary Protect Grp, Mail Stop 89,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM kjvenkat@jpl.nasa.gov NR 57 TC 79 Z9 80 U1 1 U2 15 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 DEC PY 2005 VL 71 IS 12 BP 8147 EP 8156 DI 10.1128/AEM.71.12.8147-8156.2005 PG 10 WC Biotechnology & Applied Microbiology; Microbiology SC Biotechnology & Applied Microbiology; Microbiology GA 999VB UT WOS:000234417600063 PM 16332797 ER PT J AU Vann, LB DeYoung, RJ Mihailov, SJ Lu, P Grobnic, D Walker, R AF Vann, LB DeYoung, RJ Mihailov, SJ Lu, P Grobnic, D Walker, R TI Narrowband fiber-optic phase-shifted Fabry-Perot Bragg grating filters for atmospheric water vapor lidar measurements SO APPLIED OPTICS LA English DT Article AB A unique ultranarrowband fiber-optic phase-shifted Fabry-Perot Bragg grating filter for atmospheric water vapor lidar measurements was designed, fabricated, and successfully tested. Customized optical fiber Bragg gratings were fabricated so that two transmission filter peaks occurred: one (89% transmission, 8 pro FWHM) near the 946-nm water vapor absorption line and the other peak (80% transmission, 4 pin FWHM) at a region of no absorption. Both transmission peaks were within a 2.66-nm stop band. Demonstration of tension tuning to the 946.0003-nm water vapor line was achieved, and the performance characterization of custom-made optical fiber Bragg grating filters are presented. These measurements are successfully compared to theoretical calculations using a piecewise-matrix form of the coupled-mode equations. (c) 2005 Optical Society of America. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. Commun Res Ctr, Ottawa, ON K2H 8S2, Canada. RP Vann, LB (reprint author), NASA, Langley Res Ctr, MS401, Hampton, VA 23681 USA. EM russell.j.deyoung@nasa.gov RI Mihailov, Stephen/E-2687-2013 NR 9 TC 9 Z9 10 U1 1 U2 2 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 DEC 1 PY 2005 VL 44 IS 34 BP 7371 EP 7377 DI 10.1364/AO.44.007371 PG 7 WC Optics SC Optics GA 989LH UT WOS:000233674700017 PM 16353809 ER PT J AU Hoge, FE AF Hoge, FE TI Oceanic inherent optical properties: proposed single laser lidar and retrieval theory SO APPLIED OPTICS LA English DT Article ID DISSOLVED ORGANIC-MATTER; FLUORESCENCE MEASUREMENTS; ABSORPTION-COEFFICIENT AB It is suggested that an economical airborne lidar having a single laser can retrieve the three principal inherent optical properties of the ocean. Only three time-resolved backscattering receiver channels are required: (i) elastic (on-wavelength), (ii) inelastic (water Raman), and (iii) inelastic [chromophoric dissolved organic matter (CDOM) fluorescence channel to remove the CDOM fluorescence interference from the Raman channel]. C1 NASA, Goddard Space Flight Ctr, Wallops Isl Facil, Wallops Isl, VA 23337 USA. RP Hoge, FE (reprint author), NASA, Goddard Space Flight Ctr, Wallops Isl Facil, Wallops Isl, VA 23337 USA. EM frank.hoge@nasa.gov NR 18 TC 4 Z9 4 U1 0 U2 1 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1559-128X EI 2155-3165 J9 APPL OPTICS JI Appl. Optics PD DEC 1 PY 2005 VL 44 IS 34 BP 7483 EP 7486 DI 10.1364/AO.44.007483 PG 4 WC Optics SC Optics GA 989LH UT WOS:000233674700031 PM 16353822 ER PT J AU Beaty, DW Clifford, SM Borg, LE Catling, DC Craddock, RA Des Marais, DJ Farmer, JD Frey, HV Haberle, RM McKay, CP Newsom, HE Parker, TJ Segura, T Tanaka, KL AF Beaty, DW Clifford, SM Borg, LE Catling, DC Craddock, RA Des Marais, DJ Farmer, JD Frey, HV Haberle, RM McKay, CP Newsom, HE Parker, TJ Segura, T Tanaka, KL TI Key science questions from the second conference on early Mars: Geologic, hydrologic, and climatic evolution and the implications for life SO ASTROBIOLOGY LA English DT Review DE early Mars; noachian; volatiles; habitability; water; geologic evolution ID MARTIAN IMPACT CRATERS; CARBON-DIOXIDE CLOUDS; HYDROTHERMAL ALTERATION; EARLY DIFFERENTIATION; TERRESTRIAL PLANETS; METEORITE ALH84001; FLUVIAL PROCESSES; GREENHOUSE GASES; ANCIENT OCEANS; LATE MAGMATISM AB In October 2004, more than 130 terrestrial and planetary scientists met in Jackson Hole, WY, to discuss early Mars. The first billion years of martian geologic history is of particular interest because it is a period during which the planet was most active, after which a less dynamic period ensued that extends to the present day. The early activity left a fascinating geological record, which we are only beginning to unravel through direct observation and modeling. In considering this time period, questions outnumber answers, and one of the purposes of the meeting was to gather some of the best experts in the field to consider the current state of knowledge, ascertain which questions remain to be addressed, and identify the most promising approaches to addressing those questions. The purpose of this report is to document that discussion. Throughout the planet's first billion years, planetary-scale processes-including differentiation, hydrodynamic escape, volcanism, large impacts, erosion, and sedimentation-rapidly modified the atmosphere and crust. How did these processes operate, and what were their rates and interdependencies? The early environment was also characterized by both abundant liquid water and plentiful sources of energy, two of the most important conditions considered necessary for the origin of life. Where and when did the most habitable environments occur? Did life actually occupy them, and if so, has life persisted on Mars to the present? Our understanding of early Mars is critical to understanding how the planet we see today came to be. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. CALTECH, Mars Program Off, Pasadena, CA 91109 USA. Ames Res Ctr, Moffett Field, CA USA. Northrop Grumman, Redondo Beach, CA USA. Lunar & Planetary Inst, Houston, TX 77058 USA. Univ New Mexico, Albuquerque, NM 87131 USA. Univ Bristol, Dept Earth Sci, Bristol, Avon, England. Univ Washington, Seattle, WA 98195 USA. Smithsonian Inst, Washington, DC 20560 USA. Arizona State Univ, Tucson, AZ USA. Goddard Space Flight Ctr, Greenbelt, MD USA. US Geol Survey, Reston, VA 22092 USA. RP Beaty, DW (reprint author), CALTECH, Jet Prop Lab, Mail Stop 301-345,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM David.Beaty@jpl.nasa.gov RI Catling, David/D-2082-2009; OI Catling, David/0000-0001-5646-120X NR 159 TC 12 Z9 14 U1 1 U2 14 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD DEC PY 2005 VL 5 IS 6 BP 663 EP 689 DI 10.1089/ast.2005.5.663 PG 27 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 998WY UT WOS:000234351800001 PM 16379524 ER PT J AU Szewczyk, NJ Mancinelli, RL McLamb, W Reed, D Blumberg, BS Conley, CA AF Szewczyk, NJ Mancinelli, RL McLamb, W Reed, D Blumberg, BS Conley, CA TI Caenorhabditis elegans survives atmospheric breakup of STS-107, space shuttle Columbia SO ASTROBIOLOGY LA English DT Article DE Caenorhabditis elegans; nematode; spaceflight research; atmospheric reentry; space shuttle Columbia ID CHEMICALLY-DEFINED MEDIUM; NEMATODES; EARTH; RADIATION; BIOLOGY; SYSTEM; IML-1; MARS AB The nematode Caenorhabditis elegans, a popular organism for biological studies, is being developed as a model system for space biology. The chemically defined liquid medium, C. elegans Maintenance Medium (CeMM), allows axenic cultivation and automation of experiments that are critical for spaceflight research. To validate CeMM for use during spaceflight, we grew animals using CeMM and standard laboratory conditions onboard STS-107, space shuttle Columbia. Tragically, the Columbia was destroyed while reentering the Earth's atmosphere. During the massive recovery effort, hardware that contained our experiment was found. Live animals were observed in four of the five recovered canisters, which had survived on both types of media. These data demonstrate that CeMM is capable of supporting C. elegans during spaceflight. They also demonstrate that animals can survive a relatively unprotected reentry into the Earth's atmosphere, which has implications with regard to the packaging of living material during space flight, planetary protection, and the interplanetary transfer of life. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Bionet Corp, Kennedy Space Ctr, FL USA. Fox Chase Canc Ctr, Philadelphia, PA 19111 USA. RP NASA, Ames Res Ctr, M-S 239-11, Moffett Field, CA 94035 USA. EM cassie.conley@nasa.gov RI Mancinelli, Rocco/L-8971-2016; OI Szewczyk, Nathaniel/0000-0003-4425-9746 NR 45 TC 19 Z9 20 U1 4 U2 19 PU MARY ANN LIEBERT, INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 EI 1557-8070 J9 ASTROBIOLOGY JI Astrobiology PD DEC PY 2005 VL 5 IS 6 BP 690 EP 705 DI 10.1089/ast.2005.5.690 PG 16 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 998WY UT WOS:000234351800002 PM 16379525 ER PT J AU Segura, A Kasting, JF Meadows, V Cohen, M Scalo, J Crisp, D Butler, RAH Tinetti, G AF Segura, A Kasting, JF Meadows, V Cohen, M Scalo, J Crisp, D Butler, RAH Tinetti, G TI Biosignatures from earth-like planets around M dwarfs SO ASTROBIOLOGY LA English DT Article DE habitable planets; M dwarfs; biosignatures; biomarkers; terrestrial planet finder ID PHOTOABSORPTION CROSS-SECTIONS; LOW-MASS STARS; EXTREME-ULTRAVIOLET; TERRESTRIAL PLANETS; FLARE STARS; RED DWARFS; LY-ALPHA; ATMOSPHERES; MODEL; HABITABILITY AB Coupled one-dimensional photochemical-climate calculations have been performed for hypothetical Earth-like planets around M dwarfs. Visible/near-infrared and thermal-infrared synthetic spectra of these planets were generated to determine which biosignature gases might be observed by a future, space-based telescope. Our star sample included two observed active M dwarfs-AD Leo and GJ 643-and three quiescent model stars. The spectral distribution of these stars in the ultraviolet generates a different photochemistry on these planets. As a result, the biogenic gases CH4, N2O, and CH3Cl have substantially longer lifetimes and higher mixing ratios than on Earth, making them potentially observable by space-based telescopes. On the active M-star planets, an ozone layer similar to Earth's was developed that resulted in a spectroscopic signature comparable to the terrestrial one. The simultaneous detection of O-2 (or O-3) and a reduced gas in a planet's atmosphere has been suggested as strong evidence for life. Planets circling M stars may be good locations to search for such evidence. C1 CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA. Penn State Univ, Dept Geosci, University Pk, PA 16802 USA. CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91125 USA. CALTECH, Natl Res Council, Pasadena, CA 91125 USA. Univ Calif Berkeley, Radio Astron Lab, Berkeley, CA 94720 USA. Univ Texas, Dept Astron, Austin, TX 78712 USA. RP Segura, A (reprint author), CALTECH, Ctr Infrared Proc & Anal, M-C 220-6, Pasadena, CA 91125 USA. EM antigona@ipac.caltech.edu OI Tinetti, Giovanna/0000-0001-6058-6654 NR 100 TC 175 Z9 177 U1 6 U2 30 PU MARY ANN LIEBERT INC PI NEW ROCHELLE PA 140 HUGUENOT STREET, 3RD FL, NEW ROCHELLE, NY 10801 USA SN 1531-1074 J9 ASTROBIOLOGY JI Astrobiology PD DEC PY 2005 VL 5 IS 6 BP 706 EP 725 DI 10.1089/ast.2005.5.706 PG 20 WC Astronomy & Astrophysics; Biology; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Life Sciences & Biomedicine - Other Topics; Geology GA 998WY UT WOS:000234351800003 PM 16379526 ER PT J AU Krist, JE Stapelfeldt, KR Golimowski, DA Ardila, DR Clampin, M Martel, AR Ford, HC Illingworth, GD Hartig, GF AF Krist, JE Stapelfeldt, KR Golimowski, DA Ardila, DR Clampin, M Martel, AR Ford, HC Illingworth, GD Hartig, GF TI Hubble Space Telescope ACS images of the GG Tauri circumbinary disk SO ASTRONOMICAL JOURNAL LA English DT Article DE binaries : general; circumstellar matter; stars : individual (GG Tauri); stars : pre-main-sequence ID BINARY STARS; RING; MODELS; SYSTEM; MASS AB Hubble Space Telescope Advanced Camera for Surveys images of the young binary GG Tauri and its circumbinary disk in V and I bandpasses were obtained in 2002 and are the most detailed of this system to date. They confirm features previously seen in the disk including a "gap'' apparently caused by shadowing from circumstellar material, an asymmetrical distribution of light about the line of sight on the near edge of the disk, enhanced brightness along the near edge of the disk due to forward scattering, and a compact reflection nebula near the secondary star. New features are seen in the ACS images: two short filaments along the disk, localized but strong variations in the disk intensity ("gaplets''), and a "spur'' or filament extending from the reflection nebulosity near the secondary. The back side of the disk is detected in the V band for the first time. The disk appears redder than the combined light from the stars, which may be explained by a varied distribution of grain sizes. The brightness asymmetries along the disk suggest that it is asymmetrically illuminated by the stars due to extinction by nonuniform circumstellar material or that the illuminated surface of the disk is warped by tidal effects (or perhaps both). Localized, time-dependent brightness variations in the disk are also seen. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Space Telescope Sci Inst, Baltimore, MD 21218 USA. Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Calif Santa Cruz, Univ Calif Observ, Lick Observ, Santa Cruz, CA 95064 USA. RP Krist, JE (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 NR 23 TC 36 Z9 36 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 DEC PY 2005 VL 130 IS 6 BP 2778 EP 2787 DI 10.1086/497069 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 988FH UT WOS:000233576800026 ER PT J AU Muterspaugh, MW Lane, BF Konacki, M Burke, BF Colavita, MM Kulkarni, SR Shao, M AF Muterspaugh, MW Lane, BF Konacki, M Burke, BF Colavita, MM Kulkarni, SR Shao, M TI Phases high-precision differential astrometry of delta Equulei SO ASTRONOMICAL JOURNAL LA English DT Review DE astrometry; binaries : close; binaries : visual; stars : distances; stars : individual (delta Equulei); techniques : interferometric ID ICCD SPECKLE OBSERVATIONS; DOUBLE STAR MEASURES; VISUAL DOUBLE STARS; PEAK 4-M TELESCOPE; PALOMAR TESTBED INTERFEROMETER; LINED SPECTROSCOPIC BINARIES; KITT-PEAK; MOUNT-HAMILTON; MICROMETER MEASURES; SOLAR NEIGHBORHOOD AB Delta Equulei is among the most well-studied nearby binary star systems. Results of its observation have been applied to a wide range of fundamental studies of binary systems and stellar astrophysics. It is widely used to calibrate and constrain theoretical models of the physics of stars. We report 27 high-precision differential astrometry measurements of delta Equ from the Palomar High-precision Astrometric Search for Exoplanet Systems (PHASES). The median size of the minor axes of the uncertainty ellipses for these measurements is 26 mu as. These data are combined with previously published radial velocity data and other previously published differential astrometry measurements using other techniques to produce a combined model for the system orbit. The distance to the system is determined to within one twentieth of a parsec, and the component masses are determined at the level of a percent. The constraints on masses and distance are limited by the precisions of the radial velocity data; we outline plans to improve this deficiency and discuss the outlook for further study of this binary. C1 MIT, Dept Phys, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA. CALTECH, Dept Geol & Planetary Sci, Pasadena, CA 91125 USA. Polish Acad Sci, Nicolaus Copernicus Astron Ctr, PL-87100 Torun, Poland. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. RP Muterspaugh, MW (reprint author), MIT, Dept Phys, Kavli Inst Astrophys & Space Res, 70 Vassar St, Cambridge, MA 02139 USA. EM matthew1@mit.edu; blane@mit.edu; maciej@gps.caltech.edu RI Konacki, Maciej/A-1220-2007 NR 105 TC 22 Z9 22 U1 0 U2 2 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 DEC PY 2005 VL 130 IS 6 BP 2866 EP 2875 DI 10.1086/497035 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 988FH UT WOS:000233576800033 ER PT J AU Landi, E Bhatia, AK AF Landi, E Bhatia, AK TI Atomic data and spectral line intensities for Ca XIII SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE atomic data; Sun : corona; Sun : UV radiation ID ELECTRON-IMPACT EXCITATION; OXYGEN ISOELECTRONIC SEQUENCE; OSCILLATOR-STRENGTHS; COLLISION STRENGTHS; SOLAR-FLARE; RATE COEFFICIENTS; CROSS-SECTIONS; IRON PROJECT; NI-XXI; IONS AB Electron impact collision strengths, energy levels, oscillator strengths and spontaneous radiative decay rates are calculated for Ca XIII. 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 (40, 80, 120, 160 and 200 Ry) in the distorted wave approximation. Excitation rate coefficients are calculated as a function of electron temperature by assuming a Maxwellian electron velocity distribution. 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(K) = 6.5, corresponding to maximum abundance of Ca XIII. Relative and absolute spectral line intensities are calculated, and their diagnostic relevance is discussed. This dataset will be made available in the next version of the CHIANTI database. C1 Artep Inc, Ellicott City, MD 21042 USA. USN, Res Lab, Washington, DC 20375 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Landi, E (reprint author), Artep Inc, Ellicott City, MD 21042 USA. EM landi@poppeo.nrl.navy.mil RI Landi, Enrico/H-4493-2011 NR 39 TC 2 Z9 2 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 DEC PY 2005 VL 444 IS 1 BP 305 EP 317 DI 10.1051/0004-6361:20053290 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 986LO UT WOS:000233451300031 ER PT J AU Ponthieu, N Macias-Perez, JF Tristram, M Ade, P Amblard, A Ansari, R Aumont, J Aubourg, E Benoit, A Bernard, JP Blanchard, A Bock, JJ Bouchet, FR Bourrachot, A Camus, P Cardoso, JF Couchot, F de Bernardis, P Delabrouille, J Desert, FX Douspis, M Dumoulin, L Filliatre, P Fosalba, P Giard, M Giraud-Heraud, Y Gispert, R Grain, J Guglielmi, L Hamilton, JC Hanany, S Henrot-Versille, S Kaplan, J Lagache, G Lange, AE Madet, K Maffei, B Masi, S Mayet, F Nati, F Patanchon, G Perdereau, O Plaszczynski, S Piat, M Prunet, S Puget, JL Renault, C Rosset, C Santos, D Vibert, D Yvon, D AF Ponthieu, N Macias-Perez, JF Tristram, M Ade, P Amblard, A Ansari, R Aumont, J Aubourg, E Benoit, A Bernard, JP Blanchard, A Bock, JJ Bouchet, FR Bourrachot, A Camus, P Cardoso, JF Couchot, F de Bernardis, P Delabrouille, J Desert, FX Douspis, M Dumoulin, L Filliatre, P Fosalba, P Giard, M Giraud-Heraud, Y Gispert, R Grain, J Guglielmi, L Hamilton, JC Hanany, S Henrot-Versille, S Kaplan, J Lagache, G Lange, AE Madet, K Maffei, B Masi, S Mayet, F Nati, F Patanchon, G Perdereau, O Plaszczynski, S Piat, M Prunet, S Puget, JL Renault, C Rosset, C Santos, D Vibert, D Yvon, D TI Temperature and polarization angular power spectra of Galactic dust radiation at 353 GHz as measured by Archeops SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmology : cosmic microwave background; cosmology : observations; polarization; ISM : dust, extinction ID MICROWAVE-ANISOTROPY-PROBE; WMAP OBSERVATIONS; BACKGROUND POLARIZATION; COSMOLOGICAL PARAMETERS; EMISSION; COBE; CONSTRAINTS; MAPS AB We present the first measurement of temperature and polarization angular power spectra of the diffuse emission of Galactic dust at 353 GHz as seen by Archeops on 20% of the sky. The temperature angular power spectrum is compatible with that provided by the extrapolation to 353 GHz of IRAS and DIRBE maps using Finkbeiner et al. (1999, ApJ, 524, 867) model number 8. For Galactic latitudes vertical bar b vertical bar >= 5 deg we report a 4 sigma detection of large scale (3 <= l <= 8) temperature-polarization cross-correlation (l + 1) C-l(TE)/2 pi = 76 +/- 21 mu K-RJ(2) and set upper limits to the E and B mode polarization at 11 mu K-RJ(2). For Galactic latitudes vertical bar b vertical bar >= 10 deg, on the same angular scales, we report a 2 sigma detection of temperature-polarization cross-correlation (l + 1)C-l(TE)/2 pi = 24 +/- 13 mu K-RJ(2). These results are then extrapolated to 100 GHz to estimate the contamination in CMB measurements by polarized diffuse Galactic dust emission. The TE signal is then 1.7 +/- 0.5 and 0.5 +/- 0.3 mu K-CMB(2) for vertical bar b vertical bar >= 5 and 10 deg respectively. The upper limit on E and B mode polarization becomes 0.2 mu K-CMB(2) (2 sigma). If the physical properties of dust radiation on the fraction of the sky observed by Archeops are representative of the whole sky, and if the actual level of E and B mode polarization is close to this upper limit, then dust polarized radiation will be a major foreground for determining the polarization power spectra of the CMB at high frequencies above 100 GHz. C1 Univ Paris 11, Inst Astrophys Spatiale, F-91405 Orsay, France. Lab Phys Subatom & Cosmol, F-38026 Grenoble, France. Cardiff Univ, Dept Phys, Cardiff CF24 3YB, Wales. Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA. Lab Accelerateur Lineaire, F-91898 Orsay, France. CEA CE Saclay, DAPNIA, Serv Phys Particules, F-91191 Gif Sur Yvette, France. Univ Paris 07, Federat Rech APC, Paris, France. Ctr Rech Tres Basses Temp, F-38042 Grenoble, France. Ctr Etud Spatiale Rayonnements, F-31028 Toulouse, France. UPS, OMP, CNRS, Lab Astrophys Tarbes Toulouse,UMR 5572, F-31400 Toulouse, France. CALTECH, Pasadena, CA 91125 USA. Jet Prop Lab, Pasadena, CA 91109 USA. Inst Astrophys, F-75014 Paris, France. Coll France, F-75231 Paris, France. Univ Roma La Sapienza, Dipartimento Fis, Grp Cosmol Sperimentale, I-00185 Rome, Italy. Obs Grenoble, Astrophys Lab, F-38041 Grenoble, France. CSNSM, IN2P3, F-91405 Orsay, France. CEA CE Saclay, DAPNIA, Serv Astrophys, F-91191 Gif Sur Yvette, France. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. Univ Paris 06, LPHNE, F-75252 Paris, France. Univ Paris 07, LPHNE, F-75252 Paris, France. Univ Minnesota, Sch Phys & Astron, Minneapolis, MN 55455 USA. Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. RP Ponthieu, N (reprint author), Univ Paris 11, Inst Astrophys Spatiale, Bat 121, F-91405 Orsay, France. EM reprints@archeops.org; macias@in2p3.fr RI Bouchet, Francois/B-5202-2014; amblard, alexandre/L-7694-2014; Yvon, Dominique/D-2280-2015; Fosalba Vela, Pablo/I-5515-2016; Nati, Federico/I-4469-2016; OI amblard, alexandre/0000-0002-2212-5395; Nati, Federico/0000-0002-8307-5088; Masi, Silvia/0000-0001-5105-1439; de Bernardis, Paolo/0000-0001-6547-6446; Bouchet, Francois/0000-0002-8051-2924 NR 44 TC 53 Z9 54 U1 0 U2 0 PU EDP SCIENCES S A PI LES ULIS CEDEX A PA 17, AVE DU HOGGAR, PA COURTABOEUF, BP 112, F-91944 LES ULIS CEDEX A, FRANCE SN 0004-6361 J9 ASTRON ASTROPHYS JI Astron. Astrophys. PD DEC PY 2005 VL 444 IS 1 BP 327 EP 336 DI 10.1051/0004-6361:20052715 PG 10 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 986LO UT WOS:000233451300033 ER PT J AU Paizis, A Nowak, MA Wilms, J Courvoisier, TJL Ebisawa, K Rodriguez, J Ubertini, P AF Paizis, A Nowak, MA Wilms, J Courvoisier, TJL Ebisawa, K Rodriguez, J Ubertini, P TI Chandra and RXTE spectroscopy of the accreting msec pulsar IGR J00291+5934 SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE pulsars : individual : IGR J00291+5934 ID X-RAY SPECTROSCOPY; MILLISECOND PULSAR; XMM-NEWTON; DISCOVERY; OUTBURST; SPECTRA AB We report on an observation of the recently discovered accreting millisecond X-ray pulsar IGR J00291+5934 performed with the RXTE-Proportional Counter Array ( PCA) and Chandra-High Energy Transmission Grating Spectrometer (HETGS). The RXTE data are from a two-week follow-up of the source, while the Chandra observation took place around the end of the follow-up, about 12 days after the discovery of the source, when the source flux had decreased already by a factor of ten. The analysis of the Chandra data allowed us to extract the most precise X-ray position of IGR J00291+5934, RA = 00(h) 29(m) 03.08(s), and Dec = +59 degrees 34' 19.2" (0.6" error), compatible with the optical and radio ones. We find that the spectra of IGR J00291+5934 can be described by a combination of a thermal component and a power-law. Along the outburst detected by PCA, the power-law photon index showed no particular trend, while the thermal component (similar to 1 keV, interpreted as a hot spot on the neutron star surface) became weaker until non-detection. In the simultaneous observation of the weak Chandra/RXTE spectrum, there was no longer any indication of the similar to 1 keV thermal component, while we detected a colder thermal component (similar to 0.4 keV) that we interpret as the emission from the cold disc. A hint of a 6.4 keV iron line was detected, together with an excess around 6.8 keV and absorption feature around 7.1 keV. The last two features have never been detected in the spectra of accretion-driven millisecond pulsars before and, if confirmed, would suggest the presence of an expanding hot corona with high outflow velocities. C1 INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland. INAF, IASF, Sez Milan, I-20133 Milan, Italy. MIT, Ctr Space Res, Cambridge, MA 02139 USA. Univ Warwick, Dept Phys, Coventry CV4 7AL, W Midlands, England. Observ Geneva, CH-1290 Sauverny, Switzerland. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. CEA Saclay, DSM,AIM, DAPNIA,UMR 7158, SAp,CNRS, F-91191 Gif Sur Yvette, France. INAF, IASF, Sez Roma, I-00133 Rome, Italy. RP Paizis, A (reprint author), INTEGRAL Sci Data Ctr, Chemin Ecogia 16, CH-1290 Versoix, Switzerland. EM Ada.Paizis@obs.unige.ch RI Wilms, Joern/C-8116-2013; OI Wilms, Joern/0000-0003-2065-5410; Rodriguez, Jerome/0000-0002-4151-4468; Paizis, Adamantia/0000-0001-5067-0377 NR 35 TC 12 Z9 12 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 DEC PY 2005 VL 444 IS 2 BP 357 EP 363 DI 10.1051/0004-6361:20053419 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 986PJ UT WOS:000233461900011 ER PT J AU Revnivtsev, M Gilfanov, M Jahoda, K Sunyaev, R AF Revnivtsev, M Gilfanov, M Jahoda, K Sunyaev, R TI Intensity of the cosmic X-ray backgound from HEAO1/A2 experiment SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE cosmology : observations; X-rays : general ID BACKGROUND SPECTRUM; XMM-NEWTON; CATALOG; HEAO-1 AB We reanalyze data of HEAO1/A2-the Cosmic X-ray Experiment-in order to repeat the measurements of the cosmic X-ray background (CXB) intensity and accurately compare this value with other measurements of the CXB. We used the data of MED, HED1, and HED3 detectors in scan mode, which allowed us to measure effective solid angles and effective areas of detectors self consistently, in the same mode as the CXB intensity was measured. We found that the average value of the CXB intensity is 1.96 +/- 0.10 x 10(-11) erg s(-1) cm(-2) deg(-2) in the energy band 2-10 keV, or 9.7 +/- 0.5 phot s(-1) cm(-2) at 1 keV assuming the power law spectral shape with photon index Gamma = 1.4 in this energy band. We compare the obtained measurements with those obtained by different instruments over the past few decades. C1 Max Planck Inst Astrophys, D-85740 Garching, Germany. Russian Acad Sci, Inst Space Res, Moscow 117810, Russia. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. RP Revnivtsev, M (reprint author), Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85740 Garching, Germany. EM mikej@mpa-garching.mpg.de RI Jahoda, Keith/D-5616-2012 NR 23 TC 33 Z9 33 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 DEC PY 2005 VL 444 IS 2 BP 381 EP 385 DI 10.1051/0004-6361:20042526 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 986PJ UT WOS:000233461900013 ER PT J AU Soldi, S Beckmann, V Bassani, L Courvoisier, TJL Landi, R Malizia, A Dean, AJ De Rosa, A Fabian, AC Walter, R AF Soldi, S Beckmann, V Bassani, L Courvoisier, TJL Landi, R Malizia, A Dean, AJ De Rosa, A Fabian, AC Walter, R TI INTEGRAL observations of six AGN in the galactic plane SO ASTRONOMY & ASTROPHYSICS LA English DT Article DE galaxies : active; galaxies : Seyfert; gamma rays : observations; X-rays : galaxies ID RAY-TIMING-EXPLORER; SEYFERT 2 GALAXIES; BEPPOSAX OBSERVATIONS; CENTAURUS-A; XMM-NEWTON; INSTRUMENT DESCRIPTION; AVERAGE SPECTRA; ON-BOARD; RXTE; SPECTROMETER AB We present results on approximately one year of INTEGRAL observations of six AGN detected during the regular scans of the Galactic Plane. The sample is composed by five Seyfert 2 objects (MCG-05-23-16, NGC 4945, the Circinus galaxy, NGC 6300, ESO 103-G35) and the radio galaxy Centaurus A. The continuum emission of each of these sources is well represented by a highly absorbed (N-H > 10(22) cm(-2)) power law, with average spectral index Gamma = 1.9 +/- 0.3. A high energy exponential cut-off at E-c similar to 50 keV is required to fit the spectrum of the Circinus galaxy, whereas a lower limit of 130 keV has been found for NGC 4945 and no cut-off has been detected for NGC 6300 in the energy range covered by these INTEGRAL data. The flux of Centaurus A was found to vary by a factor of similar to 2 in 10 months, showing a spectral change between the high and low state, which can be modelled equally well by a change in the absorption (N-H from 17 to 33 x 10(22) cm(-2)) or by the presence of a cut-off at greater than or similar to 120 keV in the low state spectrum. A comparison with recently reprocessed BeppoSAX/PDS data shows a general agreement with INTEGRAL results. The high energy cut-off in the hard X-ray spectra appears to be a common but not universal characteristic of Seyfert 2 and to span a wide range of energies. C1 INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland. Observ Geneva, CH-1290 Sauverny, Switzerland. NASA, Goddard Space Flight Ctr, Explorat Universe Div, Greenbelt, MD 20771 USA. Univ Maryland Baltimore Cty, Dept Phys, Joint Ctr Astrophys, Baltimore, MD 21250 USA. CNR, IASF, INAF, I-40129 Bologna, Italy. Univ Bologna, Dipartimento Fis, I-40127 Bologna, Italy. Univ Southampton, Sch Phys & Astron, Southampton SO17 1BJ, Hants, England. CNR, INAF, IASF, I-00133 Rome, Italy. Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England. RP Soldi, S (reprint author), INTEGRAL Sci Data Ctr, Chemin Ecogia 16, CH-1290 Versoix, Switzerland. EM Simona.Soldi@obs.unige.ch OI Malizia, Angela/0000-0002-6558-1163; Bassani, Loredana/0000-0003-4858-6963; De Rosa, Alessandra/0000-0001-5668-6863 NR 64 TC 26 Z9 26 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 DEC PY 2005 VL 444 IS 2 BP 431 EP 441 DI 10.1051/0004-6361:20053875 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 986PJ UT WOS:000233461900018 ER PT J AU Maier, C Lilly, SJ Carollo, CM Stockton, A Brodwin, M AF Maier, C Lilly, SJ Carollo, CM Stockton, A Brodwin, M TI Near-infrared spectroscopy of 0.4 < z < 1.0 CFRS galaxies: Oxygen abundances, SFRs, and dust SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : abundances; galaxies : evolution; galaxies : high-redshift ID STAR-FORMING GALAXIES; LUMINOSITY-METALLICITY RELATION; FIELD GALAXIES; INTERMEDIATE REDSHIFTS; COMPACT GALAXIES; METAL ABUNDANCES; KISS GALAXIES; EVOLUTION; SPECTRA; REGIONS AB Using new J-band VLT ISAAC and Keck NIRSPEC spectroscopy, we have measured H alpha and [N (II)] lambda 6584 line fluxes for 0.47 < z < 0.92 CFRS galaxies that have [O (II)] lambda 3727, H beta, and [O (III)] lambda 5007 line fluxes available from optical spectroscopy to investigate how the properties of the star-forming gas in galaxies evolve with redshift. We derive the extinction and oxygen abundances for the sample using a method based on a set of ionization parameter and oxygen abundance diagnostics, simultaneously fitting the [O (II)], H beta, [O (III)], H beta, and [N (II)] line fluxes. The individual reddening measurements allow us to accurately correct the H alpha-based star formation rate (SFR) estimates for extinction. Our most salient conclusions are as follows: (1) in all 30 CFRS galaxies, the source of the gas ionization is not due to AGN activity; ( 2) we find a range of 0 < AV < 3, suggesting that it is important to determine the extinction for every single galaxy in order to reliably measure SFRs and oxygen abundances in high-redshift galaxies; (3) high values of [N (II)] lambda 6584/H alpha > 0.1 for most (but not all) of the CFRS galaxies indicate that they lie on the high-metallicity branch of the R-23 calibration; (4) about one-third of the 0.47 < z < 0.92 CFRS galaxies in our sample have lower metallicities than local galaxies with similar luminosities and star formation rates; (5) comparison with a chemical evolution model indicates that these low-metallicity galaxies are unlikely to be the progenitors of metal-poor dwarf galaxies at z similar to 0. C1 ETH Honggerberg, ETH, Dept Phys, CH-8093 Zurich, Switzerland. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. CALTECH, Jet Propuls Lab, Pasadena, CA 91109 USA. RP ETH Honggerberg, ETH, Dept Phys, CH-8093 Zurich, Switzerland. EM chmaier@phys.ethz.ch OI Maier, Christian/0000-0001-6405-2182 NR 32 TC 51 Z9 52 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2005 VL 634 IS 2 BP 849 EP 860 DI 10.1086/497091 PN 1 PG 12 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 988FO UT WOS:000233577700011 ER PT J AU Beckmann, V Shrader, CR Gehrels, N Soldi, S Lubinski, P Zdziarski, AA Petrucci, PO Malzac, J AF Beckmann, V Shrader, CR Gehrels, N Soldi, S Lubinski, P Zdziarski, AA Petrucci, PO Malzac, J TI The high-energy spectrum of NGC 4151 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : active; galaxies : individual (NGC 4151); galaxies : Seyfert; gamma rays : observations; X-rays : galaxies ID ACTIVE GALACTIC NUCLEI; SEYFERT 1 GALAXIES; X-RAY-SPECTRA; NGC 4151; GAMMA-RAY; COMPTONIZATION MODELS; VARIABILITY; PERFORMANCE; SPI; REFLECTION AB We present the first INTEGRAL observations of the type 1.5 Seyfert galaxy NGC 4151. Combining several INTEGRAL observations performed during 2003, totaling similar to 400 ks of exposure time, allows us to study the spectrum in the 2-300 keV range. The measurements presented here reveal an overall spectrum from X-rays up to soft gamma-rays that can be described by an absorbed (NH 6: 9; 1022 cm(-2)) model based on a Compton continuum from a hot electron population (kTe = 94 keV) from an optically thick (tau = 1.3) corona, reflected on cold material (R = 0.7), consistent with earlier claims. The time-resolved analysis shows little variation of the spectral parameters over the duration of the INTEGRAL observations. The comparison with CGRO OSSE data shows that the same spectral model can be applied over a time span of 15 yr, with flux variations of the order of a factor of 2 and changes in the underlying continuum reflected by the temperature of the electron population (kT(e) = 50-100 keV). When modeled with an exponential cutoff power law plus Compton reflection, this results in photon indices ranging from T = 1.5 to 1.9 and a cutoff energy in the range 100-500 keV. C1 NASA, Goddard Space Flight Ctr, Explorat Universe Div, Greenbelt, MD 20771 USA. INTEGRAL Sci Data Ctr, CH-1290 Versoix, Switzerland. Nicholas Copernicus Astron Ctr, PL-00716 Warsaw, Poland. Lab Astrophys Grenoble, F-38041 Grenoble, France. Ctr Etud Spatiale Rayonnements, F-31028 Toulouse, France. Univ Maryland Baltimore Cty, Joint Ctr Astrophys, Dept Phys, Baltimore, MD 21250 USA. Univ Space Res Assoc, Columbia, MD 21044 USA. Observ Geneva, CH-1290 Sauverny, Switzerland. RP NASA, Goddard Space Flight Ctr, Explorat Universe Div, Code 661, Greenbelt, MD 20771 USA. EM beckmann@milkyway.gsfc.nasa.gov RI Gehrels, Neil/D-2971-2012 NR 53 TC 22 Z9 22 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2005 VL 634 IS 2 BP 939 EP 946 DI 10.1086/497120 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 988FO UT WOS:000233577700018 ER PT J AU Mukai, K Still, M Corbet, RHD Kuntz, KD Barnard, R AF Mukai, K Still, M Corbet, RHD Kuntz, KD Barnard, R TI The X-ray properties of M101 ULX-1=CXOKM101 J140332.74+542102 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : individual (M101); X rays : binaries; X rays : individual (M101 ULX-1) ID MASS BLACK-HOLE; XMM-NEWTON; CHANDRA; ACCRETION; EMISSION; BINARIES; NOVAE AB We report our analysis of X-ray data on M101 ULX-1, concentrating on high-state Chandra and XMM-Newton observations. We find that the high state of M101 ULX-1 may have a preferred recurrence timescale. If so, the underlying clock may have periods around 160 or 190 days, or possibly around 45 days. Its short-term variations resemble those of X-ray binaries at high accretion rates. If this analogy is correct, we infer that the accretor is a 20 40 M-circle dot object. This is consistent with our spectral analysis of the high-state spectra of M101 ULX-1, from which we find no evidence for an extreme (> 10(40) ergs s(-1)) luminosity. We present our interpretation in the framework of a high-mass X-ray binary system consisting of a B supergiant mass donor and a large stellar-mass black hole. C1 NASA, Goddard Space Flight Ctr, Explorat Universe Div, Greenbelt, MD 20771 USA. Johns Hopkins Univ, Henry A Rowland Dept Phys & Astron, Baltimore, MD 21218 USA. Open Univ, Dept Phys & Astron, Milton Keynes MK7 6BT, Bucks, England. RP Mukai, K (reprint author), NASA, Goddard Space Flight Ctr, Explorat Universe Div, Code 662, Greenbelt, MD 20771 USA. EM mukai@milkyway.gsfc.nasa.gov NR 24 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 0004-637X J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2005 VL 634 IS 2 BP 1085 EP 1092 DI 10.1086/497110 PN 1 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 988FO UT WOS:000233577700029 ER PT J AU Van der Horst, AJ Rol, E Wijers, RAMJ Strom, R Kaper, L Kouveliotou, C AF Van der Horst, AJ Rol, E Wijers, RAMJ Strom, R Kaper, L Kouveliotou, C TI The radio afterglow of GRB 030329 centimeter wavelengths: Evidence for a structured jet or nonrelativistic expansion SO ASTROPHYSICAL JOURNAL LA English DT Article DE gamma rays : bursts; radiation mechanisms : nonthermal; radio continuum : general ID GAMMA-RAY BURST; 28 FEBRUARY 1997; X-RAY; REFRESHED SHOCKS; VIEWING ANGLE; LIGHT CURVES; ERROR BOX; COLLAPSARS; SUPERNOVA; CALORIMETRY AB We present our centimeter wavelength(1.4, 2.3, and 4.8 GHz) light curves of the afterglow of GRB 030329, which were obtained with the Westerbork Synthesis Radio Telescope. Modeling the data according to a collimated afterglow results in a jet-break time of 10 days. This is in accordance with earlier results obtained at higher radio frequencies. However, with respect to the afterglow model, some additional flux at the lower frequencies is present when these light curves reach their maximum after 40-80 days. We show that this additional flux can be modeled with two or more components with progressively later jet breaks. From these results we infer that the jet is in fact a structured or a layered jet, where the ejecta with lower Lorentz factors produce additional flux that becomes visible at late times in the lowest frequency bands. We show that a transition to nonrelativistic expansion of the fireball at late times can also account for the observed flux excess, except for the lowest frequency ( 1.4 GHz) data. C1 Univ Amsterdam, Inst Astron, NL-1098 SJ Amsterdam, Netherlands. Univ Leicester, Dept Phys & Astron, Leicester LE2 7RH, Leics, England. ASTRON, NL-7990 AA Dwingeloo, Netherlands. NASA, Marshall Space Flight Ctr, USRA, NSSTC, Huntsville, AL 35805 USA. RP Univ Amsterdam, Inst Astron, Kruislaan 403, NL-1098 SJ Amsterdam, Netherlands. NR 31 TC 26 Z9 26 U1 0 U2 2 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-637X EI 1538-4357 J9 ASTROPHYS J JI Astrophys. J. PD DEC 1 PY 2005 VL 634 IS 2 BP 1166 EP 1172 DI 10.1086/497021 PN 1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 988FO UT WOS:000233577700037 ER PT J AU Linares, M van der Klis, M Altamirano, D Markwardt, CB AF Linares, M van der Klis, M Altamirano, D Markwardt, CB TI Discovery of kilohertz quasi-periodic oscillations and shifted frequency correlations in the accreting millisecond pulsar XTE J1807-294 SO ASTROPHYSICAL JOURNAL LA English DT Article DE binaries : close; pulsars : individual (XTE J1807-294); stars : neutron; X-rays : binaries ID X-RAY BINARIES; NEUTRON-STAR; 4U 1608-52; NONLINEAR RESONANCE; TIMING FEATURES; SPIN FREQUENCY; POWER SPECTRA; VARIABILITY; SEPARATION; BEHAVIOR AB We report the discovery of twin kilohertz quasi-periodic oscillations (kHz QPOs) in the X-ray flux of XTE J1807 - 294, the fourth accreting millisecond pulsar (AMP). This is the second AMP exhibiting twin kHz QPOs. In contrast to the first case, SAX J1808.4 - 3658, the frequency separation Delta nu between these kHz QPOs is consistent with the pulse frequency ( 190.6 Hz), not with half that value, confirming for the first time from pulsation measurements the inference, based on burst oscillations, that ''slow rotators'' ( spin frequency less than 400 Hz) have Delta nu approximately equal to the spin frequency. While the QPOs move in frequency together over a range of more than 200 Hz, Delta nu remains constant with an average value of 205 +/- 6 Hz. Variability components were found in the 5-130 Hz range, similar to those seen in other LMXBs. The correlations between the QPO and noise frequencies are also similar to those in other sources, but shifted by a factor of 1.59 in kHz QPO frequencies, similar to the factor of 1.45 shift found for SAX J1808.4 - 3658. Our results argue in favor of a spin- related formation mechanism for twin kHz QPOs and against a spin- related cause of the shift in the frequency correlations. C1 Univ Amsterdam, Astron Inst Anton Pannekoek, NL-1098 SJ Amsterdam, Netherlands. Ctr High Energy Astrophys, NL-1098 SJ Amsterdam, Netherlands. NASA, Goddard Space Flight Ctr, High Energy Astrophys Lab, Greenbelt, MD 20771 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. RP Linares, M (reprint author), Univ Amsterdam, Astron Inst Anton Pannekoek, Kruislaan 403, NL-1098 SJ Amsterdam, Netherlands. NR 50 TC 54 Z9 56 U1 0 U2 1 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 DEC 1 PY 2005 VL 634 IS 2 BP 1250 EP 1260 DI 10.1086/497025 PN 1 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 988FO UT WOS:000233577700044 ER PT J AU Chen, CH Patten, BM Werner, MW Dowell, CD Stapelfeldt, KR Song, I Stauffer, JR Blaylock, M Gordon, KD Krause, V AF Chen, CH Patten, BM Werner, MW Dowell, CD Stapelfeldt, KR Song, I Stauffer, JR Blaylock, M Gordon, KD Krause, V TI A Spitzer study of dusty disks around nearby, young stars SO ASTROPHYSICAL JOURNAL LA English DT Article DE circumstellar matter; planetary systems : formation ID VEGA-LIKE STARS; MULTIBAND IMAGING PHOTOMETER; STELLAR KINEMATIC GROUPS; PICTORIS MOVING GROUP; A-TYPE STARS; SPACE-TELESCOPE; BETA-PICTORIS; DEBRIS DISKS; NORTHERN-HEMISPHERE; MASS STARS AB We have obtained Spitzer Space Telescope MIPS (Multiband Imaging Photometer for Spitzer) observations of 39A-throughM-type dwarfs, with estimated ages between 12 and 600 Myr; IRAC observations for a subset of 11 stars; and follow-up CSO SHARC II 350 mu m observations for a subset of two stars. None of the objects observed with IRAC possess infrared excesses at 3.6 - 8.0 mu m; however, seven objects observed with MIPS possess 24 and/or 70 mu m excesses. Four objects ( k Phe, HD 92945, HD 119124, and AU Mic), with estimated ages 12 - 200 Myr, possess strong 70 mu m excesses, >= 100% larger than their predicted photospheres, and no 24 mu m excesses, suggesting that the dust grains in these systems are cold. One object ( HD 112429) possesses moderate 24 and 70 mu m excesses with a color temperature, T-gr = 100K. Two objects (alpha(1)Lib and HD 177724) possess such strong 24 mu m excesses that their 12, 24, and 70 mu m fluxes cannot be self-consistently modeled using a modified blackbody despite a 70 mu m excess > 2 times greater than the photosphere around alpha(1)Lib. The strong 24 mu m excesses may be the result of emission in spectral features, as observed toward the Hale-Bopp star HD 69830. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Calif Los Angeles, Dept Phys & Astron, Los Angeles, CA 90095 USA. Natl Opt Astron Observ, Tucson, AZ 85719 USA. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. Gemini Observ, Hilo, HI 96720 USA. CALTECH, Spitzer Sci Ctr, Pasadena, CA 91125 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. RP Chen, CH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. RI Stapelfeldt, Karl/D-2721-2012 NR 63 TC 82 Z9 82 U1 0 U2 2 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 DEC 1 PY 2005 VL 634 IS 2 BP 1372 EP 1384 DI 10.1086/497124 PN 1 PG 13 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 988FO UT WOS:000233577700055 ER PT J AU Bhattacharyya, S Strohmayer, TE AF Bhattacharyya, S Strohmayer, TE TI Evidence for harmonic content and frequency evolution of oscillations during the rising phase of X-ray bursts from 4U 1636-536 SO ASTROPHYSICAL JOURNAL LA English DT Article DE equation of state; methods : data analysis; stars : neutron; X-rays : binaries X-rays : bursts; X-rays : individual (4U 1636-536) ID MILLISECOND PULSAR XTE-J1814-338; NEUTRON-STARS; BRIGHTNESS OSCILLATIONS; COHERENT OSCILLATIONS; LIGHT CURVES; COMPACTNESS; BINARY; BOUNDS AB We report on a study of the evolution of burst oscillation properties during the rising phase of X-ray bursts from 4U 1636-536 observed with the proportional counter array on board the Rossi X- Ray Timing Explorer (RXTE). We present evidence for significant harmonic structure of burst oscillation pulses during the early rising phases of bursts. This is the first such detection in burst rise oscillations and has interesting implications for constraining neutron star structure parameters and the equation-of-state models of matter at the core of a neutron star. The detection of harmonic content only during the initial portions of the burst rise appears consistent with the theoretical expectation that with time the thermonuclear burning region becomes larger, and hence the fundamental and harmonic amplitudes both diminish. We also find, for the first time from this source, strong evidence of frequency increases during burst rise. The timing behavior of harmonic content, amplitude, and frequency of burst rise oscillations may be important in understanding the spreading of thermonuclear flames under the extreme physical conditions on neutron star surfaces. C1 Univ Maryland, Dept Astron, College Pk, MD 20742 USA. NASA, Goddard Space Flight Ctr, Xray Astrophys Lab, Explorat Universe Div, Greenbelt, MD 20771 USA. RP Bhattacharyya, S (reprint author), Univ Maryland, Dept Astron, College Pk, MD 20742 USA. EM sudip@milkyway.gsfc.nasa.gov; stroh@clarence.gsfc.nasa.gov NR 21 TC 15 Z9 15 U1 0 U2 1 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 DEC 1 PY 2005 VL 634 IS 2 BP L157 EP L160 DI 10.1086/499100 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 988FQ UT WOS:000233578000009 ER PT J AU Falgarone, E Phillips, TG Pearson, JC AF Falgarone, E Phillips, TG Pearson, JC TI First detection of (CH+)-C-13 (J=1-0) SO ASTROPHYSICAL JOURNAL LA English DT Article DE astrochemistry; ISM : individual (G10.6-0.4); ISM : kinematics and dynamics; ISM : molecules; submillimeter; turbulence ID DIFFUSE INTERSTELLAR-MEDIUM; C-12/C-13 ISOTOPE RATIO; MASSIVE STAR-FORMATION; LINE-OF-SIGHT; MOLECULAR CLOUDS; CH+; ABSORPTION; REGIONS; H-2; SIGNATURES AB We report the probable detection of the (CH+)-C-13 (1-0) line in absorption against the dust continuum emission of a bright star-forming region, G10.6-0.4. If the (CH+)-C-13 line velocity centroid is that of the H (I) gas seen in absorption, the rest frequency we determine is 830.132(3) GHz. This is to be compared to the value of 830.131 GHz derived from new direct spectroscopy laboratory measurements of (CH+)-C-12 (1-0) and scaling from (CH+)-C-12 (1-0) to (CH+)-C-13 (1-0). However, if the (CH+)-C-13 line originated in either the star-forming region or in the intervening molecular gas as traced by (CO)-C-12 (1-0) emission, then the inferred rest frequency would be 830.107(1) or 830.193(4) GHz, respectively, both clearly out of the predicted range. We thus conclude that the (CH+)-C-13 line arises in a gas phase not traced by the (CO)-C-12 (1-0) line but one containing a large column density of cold H (I) and rich enough in H-2 to form CH+. Such properties are those of the cold neutral medium. The inferred column density is N((CH+)-C-13) = (2.2 +/- 0.4) x 10(12) cm(-2), corresponding to N(CH+) = (8.8 +/- 1.7) x 10(13) cm (-2) for an isotopic abundance ratio [(CH+)-C-12]/[(CH+)-C-13] = 40. With some assumptions concerning the H-2 content of the atomic gas, we estimate the total hydrogen column density in this velocity range and find a CH+ abundance relative to H about twice that in the solar neighborhood, as derived from optical absorption lines. C1 Ecole Normale Super, CNRS, UMR 8112, LERMA, F-75231 Paris, France. Observ Paris, F-75014 Paris, France. CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Falgarone, E (reprint author), Ecole Normale Super, CNRS, UMR 8112, LERMA, 24 Rue Lhomond, F-75231 Paris, France. NR 40 TC 24 Z9 24 U1 0 U2 1 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 DEC 1 PY 2005 VL 634 IS 2 BP L149 EP L152 DI 10.1086/499047 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 988FQ UT WOS:000233578000007 ER PT J AU Mennesson, B Koresko, C Creech-Eakman, MJ Serabyn, E Colavita, MM Akeson, R Appleby, E Bell, J Booth, A Crawford, S Dahl, W Fanson, J Felizardo, C Garcia, J Gathright, J Herstein, J Hovland, E Hrynevych, M Johansson, E Le Mignant, D Ligon, R Millan-Gabet, R Moore, J Neyman, C Palmer, D Panteleeva, T Paine, C Ragland, S Reder, L Rudeen, A Saloga, T Shao, M Smythe, R Summers, K Swain, M Tsubota, K Tyau, C Vasisht, G Wizinowich, P Woillez, J AF Mennesson, B Koresko, C Creech-Eakman, MJ Serabyn, E Colavita, MM Akeson, R Appleby, E Bell, J Booth, A Crawford, S Dahl, W Fanson, J Felizardo, C Garcia, J Gathright, J Herstein, J Hovland, E Hrynevych, M Johansson, E Le Mignant, D Ligon, R Millan-Gabet, R Moore, J Neyman, C Palmer, D Panteleeva, T Paine, C Ragland, S Reder, L Rudeen, A Saloga, T Shao, M Smythe, R Summers, K Swain, M Tsubota, K Tyau, C Vasisht, G Wizinowich, P Woillez, J TI The dusty agb star RS CrB: First mid-infrared interferometric observations with the Keck telescopes SO ASTROPHYSICAL JOURNAL LA English DT Article DE infrared : stars; instrumentation : interferometers; stars : individual ( RS Coronae Borealis); stars : late-type ID MIRA VARIABLES; LABORATORY PERFORMANCE; COOL STARS; O CETI; DIAMETERS; GIANT; SPECTROSCOPY; INSTRUMENT; ATMOSPHERE; SILICATES AB We report interferometric observations of the semiregular variable star RS CrB, a red giant with strong silicate emission features. The data were among the first long-baseline mid-infrared stellar fringes obtained between the Keck telescopes, using parts of the new nulling beam combiner. The light was dispersed by a low-resolution spectrometer, allowing simultaneous measurement of the source visibility and intensity spectra from 8 to 12 mu m. The interferometric observations allow a nonambiguous determination of the dust shell spatial scale and relative flux contribution. Using a simple spherically symmetric model, in which a geometrically thin shell surrounds the stellar photosphere, we find that similar to 30% to similar to 70% of the overall mid-infrared flux-depending on the wavelength originates from 7-8 stellar radii. The derived shell opacity profile shows a broad peak around 11 mu m ( tau similar or equal to), characteristic of Mg-rich silicate dust particles. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. CALTECH, Michelson Sci Ctr, Pasadena, CA 91125 USA. New Mexico Inst Min & Technol, Dept Phys, Socorro, NM 87801 USA. Calif Assoc Res Astron, WM Keck Observ, Kamuela, HI 96743 USA. RP Mennesson, B (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 37 TC 6 Z9 6 U1 0 U2 1 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 DEC 1 PY 2005 VL 634 IS 2 BP L169 EP L172 DI 10.1086/498864 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 988FQ UT WOS:000233578000012 ER PT J AU Stanford, SA Eisenhardt, PR Brodwin, M Gonzalez, AH Stern, D Jannuzi, BT Dey, A Brown, MJI McKenzie, E Elston, R AF Stanford, SA Eisenhardt, PR Brodwin, M Gonzalez, AH Stern, D Jannuzi, BT Dey, A Brown, MJI McKenzie, E Elston, R TI An IR-selected galaxy cluster at z=1.41 SO ASTROPHYSICAL JOURNAL LA English DT Article DE galaxies : clusters : general; galaxies : evolution; galaxies : formation ID COLOR-MAGNITUDE RELATION; SPITZER-SPACE-TELESCOPE; ARRAY CAMERA IRAC; DISTANT CLUSTERS; EVOLUTION; RDCS-1252.9-2927; Z-SIMILAR-TO-1; PHOTOMETRY; MORPHOLOGY AB We report the discovery of a galaxy cluster at z = 1.41. ISCS J143809 + 341419 was found in the Spitzer/IRAC Shallow Survey of the Bootes field in the NOAO Deep Wide- Field Survey carried out using IRAC. The cluster candidate was initially identified as a high-density region of objects with photometric redshifts in the range 1.31 < z < 1.5. Optical spectroscopy of a limited number of objects in the region shows that five galaxies within an similar to 120" diameter region lie at z = 1.41 +/- 0.01. Most of these member galaxies have broadband colors consistent with the expected spectral energy distribution of a passively evolving elliptical galaxy formed at high redshift. The redshift of ISCS J143809 + 341419 is the highest currently known for a spectroscopically confirmed cluster of galaxies. C1 Univ Calif Davis, Dept Phys, Davis, CA 95616 USA. Lawrence Livermore Natl Lab, Inst Geophys & Planetary Phys, Livermore, CA 94551 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Florida, Dept Astron, Gainesville, FL 32611 USA. Natl Opt Astron Observ, Tucson, AZ 85726 USA. Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA. RP Stanford, SA (reprint author), Univ Calif Davis, Dept Phys, 1 Shields Ave, Davis, CA 95616 USA. EM adam@igpp.ucllnl.org; prme@kromos.jpl.nasa.gov; mark.brodwin@jpl.nasa.gov; anthony@astro.ufl.edu; stern@thisvi.jpl.nasa.gov; jannuzi@noao.edu; dey@noao.edu; mbrown@astro.princeton.edu; eric@astro.ufl.edu RI Brown, Michael/B-1181-2015 OI Brown, Michael/0000-0002-1207-9137 NR 33 TC 104 Z9 104 U1 0 U2 2 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 DEC 1 PY 2005 VL 634 IS 2 BP L129 EP L132 DI 10.1086/499045 PN 2 PG 4 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 988FQ UT WOS:000233578000002 ER PT J AU Sekanina, Z Chodas, PW AF Sekanina, Z Chodas, PW TI Origin of the Marsden and Kracht groups of sunskirting comets. I. Association with comet 96P/Machholz and its interplanetary complex SO ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES LA English DT Article DE celestial mechanics; comets : general; comets : individual (96P/Machholz, 8P/Tuttle, C/1490Y1, C/1882 R1, C/1965 S1, C/1992 F2, C/1996 V2, C/1997 L2, C/1998 A2, C/1998 A3, C/1998 A4, C/1999 J6, C/1999 M3, C/1999 N5, C/1999 N6, C/1999 P6, C/1999 P8, C/1999 P9, C/1999 U2, C/2000 C2, C/2000 C3, C/2000 C4, C/2000 C5, C/2000 C7, C/2000 O3, C/2001 E1, C/2001 Q7, C/2001 Q8, C/2001 R8, C/2001 R9, C/2001 X8, C/2002 N2, C/2002 Q8, C/2002 Q10, C/2002 R1, C/2002 R4, C/2002 S4, C/2002 S5, C/2002 S7, C/2002 S11, C/2002 V5, C/2003 Q1, C/2003 Q6, C/2004 A3, C/2004 B3, C/2004 J4, C/2004 J12, C/2004 J13, C/2004 J15, C/2004 J16, C/2004 J17, C/2004 J18, C/2004 L10, C/2004 V9, C/2004 V10, C/2004 W10, C/2005 E4, C/2005 G2); meteors, meteoroids; methods : data analysis; methods : n-body simulations; methods : statistical; minor planets, asteroids ID QUADRANTID METEOR STREAM; SUNGRAZING COMETS; STATISTICAL-MODEL; ORBITAL ANOMALIES; PERIODIC COMETS; RADIO METEORS; SPLIT COMETS; 2003 EH1; FRAGMENTATION; MACHHOLZ AB Of the three major groups of comets approaching the Sun to between 6 and 12 solar radii and discovered with the coronagraphs on board SOHO, we investigate the Marsden and Kracht groups. We call these comets "sunskirters" to distinguish them from the Kreutz system sungrazers. Our objective is to understand the origin, history, and orbital evolution of the two groups. The tendency for their members to arrive at perihelion in pairs or clusters is a result of their recent fragmentation. As fragments of more massive precursor objects, the Marsden- and Kracht-group comets are mostly less than 10 yr old. Although the two groups and several meteoroid swarms, such as the Daytime Arietids and Southern delta Aquarids, appear as separate populations of a complex associated with comet 96P/Machholz, our orbit integrations suggest that we deal with a single, essentially continuous population that extends from the comet's orbit for more than 160 degrees in the longitude of the node. First-generation fragments of their common progenitor with comet 96P, which were the initial direct ancestors of this population, are called the first precursors. Nearly 60,000 orbit integration runs are made in our search for their birth scenarios. We find that these objects separated from the progenitor comet before AD 950 and, as sources of continuing activity, pursued an orbital evolution very different from that of 96P. All first precursors of this low-inclination population experienced a sequence of encounters with Jupiter within 0.5 AU, starting in AD 1059 or earlier and continuing for centuries. In the process, they split into smaller pieces in a fashion reminiscent of "cascading" fragmentation of the Kreutz system. The secular planetary (mainly Jovian) perturbations control the motions of both 96P and the low-inclination population, but the dynamical evolution of the latter has been markedly accelerated by Jupiter during close encounters, so that the population's present-day orbital changes are similar to those the comet will undergo centuries from now. Precursors to the Southern delta Aquarids of the 1950s passed through the Marsden-group stage around 1700 and through the Kracht-group stage in the 1780s. The Daytime Arietids appear to be related most directly to the Marsden- group comets, which can closely approach Earth around June 12, the time of the stream's peak activity. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Sekanina, Z (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM zs@sek.jpl.nasa.gov; paul.w.chodas@jpl.nasa.gov NR 69 TC 29 Z9 29 U1 1 U2 5 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 DEC PY 2005 VL 161 IS 2 BP 551 EP 586 DI 10.1086/497374 PG 36 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993CO UT WOS:000233930500014 ER PT J AU Mironov, V Kasyanov, V Shu, XZ Eisenberg, C Eisenberg, L Gonda, S Trusk, T Markwald, RR Prestwich, GD AF Mironov, V Kasyanov, V Shu, XZ Eisenberg, C Eisenberg, L Gonda, S Trusk, T Markwald, RR Prestwich, GD TI Fabrication of tubular tissue constructs by centrifugal casting of cells suspended in an in situ crosslinkable hyaluronan-gelatin hydrogel SO BIOMATERIALS LA English DT Article DE centrifugal casting; thiol-modified gelatin; glycosaminoglycan; tubular construct; synthetic extracellular matrix ID BLOOD-VESSEL; VITRO; SCAFFOLDS; GROWTH; FORCE; FILMS AB Achieving the optimal cell density and desired cell distribution in scaffolds is a major goal of cell seeding technologies in tissue engineering. In order to reach this goal, a novel centrifugal casting technology was developed using in situ crosslinkable hyaluronan-based (HA) synthetic extracellular matrix (sECM). Living cells were suspended in a viscous solution of thiol-modified HA and thiol-modified gelatin, a polyethyleneglycol diacrylate crosslinker was added, and a hydrogel was formed during rotation. The tubular tissue constructs consisting of a densely packed cell layer were fabricated with the rotation device operating at 2000 rpm for 10 min. The majority of cells suspended in the HA mixture before rotation were located inside the layer after centrifugal casting. Cells survived the effect of the centrifugal forces experienced under the rotational regime employed. The volume cell density (65.6%) approached the maximal possible volume density based on theoretical sphere packing models. Thus, centrifugal casting allows the fabrication of tubular constructs with the desired redistribution, composition and thickness of cell layers that makes the maximum efficient use of available cells. Centrifugal casting in this sECM would enable rapid fabrication of tissue-engineered vascular grafts, as well as other tubular and planar tissue-engineered constructs. (c) 2005 Elsevier Ltd. All rights reserved. C1 Med Univ S Carolina, Charleston, SC 29426 USA. Riga Stradins Univ, LV-1007 Riga, Latvia. Univ Utah, Ctr Therapeut Biomat, Salt Lake City, UT 84108 USA. Univ Utah, Dept Med Chem, Salt Lake City, UT 84108 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Mironov, V (reprint author), Med Univ S Carolina, Charleston, SC 29426 USA. EM mironovv@musc.edu FU NIDCD NIH HHS [DC04336] NR 22 TC 53 Z9 58 U1 1 U2 29 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0142-9612 J9 BIOMATERIALS JI Biomaterials PD DEC PY 2005 VL 26 IS 36 BP 7628 EP 7635 DI 10.1016/j.biomaterials.2005.05.061 PG 8 WC Engineering, Biomedical; Materials Science, Biomaterials SC Engineering; Materials Science GA 966AK UT WOS:000231991800013 PM 16023201 ER PT J AU Anderson, TL Charlson, RJ Bellouin, N Boucher, O Chin, M Christopher, SA Haywood, J Kaufman, YJ Kinne, S Ogren, JA Remer, LA Takemura, T Tanre, D Torres, O Trepte, CR Wielicki, BA Winker, DM Yu, HB AF Anderson, TL Charlson, RJ Bellouin, N Boucher, O Chin, M Christopher, SA Haywood, J Kaufman, YJ Kinne, S Ogren, JA Remer, LA Takemura, T Tanre, D Torres, O Trepte, CR Wielicki, BA Winker, DM Yu, HB TI An "A-Train" strategy for quantifying direct climate forcing by anthropogenic aerosols SO BULLETIN OF THE AMERICAN METEOROLOGICAL SOCIETY LA English DT Article ID OPTICAL DEPTH; SATELLITE MEASUREMENTS; RADIATIVE PROPERTIES; SOOT AEROSOL; SAFARI 2000; OCEANS; AERONET; ATMOSPHERE; VARIABILITY; AIRCRAFT AB This document outlines a practical strategy for achieving an observationally based quantification of direct climate forcing by anthropogenic aerosols. The strategy involves a four-step program for shifting the current assumption-laden estimates to an increasingly empirical basis using satellite observations coordinated with suborbital remote and in situ measurements and with chemical transport models. Conceptually, the problem is framed as a need for complete global mapping of four parameters: clear-sky aerosol optical depth 8, radiative efficiency per unit optical depth E, fine-mode fraction of optical depth f(f) and the anthropogenic fraction of the fine a(f). The first three parameters can be retrieved from satellites, but correlative, suborbital measurements are required for quantifying the aerosol properties that control E, for validating the retrieval of f(f), and for partitioning fine-mode delta between natural and anthropogeniccomponents. The satellite focus is on the "A-Train," a constellation of six spacecraft that will fly in formation from about 2005 to 2008. Key satellite instruments for this report are the Moderate Resolution Imaging Spectroradiometer (MODIS) and Clouds and the Earth's Radiant Energy System (CERES) radiometers on Aqua, the Ozone Monitoring, Instrument (OMI) radiometer on Aura, the Polarization and Directionality of Earth's Reflectances (POLDER) polarimeter on the Polarization and Anistropy of Reflectances for Atmospheric Sciences Coupled with Observations from a Lidar (PARASOL), and the Cloud and Aerosol Lider with Orthogonal Polarization (CALIOP) lidar on the Cloud-Aerosol Lidar and Infrared Pathfinder Satellite Observations (CALIPSO). This strategy is offered as an framework-subject to improvement over time-for scientists around the world to participate in the A-Train opportunity. It is a specific implementation of the Progressive Aerosol Retrieval and Assimilation Global Observing Network (PARAGON) program, presented earlier in this journal, which identified the integration of diverse data as the central challenge to progress in quantifying global-scale aerosol effects. By designing a strategy around this need for integration, we develop recommendations for both satellite data interpretation and correlative suborbital activities that represent, in many respects, departures from current practice. C1 Univ Washington, Seattle, WA 98195 USA. Met Off, Exeter, Devon, England. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Alabama, Huntsville, AL USA. Max Planck Inst Meteorol, Hamburg, Germany. NOAA CMDL, Boulder, CO USA. Kyushu Univ, Fukuoka, Kyushu, Japan. Univ Lille, Lille, France. JCTE Univ Maryland, Baltimore, MD USA. NASA Langley Res Ctr, Hampton, VA USA. Univ Maryland Baltimore Cty, Baltimore, MD 21228 USA. RP Anderson, TL (reprint author), Univ Washington, Dept Atmospher Sci, Room 408 ATG, Seattle, WA 98195 USA. EM tadand@u.washington.edu RI Yu, Hongbin/C-6485-2008; Christopher, Sundar/E-6781-2011; Takemura, Toshihiko/C-2822-2009; Boucher, Olivier/J-5810-2012; Chin, Mian/J-8354-2012; Boucher, Olivier/K-7483-2012; Torres, Omar/G-4929-2013; Ogren, John/M-8255-2015; U-ID, Kyushu/C-5291-2016; Kyushu, RIAM/F-4018-2015; OI Yu, Hongbin/0000-0003-4706-1575; Takemura, Toshihiko/0000-0002-2859-6067; Boucher, Olivier/0000-0003-2328-5769; Boucher, Olivier/0000-0003-2328-5769; Ogren, John/0000-0002-7895-9583; Bellouin, Nicolas/0000-0003-2109-9559 NR 53 TC 86 Z9 88 U1 5 U2 37 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 DEC PY 2005 VL 86 IS 12 BP 1795 EP + DI 10.1175/BAMS-86-12-1795 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 003CX UT WOS:000234660300020 ER PT J AU Goericke, R Venrick, E Mantyla, A Bograd, SJ Schwing, FB Huyer, A Smith, RL Wheeler, PA Hooff, R Peterson, WT Chavez, F Collins, C Marinovic, B Lo, N Gaxiola-Castro, G Durazo, R Hyrenbach, KD Sydeman, WJ AF Goericke, R Venrick, E Mantyla, A Bograd, SJ Schwing, FB Huyer, A Smith, RL Wheeler, PA Hooff, R Peterson, WT Chavez, F Collins, C Marinovic, B Lo, N Gaxiola-Castro, G Durazo, R Hyrenbach, KD Sydeman, WJ TI The state of the California current, 2004-2005: Still cool? SO CALIFORNIA COOPERATIVE OCEANIC FISHERIES INVESTIGATIONS REPORTS LA English DT Article ID EL-NINO; CLIMATE-CHANGE; CURRENT SYSTEM; OCEANOGRAPHIC CONDITIONS; ZOOPLANKTON COMMUNITY; PACIFIC-OCEAN; NORTH PACIFIC; OREGON; OSCILLATION; SCALES AB This report summarizes the recent state of the California Current System (CCS), primarily during the period of April 2004 to January 2005. The report is based on observations made between Oregon and Baja California by various ocean observing programs. The CCS was not forced by any coherent basin-wide processes during the observation period. The weak tropical El Nino of 2004 did not appear to have had a noticeable effect on the CCS. However, the CCS remains in a cold phase, a state it has had since the 1999 La Nina phase. Some biological parameters show a distinct response to this state, i.e. zooplankton biomass and its species richness, others display a mixed response such as the CCS avifauna and its productivity, and some do not show any response, such as phytoplankton biomass and Pacific sardine (Sardinops sagax) productivity. Over all, the state of the system remains "normal" with respect to its climatology. The unusual intrusion of cold and fresh subarctic water into the CCS is waning off Oregon but still noticeable off southern California and off Baja California. Because the CCS does not appear subject to coherent basin-wide forcing, the outlook for the CCS over the next years is uncertain. C1 Univ Calif San Diego, Scripps Inst Oceanog, Integrat Oceanog Div, La Jolla, CA 92093 USA. Oregon State Univ, Hatfield Marine Sci Ctr, Cooperat Inst Marine Resource Studies, Newport, OR 97365 USA. USN, Postgrad Sch, Dept Oceanog, Monterey, CA 93943 USA. Ctr Invest Cient & Educ Super Ensenada, Dept Oceanog Biol, Ensenada 22860, Baja California, Mexico. NOAA, Natl Marine Fisheries Serv, SW Fisheries Sci Ctr, Div Environm Res, Pacific Grove, CA 93950 USA. Natl Marine Fisheries Serv, NW Fisheries Sci Ctr, Hatfield Marine Sci Ctr, Newport, OR 97365 USA. Univ Calif Santa Cruz, Long Marine Lab, Santa Cruz, CA 95060 USA. Univ Autonoma Baja California, Fac Ciencias Marinas, Ensenada, Baja California, Mexico. Oregon State Univ, Coll Ocean & Atmospher Sci, Corvallis, OR 97331 USA. Monterey Bay Aquarium Res Inst, Moss Landing, CA 95039 USA. SW Fisheries Sci Ctr, La Jolla, CA 92038 USA. Point Reyes Bird Observ, Marine Ecol Div, Stinson Beach, CA 94970 USA. RP Goericke, R (reprint author), Univ Calif San Diego, Scripps Inst Oceanog, Integrat Oceanog Div, La Jolla, CA 92093 USA. EM rgoericke@ucsd.edu NR 36 TC 40 Z9 43 U1 0 U2 6 PU SCRIPPS INST OCEANOGRAPHY PI LA JOLLA PA A-003, LA JOLLA, CA 92093 USA SN 0575-3317 J9 CAL COOP OCEAN FISH JI Calif. Coop. Ocean. Fish. Invest. Rep. PD DEC PY 2005 VL 46 BP 32 EP 71 PG 40 WC Fisheries SC Fisheries GA 021EZ UT WOS:000235967800004 ER PT J AU Seidelmann, PK Archinal, BA A'Hearn, MF Cruikshank, DP Hilton, JL Keller, HU Oberst, J Simon, JL Stooke, P Tholen, DJ Thomas, PC AF Seidelmann, PK Archinal, BA A'Hearn, MF Cruikshank, DP Hilton, JL Keller, HU Oberst, J Simon, JL Stooke, P Tholen, DJ Thomas, PC TI Report of the IAU/IAG Working Group on Cartographic Coordinates and Rotational Elements: 2003 SO CELESTIAL MECHANICS & DYNAMICAL ASTRONOMY LA English DT Article DE asteroids; cartographic coordinates; comets; planets; rotation axes; rotation periods; satellites; shapes; sizes ID RADAR OBSERVATIONS AB Every three years the IAU/IAG Working Group on Cartographic Coordinates and Rotational Elements revises tables giving the directions of the north poles of rotation and the prime meridians of the planets, satellites, and asteroids. This report introduces a system of cartographic coordinates for asteroids and comets. A topographic reference surface for Mars is recommended. Tables for the rotational elements of the planets and satellites and size and shape of the planets and satellites are not included, since there were no changes to the values. They are available in the previous report (Celest. Mech. Dyn. Astron., 82, 83-110, 2002), a version of which is also available on a web site. C1 Univ Virginia, Charlottesville, VA 22903 USA. US Geol Survey, Flagstaff, AZ 86001 USA. Univ Maryland, College Pk, MD 20742 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. USN Observ, Washington, DC 20392 USA. MPI Aeron, Katlenburg Lindau, Germany. DLR Berlin Adlershof, Berlin, Germany. Inst Mecan Celeste, Paris, France. Univ Western Ontario, London, ON, Canada. Univ Hawaii, Honolulu, HI 96822 USA. Cornell Univ, Ithaca, NY USA. RP Seidelmann, PK (reprint author), Univ Virginia, Charlottesville, VA 22903 USA. NR 12 TC 16 Z9 17 U1 0 U2 3 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0923-2958 J9 CELEST MECH DYN ASTR JI Celest. Mech. Dyn. Astron. PD DEC PY 2005 VL 91 IS 3-4 BP 203 EP 215 DI 10.1007/s10569-004-3115-4 PG 13 WC Astronomy & Astrophysics; Mathematics, Interdisciplinary Applications SC Astronomy & Astrophysics; Mathematics GA 954OE UT WOS:000231163600001 ER PT J AU Werner, RA Scheeres, DJ AF Werner, RA Scheeres, DJ TI Mutual potential of homogeneous polyhedra SO CELESTIAL MECHANICS & DYNAMICAL ASTRONOMY LA English DT Article DE inertia integral; mutual potential; polyhedron potential; two rigid bodies problem ID BODIES AB The mutual gravitational potential between a pair of homogeneous polyhedra is expressed using an infinite series. The nested volume integrals are evaluated analytically and result in simple tensor expressions containing no special functions. However, complexity increases as O(6(n)), where n is the term degree. An alternate formulation due to Liebenthal is also presented. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Michigan, Dept Aerosp Engn, Ann Arbor, MI 48109 USA. RP Werner, RA (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM robert.a.werner@jpl.nasa.gov; scheeres@umich.edu NR 9 TC 19 Z9 19 U1 0 U2 4 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0923-2958 J9 CELEST MECH DYN ASTR JI Celest. Mech. Dyn. Astron. PD DEC PY 2005 VL 91 IS 3-4 BP 337 EP 349 DI 10.1007/s10569-004-4621-0 PG 13 WC Astronomy & Astrophysics; Mathematics, Interdisciplinary Applications SC Astronomy & Astrophysics; Mathematics GA 954OE UT WOS:000231163600008 ER PT J AU Nomura, Y Mulavara, AP Richards, JT Brady, R Bloomberg, JJ AF Nomura, Y Mulavara, AP Richards, JT Brady, R Bloomberg, JJ TI Optic flow dominates visual scene polarity in causing adaptive modification of locomotor trajectory SO COGNITIVE BRAIN RESEARCH LA English DT Article DE optic flow; visual polarity; adaptation; locomotion control ID VENTRAL INTRAPARIETAL AREA; CANADIAN VESTIBULAR EXPERIMENTS; SELF-MOTION; OPTOKINETIC STIMULATION; SPATIAL ORIENTATION; VIRTUAL ENVIRONMENT; HEADING PERCEPTION; SPACELAB-1 MISSION; WALKING; ADAPTATION AB Locomotion and posture are influenced and controlled by vestibular, visual and somatosensory information. Optic flow and scene polarity are two characteristics of a visual scene that have been identified as being critical in how they affect perceived body orientation and self motion. The goal of this study was to determine the role of optic flow and visual scene polarity on adaptive modification in locomotor trajectory. An object is said to have visual polarity, or to be "visually polarized", when it contains an identifiable principal axis with one end distinct from the other. Two computer-generated virtual reality scenes were shown to subjects during 20 min of treadmill walking. One scene was a highly polarized scene, while the other was composed of objects displayed in a non-polarized fashion. Both virtual scenes depicted constant rate self motion equivalent to walking counterclockwise around the perimeter of a room. Subjects performed Stepping Tests blindfolded before and after scene exposure to assess adaptive changes in locomotor trajectory. Subjects showed a significant difference in heading direction, between pre- and post-adaptation Stepping Tests, when exposed to either scene during treadmill walking. However, there was no significant difference in the subjects' heading direction between the two visual scene polarity conditions. Therefore, it was inferred from these data that optic flow has a greater role than visual polarity in influencing adaptive locomotor function. (c) 2005 Elsevier B.V. All rights reserved. C1 Wyle Life Sci Inc, Houston, TX 77058 USA. Nihon Univ, Sch Med, Tokyo 1738610, Japan. Natl Space Biomed Res Inst, Houston, TX 77030 USA. NASA, Johnson Space Ctr, Houston, TX 77058 USA. RP Mulavara, AP (reprint author), Wyle Life Sci Inc, Houston, TX 77058 USA. EM mulavara@bcm.tmc.edu NR 54 TC 8 Z9 9 U1 0 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0926-6410 J9 COGNITIVE BRAIN RES JI Cognit. Brain Res. PD DEC PY 2005 VL 25 IS 3 BP 624 EP 631 DI 10.1016/j.cogbrainres.2005.08.012 PG 8 WC Computer Science, Artificial Intelligence; Neurosciences; Neuroimaging SC Computer Science; Neurosciences & Neurology GA 997HQ UT WOS:000234236500003 PM 16216478 ER PT J AU Gates, TS Odegard, GM Frankland, SJV Clancy, TC AF Gates, TS Odegard, GM Frankland, SJV Clancy, TC TI Computational materials: Multi-scale modeling and simulation of nanostructured materials SO COMPOSITES SCIENCE AND TECHNOLOGY LA English DT Article DE multi-scale modeling; computational materials; nanotechnology ID MOLECULAR-DYNAMICS SIMULATION; REINFORCED POLYMER COMPOSITES; STRUCTURAL MECHANICS APPROACH; WALLED CARBON NANOTUBES; CONTINUUM MODELS; ATOMIC-SCALE; LATTICE STRUCTURES; ELASTIC-MODULI; LENGTH SCALES; FORCE-FIELD AB The paper provides details on the current approach to multi-scale modeling and simulation of advanced materials for structural applications. Examples are given that illustrate the suggested approaches to predicting the behavior and influencing the design of nanostructured materials such as high-performance polymers, composites, and nanotube-reinforced polymers. Primary simulation and measurement methods applicable to multi-scale modeling are outlined. Key challenges including verification and validation are highlighted and discussed. (c) 2005 Elsevier Ltd. All rights reserved. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. Michigan Technol Univ, Houghton, MI 49931 USA. Natl Inst Aerosp, Hampton, VA 23666 USA. RP NASA, Langley Res Ctr, MS 188E, Hampton, VA 23681 USA. EM t.s.gates@larc.nasa.gov OI Odegard, Gregory/0000-0001-7577-6565 NR 79 TC 115 Z9 117 U1 1 U2 49 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0266-3538 EI 1879-1050 J9 COMPOS SCI TECHNOL JI Compos. Sci. Technol. PD DEC PY 2005 VL 65 IS 15-16 SI SI BP 2416 EP 2434 DI 10.1016/j.compscitech.2005.06.009 PG 19 WC Materials Science, Composites SC Materials Science GA 981GR UT WOS:000233076100013 ER PT J AU Bouhram, M Berthelier, JJ Illiano, JM Smith, HT Sittler, EC Crary, FJ Young, DT AF Bouhram, M Berthelier, JJ Illiano, JM Smith, HT Sittler, EC Crary, FJ Young, DT TI The Enceladus satellite as a source of N+ ions in Saturn's magnetosphere. SO COMPTES RENDUS PHYSIQUE LA French DT Article DE planetary science; plasmas; Saturn; rings and icy satellites; magnetosphere ID PLASMA OBSERVATIONS AB The first pass of the Cassini probe in the vicinity of Saturn, above the E-ring, demonstrated a plasma consisting of water group ions (H+, O+, OH+, H2O+) with a small N+ ion component (3%). Using a simple model for the transport of magnetospheric ions, we show that the N+ ions can be traced back to the Enceladus satellite. Such a result can be explained by the existence in this icy satellite, supposed to be still geologically active, of volatile components such as ammonia NH3, or by the previous implantation of N+ ions of external origin on its surface. C1 Ctr Etud Environm Terrestre & Planetaires, F-94100 St Maur des Fosses, France. Univ Virginia, Charlottesville, VA 22904 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. SW Res Inst, San Antonio, TX 78238 USA. RP Bouhram, M (reprint author), Ctr Etud Environm Terrestre & Planetaires, 4 Ave Neptune, F-94100 St Maur des Fosses, France. EM mehdi.bouhram@cetp.ipsl.fr RI Smith, Howard/H-4662-2016 OI Smith, Howard/0000-0003-3537-3360 NR 15 TC 3 Z9 3 U1 0 U2 0 PU ELSEVIER FRANCE-EDITIONS SCIENTIFIQUES MEDICALES ELSEVIER PI PARIS PA 23 RUE LINOIS, 75724 PARIS, FRANCE SN 1631-0705 J9 CR PHYS JI C. R. Phys. PD DEC PY 2005 VL 6 IS 10 BP 1176 EP 1181 DI 10.1016/j.crhy.2005.12.008 PG 6 WC Astronomy & Astrophysics; Physics, Multidisciplinary SC Astronomy & Astrophysics; Physics GA 010VQ UT WOS:000235226400017 ER PT J AU Matese, JJ Whitmire, DP Lissauer, JJ AF Matese, John J. Whitmire, Daniel P. Lissauer, Jack J. TI A Widebinary solar companion as a possible origin of Sedna-like objects SO EARTH MOON AND PLANETS LA English DT Article; Proceedings Paper CT Asteroids, Comets and Meteors Meeting CY AUG, 2005 CL Buzios, BRAZIL DE Kuiper Belt; Oort Cloud; comets : 2003 VB12; comets : general; binaries : general ID TRANS-NEPTUNIAN OBJECTS; OORT CLOUD; CANDIDATE; ORBITS AB Sedna is the first inner Oort cloud object to be discovered. Its dynamical origin remains unclear, and a possible mechanism is considered here. We investigate the parameter space of a hypothetical solar companion which could adiabatically detach the perihelion of a Neptune-dominated TNO with a Sedna-like semimajor axis. Demanding that the TNO's maximum value of osculating perihelion exceed Sedna's observed value of 76 AU, we find that the companion's mass and orbital parameters (m(c), a(c), q(c), Q(c), i(c)) are restricted to m(c) greater than or similar to 5 M-J(Q(c)/7850 AU q(c)/7850 AU)(3/2) during the epoch of strongest perturbations. The ecliptic inclination of the companion should be in the range 45 degrees less than or similar to i(c) less than or similar to 135 degrees if the TNO is to retain a small inclination while its perihelion is increased. We also consider the circumstances where the minimum value of osculating perihelion would pass the object to the dynamical dominance of Saturn and Jupiter, if allowed. It has previously been argued that an overpopulated band of outer Oort cloud comets with an anomalous distribution of orbital elements could be produced by a solar companion with present parameter values m(c) approximate to 5 M-J(9000 AU/a(c))(1/2). If the same hypothetical object is responsible for both observations, then it is likely recorded in the IRAS and possibly the 2MASS databases. C1 Univ Louisiana, Dept Phys, Lafayette, LA 70504 USA. NASA, Space Sci & Astrobiol Div, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Matese, JJ (reprint author), Univ Louisiana, Dept Phys, Lafayette, LA 70504 USA. EM matese@louisiana.edu NR 11 TC 12 Z9 12 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0167-9295 J9 EARTH MOON PLANETS JI Earth Moon Planets PD DEC PY 2005 VL 97 IS 3-4 BP 459 EP 470 DI 10.1007/s11038-006-9078-6 PG 12 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA 092WN UT WOS:000241128100022 ER PT J AU Hildebr, AR Cardinal, RD Carroll, KA Faber, DR Tedesco, EF Matthews, JM Kuschnig, R Walker, GAH Gladman, B Pazder, J Brown, PG Larson, SM Worden, SP Wallace, BJ Chodas, PW Muinonen, K Cheng, A AF Hildebr, AR Cardinal, RD Carroll, KA Faber, DR Tedesco, EF Matthews, JM Kuschnig, R Walker, GAH Gladman, B Pazder, J Brown, PG Larson, SM Worden, SP Wallace, BJ Chodas, PW Muinonen, K Cheng, A TI Advantages of searching for asteroids from low Earth orbit: The NEOSSat mission SO EARTH MOON AND PLANETS LA English DT Article; Proceedings Paper CT Meteoroids 2004 Conference CY AUG 16-20, 2004 CL Univ Western Ontario, London, ENGLAND HO Univ Western Ontario DE asteroid; asteroid searching; Aten; IEO; microsatellite mission; NEOs; NEOSSat spacecraft; NESS project; observing parallax ID SPACE AB Space-based observatories have several advantages over ground-based observatories in searching for asteroids and comets. In particular, the Aten and Interior to Earth's Orbit (IEO) asteroid classes may be efficiently sought at low solar elongations along the ecliptic plane. A telescope in low Earth orbit has a sufficiently long orbital baseline to determine the parallax for all Aten and IEO class asteroids discovered with this observing strategy. The Near Earth Object Space Surveillance Satellite (NEOSSat) mission will launch a microsatellite to exploit this observing strategy complementing ground-based search programmes. C1 Univ Calgary, Dept Geol & Geophys, Calgary, AB T2N 1N4, Canada. Dynacon Inc, Mississauga, ON L4V 1R1, Canada. Univ New Hampshire, Ctr Space Sci, Durham, NH 03824 USA. Univ British Columbia, Dept Phys & Astron, Vancouver, BC V6T 1Z1, Canada. Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7, Canada. Univ Western Ontario, Dept Phys & Astron, London, ON N6A 3K7, Canada. Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. Dept Astron, Tucson, AZ 85721 USA. Univ Arizona, Steward Observ, Tucson, AZ 85721 USA. Def Res & Dev Canada, Ottawa, ON K1A 0Z4, Canada. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Helsinki Observ, FIN-00014 Helsinki, Finland. Johns Hopkins Univ, Appl Phys Lab, Laurel, MD 20723 USA. RP Hildebr, AR (reprint author), Univ Calgary, Dept Geol & Geophys, 2500 Univ Dr NW, Calgary, AB T2N 1N4, Canada. EM ahildebr@ucalgary.ca NR 14 TC 8 Z9 8 U1 0 U2 7 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0167-9295 J9 EARTH MOON PLANETS JI Earth Moon Planets PD DEC PY 2005 VL 95 IS 1-4 BP 33 EP 40 DI 10.1007/s11038-005-9016-z PG 8 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA 022VF UT WOS:000236083500006 ER PT J AU McNamara, H Suggs, R Kauffman, B Jones, J Cooke, W Smith, S AF McNamara, H Suggs, R Kauffman, B Jones, J Cooke, W Smith, S TI Meteoroid engineering model (MEM): A meteoroid model for the inner solar system SO EARTH MOON AND PLANETS LA English DT Article; Proceedings Paper CT Meteoroids 2004 Conference CY AUG 16-20, 2004 CL Univ Western Ontario, London, ENGLAND HO Univ Western Ontario DE engineering model; interplanetary; sporadic meteoroids AB In an attempt to overcome some of the deficiencies of existing meteoroid models, NASA's Space Environments and Effects (SEE) Program sponsored a 3 year research effort at the University of Western Ontario. The resulting understanding of the sporadic meteoroid environment - particularly the nature and distribution of the sporadic sources - were then incorporated into a new Meteoroid Engineering Model (MEM) by members of the Space Environments Team at NASA's Marshall Space Flight Center. This paper discusses some of the revolutionary aspects of MEM which include (a) identification of the sporadic radiants with real sources of meteoroids, such as comets, (b) a physics-based approach which yields accurate fluxes and directionality for interplanetary spacecraft anywhere from 0.2 to 2.0 astronomical units (AU), and (c) velocity distributions obtained from theory and validated against observation. Use of the model, which gives penetrating fluxes and average impact speeds on the surfaces of a cube-like structure, is also described along with its current limitations and plans for future improvements. C1 NASA, Space Environm Team, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. NASA, Space Environm & Effects Program, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. Univ Western Ontario, Dept Phys, London, ON N6A 3K7, Canada. RP McNamara, H (reprint author), NASA, Space Environm Team, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. EM heather.a.mcnamara@nasa.gov NR 30 TC 17 Z9 17 U1 1 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0167-9295 J9 EARTH MOON PLANETS JI Earth Moon Planets PD DEC PY 2005 VL 95 IS 1-4 BP 123 EP 139 DI 10.1007/s11038-005-9044-8 PG 17 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA 022VF UT WOS:000236083500016 ER PT J AU Moser, DE Cooke, WJ AF Moser, DE Cooke, WJ TI MSFC stream model preliminary results: Modeling recent Leonid and Perseid encounters SO EARTH MOON AND PLANETS LA English DT Article; Proceedings Paper CT Meteoroids 2004 Conference CY AUG 16-20, 2004 CL Univ Western Ontario, London, ENGLAND HO Univ Western Ontario DE comet; comet ejection; Leonids; meteor; meteor shower; meteoroids; model predictions; numerical integration; Perseids ID COMET P/SWIFT-TUTTLE; VISUAL OBSERVATIONS; METEOR STORMS; EJECTION; NUCLEUS; EVOLUTION; SHOWER; DUST AB The cometary meteoroid ejection model of Jones and Brown [Physics, Chemistry, and Dynamics of Interplanetary Dust, ASP Conference Series 104 (1996b) 137] was used to simulate ejection from comets 55P/Tempel-Tuttle during the last 12 revolutions, and the last 9 apparitions of 109P/Swift-Tuttle. Using cometary ephemerides generated by the Jet Propulsion Laboratory's (JPL) HORIZONS Solar System Data and Ephemeris Computation Service, two independent ejection schemes were simulated. In the first case, ejection was simulated in 1 h time steps along the comet's orbit while it was within 2.5 AU of the Sun. In the second case, ejection was simulated to occur at the hour the comet reached perihelion. A 4th order variable step-size Runge-Kutta integrator was then used to integrate meteoroid position and velocity forward in time, accounting for the effects of radiation pressure, Poynting-Robertson drag, and the gravitational forces of the planets, which were computed using JPL's DE406 planetary ephemerides. An impact parameter (IP) was computed for each particle approaching the Earth to create a flux profile, and the results compared to observations of the 1998 and 1999 Leonid showers, and the 1993 and 2004 Perseids. C1 NASA, UNITeS, Morgan Res Corp, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Moser, DE (reprint author), NASA, UNITeS, Morgan Res Corp, George C Marshall Space Flight Ctr, Bldg 4487,EV13, Huntsville, AL 35812 USA. NR 28 TC 1 Z9 1 U1 0 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0167-9295 J9 EARTH MOON PLANETS JI Earth Moon Planets PD DEC PY 2005 VL 95 IS 1-4 BP 141 EP 153 DI 10.1007/s11038-005-3185-7 PG 13 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA 022VF UT WOS:000236083500017 ER PT J AU Jenniskens, P Wercinski, P Olejniczak, J Raiche, G Kontinos, D Allen, G Desai, PN Revelle, D Hatton, J Baker, RL Russell, RW Taylor, M Rietmeijer, F AF Jenniskens, P Wercinski, P Olejniczak, J Raiche, G Kontinos, D Allen, G Desai, PN Revelle, D Hatton, J Baker, RL Russell, RW Taylor, M Rietmeijer, F TI Preparing for hyperseed MAC: An observing campaign to monitor the entry of the Genesis Sample Return Capsule SO EARTH MOON AND PLANETS LA English DT Article; Proceedings Paper CT Meteoroids 2004 Conference CY AUG 16-20, 2004 CL Univ Western Ontario, London, ENGLAND SP Gerenc Seguridad Ind & Protecc Ambiental RMNE, PEMEX Explorac Producc HO Univ Western Ontario DE astrobiology; fireball; Genesis; meteor; reentry; sample return capsule; thermal protection system AB The return of the Genesis Sample Return Capsule ( SRC) from the Earth's L1 point on September 8, 2004, represents the first opportunity since the Apollo era to study the atmospheric entry of a meter-sized body at or above the Earth's escape speed. Until now, reentry heating models are based on only one successful reentry with an instrumented vehicle at higher than escape speed, the 22 May 1965 NASA "FIRE 2'' experiment. In preparation of an instrumented airborne and ground-based observing campaign, we examined the expected bolide radiation for the reentry of the Genesis SRC. We find that the expected emission spectrum consists mostly of blackbody emission from the SRC surface ( T similar to 2630 K@ peak heating), slightly skewed in shape because of a range of surface temperatures. At high enough spectral resolution, shock emission from nitrogen and oxygen atoms, as well as the first positive and first negative bands of N-2(+), will stand out above this continuum. Carbon atom lines and the 389-nm CN band emission may also be detected, as well as the mid-IR 4.6-mu m CO band. The ablation rate can be studied from the signature of trace sodium in the heat shield material, calibrated by the total amount of matter lost from the recovered shield. A pristine collection of the heat shield would also permit the sampling of products of ablation. C1 SETI Inst, Mountain View, CA 94043 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. ELORET Inst, Sunnyvale, CA USA. NASA, Langley Res Ctr, Hampton, VA 23665 USA. Los Alamos Natl Lab, Los Alamos, NM USA. Univ Calif San Francisco, San Francisco, CA 94143 USA. Aerosp Corp, El Segundo, CA USA. Utah State Univ, Logan, UT 84322 USA. Univ New Mexico, Albuquerque, NM 87131 USA. RP Jenniskens, P (reprint author), SETI Inst, 515 N Whisman Rd, Mountain View, CA 94043 USA. EM pjenniskens@mail.arc.nasa.gov NR 12 TC 12 Z9 12 U1 0 U2 3 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0167-9295 J9 EARTH MOON PLANETS JI Earth Moon Planets PD DEC PY 2005 VL 95 IS 1-4 BP 339 EP 360 DI 10.1007/s11038-005-9021-2 PG 22 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA 022VF UT WOS:000236083500035 ER PT J AU Swift, WR Suggs, RM Cooke, WJ AF Swift, WR Suggs, RM Cooke, WJ TI Meteor44 video meteor photometry SO EARTH MOON AND PLANETS LA English DT Article; Proceedings Paper CT Meteoroids 2004 Conference CY AUG 16-20, 2004 CL Univ Western Ontario, London, ENGLAND HO Univ Western Ontario DE meteor; video photometry; leonids; video calibration AB Meteor44 is a software system developed at MSFC for the calibration and analysis of video meteor data. The photometric range of the (8 bit) video data is extended from a visual magnitude range of from 8 to 3 to from 8 to -8 for both meteors and stellar images using saturation compensation. Camera and lens specific saturation compensation coefficients are derived from artificial variable star laboratory measurements. Saturation compensation significantly increases the number of meteors with measured intensity and improves the estimation of meteoroid mass distribution. Astrometry is automated to determine each image's plate coefficient using appropriate star catalogs. The images are simultaneously intensity calibrated from the contained stars to determine the photon sensitivity and the saturation level referenced above the atmosphere. The camera's spectral response is used to compensate for stellar color index and typical meteor spectra in order to report meteor light curves in traditional visual magnitude units. Recent efforts include improved camera calibration procedures and long focal length "streak" meteor photometry. Meteor44 has been used to analyze data from the 2001, 2002 and 2003 MSFC Leonid observational campaigns as well as several lesser showers. C1 NASA, Raytheon MSFC Grp, Space Environm Team, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. RP Swift, WR (reprint author), NASA, Raytheon MSFC Grp, Space Environm Team, George C Marshall Space Flight Ctr, EV13, Huntsville, AL 35812 USA. EM rob.suggs@nasa.com NR 7 TC 2 Z9 2 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0167-9295 J9 EARTH MOON PLANETS JI Earth Moon Planets PD DEC PY 2005 VL 95 IS 1-4 BP 533 EP 540 DI 10.1007/s11038-005-1639-6 PG 8 WC Astronomy & Astrophysics; Geosciences, Multidisciplinary SC Astronomy & Astrophysics; Geology GA 022VF UT WOS:000236083500050 ER PT J AU Ramsey, BD AF Ramsey, Brian D. TI Replicated nickel optics for the hard-x-ray region SO EXPERIMENTAL ASTRONOMY LA English DT Article; Proceedings Paper CT Workshop on Focusing Telescopes in Nuclear Astrophysics CY SEP 12-15, 2005 CL Bonifacio, FRANCE DE replicated; X-ray astronomy; x-ray optics AB Replicated nickel optics has been used extensively in x-ray astronomy, most notably for the XMM/Newton mission. The combination of relative ease of fabrication and the inherent stability of full-shell optics, make them an attractive approach for medium-resolution, high-throughput applications. MSFC has been developing these optics for use in the hard-x-ray region. Efforts at improving their angular resolution, particularly for the very-thin-wall shells required to meet the weight budgets of future missions, are described together with the prospects for future significant improvements. 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@nasa.gov NR 3 TC 15 Z9 15 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0922-6435 J9 EXP ASTRON JI Exp. Astron. PD DEC PY 2005 VL 20 IS 1-3 BP 85 EP 92 DI 10.1007/s10686-006-9033-6 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 126RD UT WOS:000243531600011 ER PT J AU Tueller, J Krimm, HA Okajima, T Barthelmy, SD Owens, SM Serlemitsos, PJ Soong, Y Chan, KW Ogasaka, Y Shibata, R Tamura, K Furuzawa, A Tawara, Y Kunieda, H Yamashita, K AF Tueller, J. Krimm, H. A. Okajima, T. Barthelmy, S. D. Owens, S. M. Serlemitsos, P. J. Soong, Y. Chan, K. -W. Ogasaka, Y. Shibata, R. Tamura, K. Furuzawa, A. Tawara, Y. Kunieda, H. Yamashita, K. TI InFOC mu S hard X-ray imaging telescope SO EXPERIMENTAL ASTRONOMY LA English DT Article; Proceedings Paper CT Workshop on Focusing Telescopes in Nuclear Astrophysics CY SEP 12-15, 2005 CL Bonifacio, FRANCE DE hard X-rays; multilayer mirror; CdZnTe pixellated detector; balloon experiments; background AB InFOC mu S is a new generation balloon-borne hard X-ray telescope with focusing optics and spectroscopy. We had a successful 22.5-hour flight from Fort Sumner, NM on September 16,17, 2004. In this paper, we present the performance of the hard X-ray telescope, which consists of a depth-graded platinum/carbon multilayer mirror and a CdZnTe detector. The telescope has an effective area of 49 cm(2) at 30 keV, an angular resolution of 2.4 arcmin (HPD), and a field of view of 11 arcmin (FWHM) depending on energies. The CdZnTe detector is configured with a 12 x 12 segmented array of detector pixels. The pixels are 2 mm square, and are placed on 2.1 mm centers. An averaged energy resolution is 4.4 keV at 60 keV and its standard deviation is 0.36 keV over 128 pixels. The detector is surrounded by a 3-cm thick CsI anti coincidence shield to reduce background from particles and photons not incident along the mirror focal direction. The inflight background is 2.9 x 10(-4) cts cm(-2) sec(-1) keV(-1) in the 20-50 keV band. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20711 USA. Nagoya Univ, Chikusa Ku, Nagoya, Aichi 4648602, Japan. RP Okajima, T (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20711 USA. EM okajima@milkyway.gsfc.nasa.gov RI Barthelmy, Scott/D-2943-2012; Tueller, Jack/D-5334-2012 NR 5 TC 10 Z9 10 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0922-6435 J9 EXP ASTRON JI Exp. Astron. PD DEC PY 2005 VL 20 IS 1-3 BP 121 EP 129 DI 10.1007/s10686-006-9028-3 PG 9 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 126RD UT WOS:000243531600015 ER PT J AU Krizmanic, J Morgan, B Streitmatter, R Gehrels, N Gendreau, K Arzoumanian, Z Ghodssi, R Skinner, G AF Krizmanic, John Morgan, Brian Streitmatter, Robert Gehrels, Neil Gendreau, Keith Arzoumanian, Zaven Ghodssi, Reza Skinner, Gerry TI Development of ground-testable phase fresnel lenses in silicon SO EXPERIMENTAL ASTRONOMY LA English DT Article; Proceedings Paper CT Workshop on Focusing Telescopes in Nuclear Astrophysics CY SEP 12-15, 2005 CL Bonifacio, FRANCE DE X-ray astronomy; gamma-ray astronomy; optics ID HIGH-ENERGY ASTRONOMY; OPTICS AB Diffractive optics, such as Phase Fresnel Lenses (PFL's), offer the potential to achieve excellent imaging performance in the x-ray and gamma-ray photon regimes. In principle, the angular resolution obtained with these devices can be diffraction limited. Furthermore, improvements in signal sensitivity can be achieved as virtually the entire flux incident on a lens can be concentrated onto a small detector area. In order to verify experimentally the imaging performance, we have fabricated PFL's in silicon using gray-scale lithography to produce the required Fresnel profile. These devices are to be evaluated in the recently constructed 600-meter x-ray interferometry testbed at NASA/GSFC. Profile measurements of the Fresnel structures in fabricated PFL's have been performed and have been used to obtain initial characterization of the expected PFL imaging efficiencies. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Maryland, Dept Elect & Comp Engn, College Pk, MD 20742 USA. CESR, F-31028 Toulouse, France. EM jfk@cosmicra.gsfc.nasa.gov RI Gehrels, Neil/D-2971-2012 NR 8 TC 6 Z9 6 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0922-6435 J9 EXP ASTRON JI Exp. Astron. PD DEC PY 2005 VL 20 IS 1-3 BP 299 EP 306 DI 10.1007/s10686-006-9030-9 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 126RD UT WOS:000243531600031 ER PT J AU Freyberg, MJ Brauninger, H Burkert, W Hartner, GD Citterio, O Mazzoleni, F Pareschi, G Spiga, D Romaine, S Gorenstein, P Ramsey, BD AF Freyberg, M. J. Braeuninger, H. Burkert, W. Hartner, G. D. Citterio, O. Mazzoleni, F. Pareschi, G. Spiga, D. Romaine, S. Gorenstein, P. Ramsey, B. D. TI The MPE X-ray test facility PANTER: Calibration of hard X-ray (15-50 kev) optics SO EXPERIMENTAL ASTRONOMY LA English DT Article; Proceedings Paper CT Workshop on Focusing Telescopes in Nuclear Astrophysics CY SEP 12-15, 2005 CL Bonifacio, FRANCE DE X-ray astronomy; X-ray telescopes; X-ray optics; X-ray detectors; multilayers; calibration ID XMM-NEWTON; PERFORMANCE; ASTRONOMY; DESIGN; TELESCOPES; ROSAT AB The Max-Planck-Institut fur extraterrestrische Physik (MPE) in Garching, Get-many, uses its large X-ray beam line facility PANTER for testing X-ray astronomical instrumentation. A number of telescopes, gratings, filters, and detectors, e.g. for astronomical satellite missions like Exosat, ROSAT, Chandra (LETG), BeppoSAX, SOHO (CDS), XMM-Newton, ABRIXAS, Swift (XRT), have been successfully calibrated in the soft X-ray energy range (< 15keV). Moreover, measurements with mirror test samples for new missions like ROSITA and XEUS have been carried out at PANTER. Here we report on an extension of the energy range, enabling calibrations of hard X-ray optics over the energy range 15-50 keV. Several future X-ray astronomy missions (e.g., Simbol-X, Constellation-X, XEUS) have been proposed, which make use of hard X-ray optics based on multilayer coatings. Such optics are currently being developed by the Osservatorio Astronomico di Brera (OAB), Milano. Italy, and the Harvard-Smithsonian Center for Astrophysics (CIA), Cambridge, MA, USA. These optics have been tested at the PANTER facility with a broad energy band beam (up to 50 keV) using the XMM-Newton EPIC-pn flight spare CCD camera with its good intrinsic energy resolution, and also with monochromatic X-rays between C-K (0.277 keV) and Cu-K alpha (8.04 keV). C1 Max Planck Inst Extraterr Phys, PANTER Xray Test Facil, D-82061 Neuried, Germany. INAF, Osservatorio Astron Brera, I-23807 Merate, Italy. Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA. NASA, MSFC, Dept Space Sci, Huntsville, AL 35812 USA. RP Freyberg, MJ (reprint author), Max Planck Inst Extraterr Phys, PANTER Xray Test Facil, Gautinger Str 45, D-82061 Neuried, Germany. EM mjf@mpe.mpg.de OI Spiga, Daniele/0000-0003-1163-7843; Pareschi, Giovanni/0000-0003-3967-403X NR 16 TC 1 Z9 1 U1 1 U2 2 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0922-6435 J9 EXP ASTRON JI Exp. Astron. PD DEC PY 2005 VL 20 IS 1-3 BP 407 EP 414 DI 10.1007/s10686-006-9068-8 PG 8 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 126RD UT WOS:000243531600041 ER PT J AU Krizmanic, J Skinner, G Gehrels, N AF Krizmanic, John Skinner, Gerry Gehrels, Neil TI Formation flying for a Fresnel lens observatory mission SO EXPERIMENTAL ASTRONOMY LA English DT Article; Proceedings Paper CT Workshop on Focusing Telescopes in Nuclear Astrophysics CY SEP 12-15, 2005 CL Bonifacio, FRANCE DE gamma-ray astronomy; optics; formation flying ID TELESCOPE AB The employment of a large area Phase Fresnel Lens (PFL) in a gamma-ray telescope offers the potential to image astrophysical phenomena with micro-arcsecond (mu '') angular resolution [1]. In order to assess the feasibility of this concept, two detailed studies have been conducted of formation flying missions in which a Fresnel lens capable of focussing gamma-rays and the associated detector are carried on two spacecraft separated by up to 10(6) km. These studies were performed at the NASA Goddard Space Flight Center Integrated Mission Design Center (IMDC) which developed spacecraft, orbital dynamics, and mission profiles. The results of the studies indicated that the missions are challenging but could be accomplished with technologies available currently or in the near term. The findings of the original studies have been updated taking account of recent advances in ion thruster propulsion technology. C1 NASA, Goddard Space Flight Ctr, Univ Space Res Assoc, Greenbelt, MD 20771 USA. CESR, F-31028 Toulouse, France. RP Krizmanic, J (reprint author), NASA, Goddard Space Flight Ctr, Univ Space Res Assoc, Code 661, Greenbelt, MD 20771 USA. EM jfk@cosmicra.gsfc.nasa.gov RI Gehrels, Neil/D-2971-2012 NR 3 TC 2 Z9 2 U1 0 U2 1 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0922-6435 J9 EXP ASTRON JI Exp. Astron. PD DEC PY 2005 VL 20 IS 1-3 BP 499 EP 505 DI 10.1007/s10686-006-9038-1 PG 7 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 126RD UT WOS:000243531600049 ER PT J AU Chasiotis, I Chen, Q Odegard, GM Gates, TS AF Chasiotis, I Chen, Q Odegard, GM Gates, TS TI Structure-property relationships in polymer composites with micrometer and submicrometer graphite platelets SO EXPERIMENTAL MECHANICS LA English DT Article DE polymer composites; graphite platelets; mechanical properties; local properties; nanoindentation ID NANOINDENTATION; NANOCOMPOSITES; INDENTATION AB The objectives of this work were (a) to investigate the influence of micrometer and submicrometer scale graphite platelets of different aspect ratios and volume fractions on the effective and local quasi-static and dynamic properties of composites with micrometer and submicrometer scale reinforcement, and (b) to compare and evaluate mechanical property measurements of inhomogeneous materials via local (microscale) and bulk (macroscale) experimental methods. Small platelet volume fractions (0.5%) provided proportionally larger increase of the elastic and storage moduli compared to large volume fractions (3.0%). Randomly distributed 15 mu m platelets provided marginally higher composite stiffness compared to 1 mu m platelets while small volume fractions (0.5%) of 15 mu m platelets had a pronounced effect on the effective Poisson's ratio. It was found that local property measurements of inhomogeneous materials conducted by nanoindentation are not representative of the bulk behavior even when the characteristic length of the inhomogeneity is an order of magnitude smaller than the indentation contact area. In this case, statistical averaging of data from a large number of indentations does not result in agreement with bulk measurements. On the other hand, for small aspect ratio platelets with dimensions two orders of magnitude smaller than the nanoindentation contact area, the nanoindenter-obtained properties agreed well with the effective material behavior. It was found that platelets residing at the specimen surface contribute the most to nanoindentation data, which implies that this technique is only valid for well-distributed nanoparticulate and microparticulate systems, and that nanoindentation cannot be used for depth profiling of microstructured composites. C1 Univ Illinois, Urbana, IL 61801 USA. Michigan Technol Univ, Houghton, MI 49931 USA. NASA, Langley Res Ctr, Durabil Branch, Hampton, VA 23681 USA. RP Chasiotis, I (reprint author), Univ Illinois, Urbana, IL 61801 USA. EM chasioto@uiuc.edu OI Odegard, Gregory/0000-0001-7577-6565 NR 16 TC 24 Z9 24 U1 1 U2 11 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 0014-4851 J9 EXP MECH JI Exp. Mech. PD DEC PY 2005 VL 45 IS 6 BP 507 EP 516 DI 10.1177/0014485105059992 PG 10 WC Materials Science, Multidisciplinary; Mechanics; Materials Science, Characterization & Testing SC Materials Science; Mechanics GA 986NS UT WOS:000233457600004 ER PT J AU O'Reilly, SE Watkins, J Furukawa, Y AF O'Reilly, SE Watkins, J Furukawa, Y TI Secondary mineral formation associated with respiration of nontronite, NAu-1 by iron reducing bacteria SO GEOCHEMICAL TRANSACTIONS LA English DT Article ID SALT-MARSH SEDIMENTS; TRANSMISSION ELECTRON-MICROSCOPY; CONTINENTAL-MARGIN SEDIMENTS; ORGANIC-CARBON OXIDATION; FE(III) OXIDE REDUCTION; SHEWANELLA-PUTREFACIENS; STRUCTURAL FE(III); MARINE-SEDIMENTS; CLAY-MINERALS; MANGANESE REDUCTION AB Experimental batch and miscible-flow cultures were studied in order to determine the mechanistic pathways of microbial Fe(III) respiration in ferruginous smectite clay, NAu-1. The primary purpose was to resolve if alteration of smectite and release of Fe precedes microbial respiration. Alteration of NAu-1, represented by the morphological and mineralogical changes, occurred regardless of the extent of microbial Fe(III) reduction in all of our experimental systems, including those that contained heat-killed bacteria and those in which O-2, rather than Fe(III), was the primary terminal electron acceptor. The solid alteration products observed under transmission electron microscopy included poorly crystalline smectite with diffuse electron diffraction signals, discrete grains of Fe-free amorphous aluminosilicate with increased Al/Si ratio, Fe-rich grains, and amorphous Si globules in the immediate vicinity of bacterial cells and extracellular polymeric substances. In reducing systems, Fe was also found as siderite. The small amount of Fe partitioned to the aqueous phase was primarily in the form of dissolved Fe(III) species even in the systems in which Fe(III) was the primary terminal electron acceptor for microbial respiration. From these observations, we conclude that microbial respiration of Fe(III) in our laboratory systems proceeded through the following: (1) alteration of NAu-1 and concurrent release of Fe(III) from the octahedral sheets of NAu-1; and (2) subsequent microbial respiration of Fe(III). (C) 2005 American Institute of Physics. C1 USN, Res Lab, Seafloor Sci Branch, Stennis Space Ctr, Stennis Space Ctr, MS 39529 USA. RP Furukawa, Y (reprint author), USN, Res Lab, Seafloor Sci Branch, Stennis Space Ctr, Stennis Space Ctr, MS 39529 USA. EM yoko.furukawa@nrlssc.navy.mil RI Furukawa, Yoko/B-3099-2013 NR 59 TC 28 Z9 30 U1 2 U2 22 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 1467-4866 J9 GEOCHEM T JI Geochem. Trans. PD DEC PY 2005 VL 6 IS 4 BP 67 EP 76 DI 10.1063/1.2084787 PG 10 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 998UV UT WOS:000234346300001 ER PT J AU Potter, C Klooster, S Tan, P Steinbach, M Kumar, V Genovese, V AF Potter, C Klooster, S Tan, P Steinbach, M Kumar, V Genovese, V TI Variability in terrestrial carbon sinks over two decades: Part 2 - Eurasia SO GLOBAL AND PLANETARY CHANGE LA English DT Article DE carbon; ecosystems; remote sensing; soil ID NET PRIMARY PRODUCTION; SATELLITE DATA; GLOBAL SATELLITE; DIOXIDE FLUXES; SCALE; EXCHANGE; FORESTS; CLIMATE; MODEL; ECOSYSTEMS AB We have analyzed 17 yr (1982-1998) of net carbon flux predictions from a simulation model based on satellite observations of monthly vegetation cover. The NASA-CASA model was driven by vegetation cover properties derived from the Advanced Very High Resolution Radiometer and radiative transter algorithms that were developed for the Moderate Resolution Imaging Spectroradionicter (MODIS). We report that although the terrestrial ecosystem sink for atmospheric CO2 for the Eurasian region has been fairly consistent at between 0.3 and 0.6 Pg C per year since 1988, high interannual variability in net ecosystem production (NEP) fluxes can be readily identified at locations across the continent. Ten major areas of highest variability in NEP were detected: eastern Europe, the Iberian Peninsula, the Balkan states, Scandinavia, northern and western Russia, eastern Siberia, Mongolia and western China, and central India. Analysis of climate anomalies over this 17-yr time period suggests that variability in precipitation and surface solar irradiance could be associated with trends in carbon sink fluxes within such regions of high NEP variability. (c) 2005 Elsevier B.V. All rights reserved. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Calif State Univ, Seaside, CA USA. Univ Minnesota, Minneapolis, MN USA. RP Potter, C (reprint author), NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. EM cpotter@mail.arc.nasa.gov NR 30 TC 18 Z9 21 U1 0 U2 9 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0921-8181 J9 GLOBAL PLANET CHANGE JI Glob. Planet. Change PD DEC PY 2005 VL 49 IS 3-4 BP 177 EP 186 DI 10.1016/j.gloplacha.2005.07.002 PG 10 WC Geography, Physical; Geosciences, Multidisciplinary SC Physical Geography; Geology GA 000LV UT WOS:000234464400003 ER PT J AU Herrmann, SM Anyamba, A Tucker, CJ AF Herrmann, SM Anyamba, A Tucker, CJ TI Recent trends in vegetation dynamics in the African Sahel and their relationship to climate SO GLOBAL ENVIRONMENTAL CHANGE-HUMAN AND POLICY DIMENSIONS LA English DT Article DE desertification; greening; Sahel; remote sensing; time series analysis ID DENSITY GAUGE DATASET; WEST-AFRICA; SAHARA DESERT; BURKINA-FASO; NOAA-AVHRR; RAINFALL; DESERTIFICATION; SATELLITE; INDEX; TRMM AB Contrary to assertions of widespread irreversible desertification in the African Sahel, a recent increase in seasonal greenness over large areas of the Sahel has been observed, which has been interpreted as a recovery from the great Sahelian droughts. This research investigates temporal and spatial patterns of vegetation greenness and rainfall variability in the African Sahel and their interrelationships based on analyses of Normalized Difference Vegetation Index (NDVI) time series for the period 1982-2003 and gridded satellite rainfall estimates. While rainfall emerges as the dominant causative factor for the increase in vegetation greenness, there is evidence of another causative factor, hypothetically a human-induced change superimposed on the climate trend. (c) 2005 Elsevier Ltd. All rights reserved. C1 Univ Arizona, Off Arid Land Studies, Tucson, AZ 85719 USA. Univ Maryland Baltimore Cty, Goddard Earth Sci Technol Ctr, Baltimore, MD 21228 USA. NASA, Goddard Space Flight Ctr, Biospher Sci Branch, Greenbelt, MD 20771 USA. RP Herrmann, SM (reprint author), Univ Arizona, Off Arid Land Studies, 1955 E 6th St, Tucson, AZ 85719 USA. EM stefanie@ag.arizona.edu; assaf@ltpmailx.gsfc.nasa.gov; compton@ltpmailx.gsfc.nasa.gov NR 73 TC 286 Z9 321 U1 24 U2 158 PU ELSEVIER SCI LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, OXON, ENGLAND SN 0959-3780 J9 GLOBAL ENVIRON CHANG JI Glob. Environ. Change-Human Policy Dimens. PD DEC PY 2005 VL 15 IS 4 BP 394 EP 404 DI 10.1016/j.gloenvcha.2005.08.004 PG 11 WC Environmental Sciences; Environmental Studies; Geography SC Environmental Sciences & Ecology; Geography GA 988TG UT WOS:000233623200010 ER PT J AU Tigelaar, DM Klein, DJ Xu, TB Su, J Bryant, RG AF Tigelaar, DM Klein, DJ Xu, TB Su, J Bryant, RG TI Synthesis and characterization of poly(pyridinium triflate)s with alkyl and aromatic spacer groups for potential use as nonlinear optic materials SO HIGH PERFORMANCE POLYMERS LA English DT Article DE poly(pyridinium triflate)s; accordion polymers; ionomers; nonlinear optic polymers ID POLYMERS; SALT)S; FILMS AB A series of poly(pyridinium triflate)s with alkyl and aromatic spacer groups were prepared by ring transformation polymerizations between various pyrylium triflates and diamines. The polymers are soluble in polar aprotic solvents and form tough, clear, flexible films. These novel polymers were characterized by IR, NMR, UV, DSC, TMA, and TGA. The polymers were thermally stable to 340 C under nitrogen, and had softening points that ranged from 151 to 255 degrees C. Thin films were shown to display electrostrictive behavior in the presence of an applied electric field, with the amount of transverse strain being proportional to the concentration of charge in the polymer. C1 NASA, Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA. RP Tigelaar, DM (reprint author), NASA, Langley Res Ctr, Adv Mat & Proc Branch, Hampton, VA 23681 USA. EM Dean.tigelaar@grc.nasa.gov NR 33 TC 3 Z9 3 U1 1 U2 3 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 0954-0083 J9 HIGH PERFORM POLYM JI High Perform. Polym. PD DEC PY 2005 VL 17 IS 4 BP 515 EP 531 DI 10.1177/0954008305050676 PG 17 WC Polymer Science SC Polymer Science GA 987UX UT WOS:000233544000004 ER PT J AU Devasahayam, S Hill, DJT AF Devasahayam, S Hill, DJT TI Effect of electron beam radiolysis on mechanical properties of high performance polyimides. A comparative study of transparent polymer films SO HIGH PERFORMANCE POLYMERS LA English DT Article DE polymer materials; transparent polyimides; e-beam radiolysis; tensile properties; optical properties ID CROSS-LINKING; TEMPERATURE-DEPENDENCE; RADIATION-RESISTANCE; AROMATIC POLYMERS; GAS EVOLUTION; POLYETHYLENE; IRRADIATION; DEGRADATION; CHEMISTRY; ACID AB The mechanical properties of four optically transparent polyimides prepared from the dianhydrides ODPA and 6FDA and the diamines ODA and DAB were assessed. The property changes when these polymers are subjected to high-energy electron-beam irradiation (1 MeV) for doses up to 18.5 MGy and temperatures up to 523 K were also studied and compared. The corresponding changes on radiolysis of Kapton are reported for comparison with the other polymers. The tensile properties of the four polyimides differed mainly by the nature of the dianhydride, with the ODPA polymers undergoing necking and cold drawing and the 6FDA polymers brittle fracture. The four polyimides were synthesized with the objective of obtaining optimum transparency for space applications where high-energy radiation doses of 15-20 MGy may be expected in geosynchronous orbits over a life span of 20 years. The polyimides were shown to maintain good optical and tensile properties at temperatures up to about 450 K for a dose of 18.5 MGy, but above this temperature the moduli of the polymers began to deteriorate and there was a small decrease in the transmittance of the exposed polymer films. C1 Univ Sydney, Sch Chem, Key Ctr Polymer Colloids, Sydney, NSW 2006, Australia. Univ Queensland, Dept Chem, Polymer Mat & Radiat Grp, Brisbane, Qld 4072, Australia. NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Hill, DJT (reprint author), Univ Sydney, Sch Chem, Key Ctr Polymer Colloids, Sydney, NSW 2006, Australia. EM d.hill@uq.edu.au NR 29 TC 6 Z9 6 U1 0 U2 16 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 0954-0083 J9 HIGH PERFORM POLYM JI High Perform. Polym. PD DEC PY 2005 VL 17 IS 4 BP 547 EP 559 DI 10.1177/0954008305051662 PG 13 WC Polymer Science SC Polymer Science GA 987UX UT WOS:000233544000006 ER PT J AU Kaber, DB Wright, MC Prinzel, LJ Clamann, MP AF Kaber, DB Wright, MC Prinzel, LJ Clamann, MP TI Adaptive automation of human-machine system information-processing functions SO HUMAN FACTORS LA English DT Article ID PERFORMANCE; ALLOCATION; MODEL; TASK AB The goal of this research was to describe the ability of human operators to interact with adaptive automation (AA) applied to various stages of complex systems information processing, defined in a model of human-automation interaction. Forty participants operated a simulation of an air traffic control task. Automated assistance was adaptively applied to information acquisition, information analysis, decision making, and action implementation aspects of the task based on operator workload states, which were measured using a secondary task. The differential effects of the forms of automation were determined and compared with a manual control condition. Results of two 20-min trials of AA or manual control revealed a significant effect of the type of automation on performance, particularly during manual control periods as part of the adaptive conditions. Humans appear to better adapt to AA applied to sensory and psychomotor information-processing functions (action implementation) than to AA applied to cognitive functions (information analysis and decision making), and AA is superior to completely manual control. Potential applications of this research include the design of automation to support air traffic controller information processing. C1 N Carolina State Univ, Dept Ind Engn, Raleigh, NC 27695 USA. Duke Univ, Med Ctr, Durham, NC 27706 USA. NASA, Langley Res Ctr, Hampton, VA 23665 USA. Micro Anal & Design, Boulder, CO USA. RP Kaber, DB (reprint author), N Carolina State Univ, Dept Ind Engn, 328 Riddick Labs, Raleigh, NC 27695 USA. EM dbkaber@ncsu.edu OI Wright, Melanie/0000-0001-7121-504X NR 28 TC 36 Z9 36 U1 1 U2 3 PU HUMAN FACTORS SOC PI SANTA MONICA PA BOX 1369, SANTA MONICA, CA 90406 USA SN 0018-7208 J9 HUM FACTORS JI Hum. Factors PD WIN PY 2005 VL 47 IS 4 BP 730 EP 741 DI 10.1518/001872005775570989 PG 12 WC Behavioral Sciences; Engineering, Industrial; Ergonomics; Psychology, Applied; Psychology SC Behavioral Sciences; Engineering; Psychology GA 013PY UT WOS:000235422600004 PM 16553062 ER PT J AU Beyer, RA McEwen, AS AF Beyer, RA McEwen, AS TI Layering stratigraphy of eastern Coprates and northern Capri Chasmata, Mars SO ICARUS LA English DT Article DE geological processes; geophysics; image processing; Mars; surface; surfaces; planets; tectonics; terrestrial planets; volcanism ID VALLES-MARINERIS; ORBITER CAMERA; ALBA-PATERA; LAVA FLOWS; TERRESTRIAL; EMPLACEMENT; TOPOGRAPHY; EVOLUTION; VOLCANISM; MODELS AB Distinct competent layers are observed in the slopes of eastern Coprates Chasma, part of the Valles Marineris system on Mars. Our observations indicate that the stratigraphy of Coprates Chasma consists of alternating thin strong layers and thicker sequences of relatively weak layers. The strong, competent layers maintain steeper slopes and play a major role in controlling the overall shape and geomorphology of the chasmata slopes. The topmost competent layer in this area is well preserved and easy to identify in outcrops on the northern rim of Coprates Chasma less than 100 m below the southern Ophir Planum surface. The volume of the topmost emplaced layer is at least 70 km(3) and may be greater than 2100 km(3) if the unit underlies most of Ophir Planum. The broad extent of this layer allows us to measure elevation offsets within the. north rim of the chasma and in a freestanding massif within Coprates Chasma where the layer is also observed. Rim outcrop morphology and elevation differences between Ophir and Aurorae Plana may be indicative of the easternmost extent of the topmost competent layer. These observations allow an insight into the depositional processes that formed the stratigraphic stack into which this portion of the Valles Marineris is carved, and they present a picture of some of the last volcanic activity in this area. Furthermore, the elevation offsets within the layer are evidence of significant subsidence of the massif and surrounding material. (c) 2005 Ross Beyer. Published by Elsevier Inc. All rights reserved. C1 Univ Arizona, Dept Planetary Sci, Tucson, AZ 85721 USA. RP Beyer, RA (reprint author), NASA, Ames Res Ctr, MS 245-3, Moffett Field, CA 94035 USA. EM rbeyer@arc.nasa.gov; mcewen@lpl.arizona.edu OI Beyer, Ross/0000-0003-4503-3335 NR 60 TC 29 Z9 29 U1 0 U2 6 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 EI 1090-2643 J9 ICARUS JI Icarus PD DEC 1 PY 2005 VL 179 IS 1 BP 1 EP 23 DI 10.1016/j.icarus.2005.06.014 PG 23 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 987XI UT WOS:000233550600001 ER PT J AU Vokrouhlicky, D Capek, D Chesley, SR Ostro, SJ AF Vokrouhlicky, D Capek, D Chesley, SR Ostro, SJ TI Yarkovsky detection opportunities - II. Binary systems SO ICARUS LA English DT Article DE asteroids; Yarkovsky effect; orbit determination ID NEAR-EARTH ASTEROIDS; NONLINEARIZED THEORY; FRAGMENTS; SATELLITES; STABILITY AB We consider the possibility of detecting the Yarkovsky orbital perturbation acting on binary systems among the near-Earth asteroids. This task is significantly more difficult than for solitary asteroids because the Yarkovsky force affects both the heliocentric orbit of the system's center of mass and the relative orbit of the two components. Nevertheless, we argue these are sufficiently well decoupled so that the major Yarkovsky perturbation is in the simpler heliocentric motion and is observable with the current means of radar astrometry. Over the long term, the Yarkovsky perturbation in the relative motion of the two components is also detectable for the best observed systems. However, here we consider a simplified version of the problem by ignoring mutual non-spherical gravitational perturbations between the two asteroids. With the orbital plane constant in space and the components' rotation poles fixed (and assumed perpendicular to the orbital plane), we do not examine the coupling between Yarkovsky and gravitational effects. While radar observations remain an essential element of Yarkovsky detections, lightcurve observations, with their ability to track occultation and eclipse phenomena, are also very important in the case of binaries. The nearest possible future detection of the Yarkovsky effect for a binary system occurs for (66063) 1998 RO1 in September 2006. Farther out, even more statistically significant detections are possible for several other systems including 2000 DP107, (66391) 1999 KW4 and 1996 FG(3). Published by Elsevier Inc. C1 Charles Univ, Inst Astron, CZ-18000 Prague, Czech Republic. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Vokrouhlicky, D (reprint author), Charles Univ, Inst Astron, V Holesovickach 2, CZ-18000 Prague, Czech Republic. EM vokrouhl@mbox.cesnet.cz; capek@sirrah.troja.mff.cuni.cz; steve.chesley@jpl.nasa.gov; ostro@reason.jpl.nasa.gov RI Capek, David/G-9005-2014 NR 27 TC 9 Z9 9 U1 0 U2 1 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD DEC 1 PY 2005 VL 179 IS 1 BP 128 EP 138 DI 10.1016/j.icarus.2005.06.003 PG 11 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 987XI UT WOS:000233550600008 ER PT J AU Abell, PA Fernandez, YR Pravec, P French, LM Farnham, TL Gaffey, MJ Hardersen, PS Kusnirak, P Sarounova, L Sheppard, SS Narayan, G AF Abell, PA Fernandez, YR Pravec, P French, LM Farnham, TL Gaffey, MJ Hardersen, PS Kusnirak, P Sarounova, L Sheppard, SS Narayan, G TI Physical characteristics of Comet Nucleus C/2001 OG(108) (LONEOS) SO ICARUS LA English DT Review DE comets, composition; infrared observations; visible observations; comets, origin; near-earth asteroids, origin ID NEAR-EARTH ASTEROIDS; THERMAL-INFRARED SPECTROPHOTOMETRY; INTERPLANETARY DUST PARTICLES; TAGISH LAKE METEORITE; KUIPER-BELT; 1996 PW; REFLECTANCE SPECTROSCOPY; CARBONACEOUS CHONDRITE; DYNAMICAL EVOLUTION; SURFACE-COMPOSITION AB A detailed description of the Halley-type Comet C/2001 OG(108) (LONEOS) has been derived from visible, near-infrared, and mid-infrared observations obtained in October and November 2001. These data represent the first high-quality ground-based observations of a bare Halley-type comet nucleus and provide the best characterization of a Halley-type comet other than 1P/Halley itself. Analysis of time series photometry suggests that the nucleus has a rotation period of 57.2 +/- 0.5 h with a minimum nuclear axial ratio of 1.3, a phase-darkening slope parameter G of -0.01 +/- 0.10, and an estimated H = 13.05 +/- 0.10. The rotation period of C/2001 OG(108) is one of the longest observed among comet nuclei. The V-R color index for this object is measured to be 0.461 +/- 0.02, which is virtually identical to that of other cometary nuclei and other possible extinct comet candidates. Measurements of the comet's thermal emission constrain the projected elliptical nuclear radii to be 9.6 +/- 1.0 km and 7.4 +/- 1.0 km, which makes C/2001 OG(108) one of the larger cometary nuclei known. The derived geometric albedo in V-band of 0.040 +/- 0.010 is typical for comet nuclei. Visible-wavelength spectrophotometry and near-infrared spectroscopy were combined to derive the nucleus's reflectance spectrum over a 0.4 to 2.5 mu m wavelength range. These measurements represent one of the few nuclear spectra ever observed and the only known spectrum of a Halley-type comet. The spectrum of this comet nucleus is very nearly linear and shows no discernable absorption features at a 5% detection limit. The lack of any features, especially in the 0.8 to 1.0 mu m range such as are seen in the spectra of carbonaceous chondrite meteorites and many low-albedo asteroids, is consistent with the presence of anhydrous rather than hydrous silicates on the surface of this comet. None of the currently recognized meteorites in the terrestrial collections have reflectance spectra that match C/2001 OG(108). The near-infrared spectrum, the geometric albedo, and the visible spectrophotometry all indicate that C/2001 OG(108) has spectral properties analogous to the D-type, and possibly P-type asteroids. Comparison of the measured albedo and diameter of C/2001 OG(108) with those of Damocloid asteroids reveals similarities between these asteroids and this comet nucleus, a finding which supports previous dynamical arguments that Damocloid asteroids could be composed of cometary-like materials. These observations are also consistent with findings that two Jupiter-family comets may have spectral signatures indicative of D-type asteroids. C/2001 OG(108) probably represents the transition from a typical active comet to an extinct cometary nucleus, and, as a Halley-type comet, suggests that some comets originating in the Oort cloud can become extinct without disintegrating. As a near-Earth object, C/2001 OG(108) supports the suggestion that some fraction of the near-Earth asteroid population consists of extinct cometary nuclei. (c) 2005 Elsevier Inc. All rights reserved. C1 NASA, Lyndon B Johnson Space Ctr, Planetary Astron Grp, Houston, TX 77058 USA. Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA. Acad Sci Czech Republ, Inst Astron, CZ-25165 Ondrejov, Czech Republic. Illinois Wesleyan Univ, Dept Phys, Bloomington, IL 61702 USA. Univ Maryland, Dept Astron, College Pk, MD 20742 USA. Univ N Dakota, Dept Space Studies, Grand Forks, ND 58202 USA. Carnegie Inst Washington, Dept Terr Magnetism, Washington, DC 20015 USA. RP Abell, PA (reprint author), Univ Hawaii, Infrared Telescope Facil, Honolulu, HI 96822 USA. EM paul.a.abell1@jsc.nasa.gov RI Pravec, Petr/G-9037-2014; Hardersen, Paul/N-9343-2014; OI Hardersen, Paul/0000-0002-0440-9095; Fernandez, Yanga/0000-0003-1156-9721 NR 134 TC 28 Z9 28 U1 0 U2 1 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD DEC 1 PY 2005 VL 179 IS 1 BP 174 EP 194 DI 10.1016/j.icarus.2005.06.012 PG 21 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 987XI UT WOS:000233550600011 ER PT J AU Milazzo, MP Keszthelyi, LP Radebaugh, J Davies, AG Turtle, EP Geissler, P Klaasen, KP Rathbun, JA McEwen, AS AF Milazzo, MP Keszthelyi, LP Radebaugh, J Davies, AG Turtle, EP Geissler, P Klaasen, KP Rathbun, JA McEwen, AS TI Volcanic activity at Tvashtar Catena, Io SO ICARUS LA English DT Article DE Io; volcanism; surfaces; satellites; image processing ID INFRARED MAPPING SPECTROMETER; STATE IMAGING-SYSTEM; JUPITERS MOON IO; GALILEO MISSION; HEAT-FLOW; SILICATE VOLCANISM; THERMAL EMISSION; LAVA FLOWS; NIMS; CALIBRATION AB Galileo's Solid State Imager (SSI) observed Tvashtar Catena four times between November 1999 and October 2001, providing a unique look at a distinctive high latitude volcanic complex on Io. The first observation (orbit 125, November 1999) resolved, for the first time, an active extraterrestrial fissure eruption; the brightness temperature was at least 1300 K. The second observation (orbit 127, February 2000) showed a large (similar to 500 km(2)) region with many, small, hot, regions of active lava. The third observation was taken in conjunction with Cassini imaging in December 2000 and showed a Pele-like, annular plume deposit. The Cassini images revealed an similar to 400 km high Pele-type plume above Tvashtar Catena. The final Galileo SSI observation of Tvashtar (orbit 132, October 2001), revealed that obvious (to SSI) activity had ceased, although data from Galileo's Near Infrared Mapping Spectrometer (NIMS) indicated that there was still significant thermal emission from the Tvashtar region. In this paper, we primarily analyze the style of eruption during orbit 127 (February 2000). Comparison with a lava flow cooling model indicates that the behavior of the Tvashtar eruption during 127 does not match that of simple advancing lava flows. Instead, it may be an active lava lake or a complex set of lava flows with episodic, overlapping eruptions. The highest reliable color temperature is similar to 1300 K. Although higher temperatures cannot be ruled out, they do not need to be invoked to fit the observed data. The total power output from the active lavas in February 2000 was at least 10(11) W. (c) 2005 Elsevier Inc. All rights reserved. C1 Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. US Geol Survey, Astrogeol Team, Flagstaff, AZ 86001 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Planetary Sci Inst, Tucson, AZ 85719 USA. Univ Redlands, Redlands, CA 92373 USA. RP Milazzo, MP (reprint author), Univ Arizona, Lunar & Planetary Lab, 1541 E Univ Blvd, Tucson, AZ 85721 USA. EM mmilazzo@pirlmail.lpl.arizona.edu RI Turtle, Elizabeth/K-8673-2012 OI Turtle, Elizabeth/0000-0003-1423-5751 NR 69 TC 21 Z9 21 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 DEC 1 PY 2005 VL 179 IS 1 BP 235 EP 251 DI 10.1016/j.icarus.2005.05.013 PG 17 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 987XI UT WOS:000233550600014 ER PT J AU Roush, TL AF Roush, TL TI Near-infrared (0.67-4.7 mu m) optical constants estimated for montmorillonite SO ICARUS LA English DT Article DE mineralogy; radiative transfer; surfaces; planets; surfaces; satellites ID BIDIRECTIONAL REFLECTANCE SPECTROSCOPY; ABSORPTION-COEFFICIENTS; SPECTRAL REFLECTANCE; WATER ICE; MINERALS; OLIVINE; CLAYS; MODEL AB Optical constants are estimated from near-infrared reflectance spectra of the smectite clay montmorillonite using an iterative combination of particulate scattering theory and Kramers-Kronig analysis. The final results provide wavelength dependent imaginary indices of refraction similar to previous studies, but in addition produce wavelength dependent real indices of refraction, unlike most previous studies. A comparison of the values derived here to those previously reported for montmorillonite shows that the maxima absorption coefficient values from the two studies are in excellent agreement, and in other wavelength regions the two studies agree to within about a factor of two. This suggests that the approach presented can provide a reliable mechanism of estimating the wavelength dependence of both the real and imaginary indices for materials at visible and near-infrared wavelengths. The resulting near-infrared values are combined with mid-infrared values of the same sample to provide optical constants of montmorillonite over the 0.66-25 mu m wavelength region. Published by Elsevier Inc. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Roush, TL (reprint author), NASA, Ames Res Ctr, MS 245-3, Moffett Field, CA 94035 USA. EM troush@mail.arc.nasa.gov NR 36 TC 16 Z9 16 U1 1 U2 4 PU ACADEMIC PRESS INC ELSEVIER SCIENCE PI SAN DIEGO PA 525 B ST, STE 1900, SAN DIEGO, CA 92101-4495 USA SN 0019-1035 J9 ICARUS JI Icarus PD DEC 1 PY 2005 VL 179 IS 1 BP 259 EP 264 DI 10.1016/j.icarus.2005.06.004 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 987XI UT WOS:000233550600016 ER PT J AU Kent, BM Watkins, J Freundl, K Coveyou, T Cravens, L Buterbaugh, A Griffith, AD Scully, R AF Kent, BM Watkins, J Freundl, K Coveyou, T Cravens, L Buterbaugh, A Griffith, AD Scully, R TI Electromagnetic interference attenuation test of the space shuttle Discovery using the air force research laboratory mobile diagnostic laboratory SO IEEE ANTENNAS AND PROPAGATION MAGAZINE LA English DT Article DE electromagnetic measurements; electromagnetic interference; radar interference; radar measurements; attenuation measurement AB As NASA prepared the Space Shuttle for its first return-to-flight mission (STS-114) in July of 2005, a number of new visual and radar sensors were used during the critical ascent phase of the flight, to assess if unintentional debris was liberated from the Shuttle as it raced into orbit. New high-resolution C-band and X-band radars were used to help ascertain the location and speed of released debris. We also used both radars to monitor debris generated by routine flight events, such as solid rocket booster (SRB) separation. To assure that these new radars did not interfere with flight-critical engine subsystems, an electromagnetic interference (EMI) measurement was performed on the Shuttle Orbiter Discovery in January, 2005, using the Air Force Research Laboratory's Mobile Diagnostic Laboratory (MDL). This portable EM measurement system performed a large number of attenuation measurements the night of January 17-18, 2005. This paper describes how the attenuation data were acquired, and the methodology used to reduce the data to predict average attenuation of the radar energy from the outside world to the inside of the aft engine bay of the Orbiter. These data were combined with a separate NASA-performed avionics EMI analysis to demonstrate that the new C- and X-band debris radars could be operated without adversely interfering with the Orbiter aft-bay avionics systems. C1 USAF, Res Lab, Wright Patterson AFB, OH 45433 USA. ATK, Mission Res, Dayton, OH 45430 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Kent, BM (reprint author), USAF, Res Lab, AFRL SNS Bldg 254,2591 K St, Wright Patterson AFB, OH 45433 USA. NR 4 TC 0 Z9 0 U1 1 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1045-9243 EI 1558-4143 J9 IEEE ANTENN PROPAG M JI IEEE Antennas Propag. Mag. PD DEC PY 2005 VL 47 IS 6 BP 128 EP 134 DI 10.1109/MAP.2005.1608760 PG 7 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA 024SK UT WOS:000236216200016 ER PT J AU Poberezhskiy, IY Bortnik, B Chou, J Jalali, B Fetterman, HR AF Poberezhskiy, IY Bortnik, B Chou, J Jalali, B Fetterman, HR TI Serrodyne frequency translation of continuous optical signals using ultrawide-band electrical sawtooth waveforms SO IEEE JOURNAL OF QUANTUM ELECTRONICS LA English DT Article DE electrooptic modulation; optical frequency conversion; optical pulse shaping; phase modulation; signal synthesis ID SHIFTER AB Serrodyne frequency translation of continuous optical signals by +/- 1.28 GHz is reported, significantly exceeding the highest previously published serrodyne shifts. To achieve these shifts, an ultrawide-band high-power electrical sawtooth created by spectral modulation of dispersed optical pulses was used. Its amplification involved a novel predistortion technique to compensate for the gain and phase ripple in the amplifier bandwidth. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Calif Los Angeles, Dept Elect Engn, Los Angeles, CA 90095 USA. RP Poberezhskiy, IY (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM ilya@jpl.nasa.gov NR 11 TC 9 Z9 9 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9197 J9 IEEE J QUANTUM ELECT JI IEEE J. Quantum Electron. PD DEC PY 2005 VL 41 IS 12 BP 1533 EP 1539 DI 10.1109/JQE.2005.858467 PG 7 WC Engineering, Electrical & Electronic; Optics; Physics, Applied SC Engineering; Optics; Physics GA 988EM UT WOS:000233574400013 ER PT J AU Maestrini, A Ward, JS Javadi, H Tripon-Canseliet, C Gill, J Chattopadhyay, G Schlecht, E Mehdi, I AF Maestrini, A Ward, JS Javadi, H Tripon-Canseliet, C Gill, J Chattopadhyay, G Schlecht, E Mehdi, I TI Local oscillator chain for 1.55 to 1.75 THz with 100-/-mu W peak power SO IEEE MICROWAVE AND WIRELESS COMPONENTS LETTERS LA English DT Article DE frequency multiplier; frequency tripler; local oscillator (LO); Schottky diode; submillimeter wavelength; THz technology; varactor ID FREQUENCY TRIPLER AB We report on the design and performance of a fix-tuned x2x3x3 frequency multiplier chain that covers 1.55-1.75 THz. The chain is nominally pumped with 100 mW at W-band. At 120 K the measured output power is larger than 4 mu W across the band with a peak power of 100 mu W at 1.665 THz. A similar chain operated at room temperature produced a peak power of 21 mu W. These power levels now make it possible to deploy multipixel heterodyne imaging arrays in this frequency range. C1 Univ Paris 06, LISIF, F-75252 Paris, France. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Maestrini, A (reprint author), Univ Paris 06, LISIF, 12 Rue Cuvier, F-75252 Paris, France. EM alain.maestrini@lisif.jussieu.fr; john.ward@jpl.nasa.gov NR 7 TC 24 Z9 26 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 1531-1309 J9 IEEE MICROW WIREL CO JI IEEE Microw. Wirel. Compon. Lett. PD DEC PY 2005 VL 15 IS 12 BP 871 EP 873 DI 10.1109/LMWC.2005.859989 PG 3 WC Engineering, Electrical & Electronic SC Engineering GA 994OF UT WOS:000234040400015 ER PT J AU Dawson, D Samoska, L Fung, AK Lee, K Lai, R Grundbacher, R Liu, PH Raja, R AF Dawson, D Samoska, L Fung, AK Lee, K Lai, R Grundbacher, R Liu, PH Raja, R TI Beyond G-Band: A 235 GHz InP MMIC amplifier SO IEEE MICROWAVE AND WIRELESS COMPONENTS LETTERS LA English DT Article DE G-Band; high electron mobility transistors (HEMTs); indium phosphide; millimeter wave field-effect transistor (FET) amplifiers; monolithic millimeter-wave integrated circuits (MMICs); WR3 waveguide ID INDIUM-PHOSPHIDE; MODULE AB We present results on an InP monolithic millimeter-wave integrated circuit (MMIC) amplifier having 10-dB gain at 235 GHz. We designed this circuit and fabricated the chip in Northrop Grumman Space Technology's (NGST) 0.07-mu m InP high electron mobility transistor (HEMT) process. Using a WR3 (220-325 GHz) waveguide vector network analyzer system interfaced to waveguide wafer probes, we measured this chip on-wafer for S-parameters. To our knowledge, this is the first time a WR3 waveguide on-wafer measurement system has been used to measure gain in a MMIC amplifier above 230 GHz. Index Terms-G-Band, high electron mobility transistors (HEMTs), indium phosphide, millimeter wave field-effect transistor (FET) amplifiers, monolithic millimeter-wave integrated circuits (MMICs), WR3 waveguide. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Northrop Grumman Space Technol, Redondo Beach, CA 90278 USA. RP CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM lorene.samoska@jpl.nasa.gov; ronald.grundbacher@ngc.com NR 13 TC 32 Z9 33 U1 0 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1531-1309 EI 1558-1764 J9 IEEE MICROW WIREL CO JI IEEE Microw. Wirel. Compon. Lett. PD DEC PY 2005 VL 15 IS 12 BP 874 EP 876 DI 10.1109/LMWC.2005.859984 PG 3 WC Engineering, Electrical & Electronic SC Engineering GA 994OF UT WOS:000234040400016 ER PT J AU Bleier, T Freund, F AF Bleier, T Freund, F TI Earthquake SO IEEE SPECTRUM LA English DT Article C1 QuakeFinder, Palo Alto, CA USA. NASA, Ames Res Ctr, Mountain View, CA USA. San Jose State Univ, San Jose, CA 95192 USA. RP Bleier, T (reprint author), QuakeFinder, Palo Alto, CA USA. NR 0 TC 8 Z9 8 U1 0 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9235 J9 IEEE SPECTRUM JI IEEE Spectr. PD DEC PY 2005 VL 42 IS 12 BP 22 EP 27 DI 10.1109/MSPEC.2005.1549778 PG 6 WC Engineering, Electrical & Electronic SC Engineering GA 990ZO UT WOS:000233782100016 ER PT J AU Pogorzelski, RJ AF Pogorzelski, RJ TI On the steady-state phase distribution in a hexagonally coupled oscillator array SO IEEE TRANSACTIONS ON ANTENNAS AND PROPAGATION LA English DT Article DE mutual injection locking; phased array antennas; voltage controlled oscillators ID INJECTION; DYNAMICS AB The distribution of the phase of the oscillations of a set of mutually injection locked electronic oscillators is investigated for the case of a hexagonal nearest neighbor coupling topology. It is shown that planar distributions are not, in general, steady-state solutions of the system of nonlinear differential equations governing the system. An exact steady-state solution of the equations is obtained and shown to be planar only for six discrete azimuth angles. The degree of deviation from a planar distribution is determined and its impact on the directivity of a phased array excited by the oscillator output signals is estimated. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM pogo@jpl.nasa.gov NR 20 TC 5 Z9 5 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-926X EI 1558-2221 J9 IEEE T ANTENN PROPAG JI IEEE Trans. Antennas Propag. PD DEC PY 2005 VL 53 IS 12 BP 4058 EP 4064 DI 10.1109/TAP.2005.859766 PG 7 WC Engineering, Electrical & Electronic; Telecommunications SC Engineering; Telecommunications GA 994OD UT WOS:000234040200030 ER PT J AU Wolpert, DH Macready, WG AF Wolpert, DH Macready, WG TI Coevolutionary free lunches SO IEEE TRANSACTIONS ON EVOLUTIONARY COMPUTATION LA English DT Article DE coevolution; multiarmed bandits; no free lunch; optimizations; self-play ID A-PRIORI DISTINCTIONS; NO FREE LUNCH; LEARNING ALGORITHMS; SEARCH; EVOLUTION AB Recent work on the foundational underpinnings of black-box optimization has begun to uncover a rich mathematical structure. In particular, it is now known that an inner product between the optimization algorithm and the distribution of optimization problems likely to be encountered fixes the distribution over likely performances in running that algorithm. One ramilication of this is the "No Free Lunch" (NFL) theorems, which state that any two algorithms are equivalent when their performance is averaged across all possible problems. This highlights the need for exploiting problem-specific knowledge to achieve better than random performance. In this paper, we present a general framework covering most optimization scenarios. In addition to the optimization scenarios addressed in the NFL results, this framework covers multiarmed bandit problems and evolution of multiple coevolving players. As a particular instance of the latter, it covers "self-play" problems. In these problems, the set of players work together to produce a champion, who then engages one or more antagonists in a subsequent multiplayer game. In contrast to the traditional optimization case where the NFL results hold, we show that in self-play there are free lunches: in coevolution some algorithms have better performance than other algorithms, averaged across all possible problems. However, in the typical coevolutionary scenarios encountered in biology, where there is no champion, the NFL theorems still hold. C1 NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. D Wave Syst, Vancouver, BC V6J 4Y3, Canada. RP NASA, Ames Res Ctr, Moffett Field, Moffett Field, CA 94035 USA. EM dhw@email.arc.nasa.gov; wgm@dwavesys.com NR 36 TC 48 Z9 50 U1 0 U2 11 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1089-778X EI 1941-0026 J9 IEEE T EVOLUT COMPUT JI IEEE Trans. Evol. Comput. PD DEC PY 2005 VL 9 IS 6 BP 721 EP 735 DI 10.1109/TEVC.2005.856205 PG 15 WC Computer Science, Artificial Intelligence; Computer Science, Theory & Methods SC Computer Science GA 993RO UT WOS:000233972800015 ER PT J AU Fujisada, H Bailey, GB Kelly, GG Hara, S Abrams, MJ AF Fujisada, H Bailey, GB Kelly, GG Hara, S Abrams, MJ TI ASTER DEM performance SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) instrument; digital elevation model (DEM); high resolution; optical sensor; stereo AB The Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) instrument onboard the National Aeronautics and Space Administration's Terra spacecraft has an along-track stereoscopic capability using its a near-infrared spectral band to acquire the stereo data. ASTER has two telescopes, one for nadir-viewing and another for backward-viewing, with a base-to-height ratio of 0.6. The spatial resolution is 15 in in the horizontal plane. Parameters such as the line-of-sight vectors and the pointing axis were adjusted during the initial operation period to generate Level-1 data products with a high-quality stereo system performance. The evaluation of the digital elevation model (DEM) data was carried out both by Japanese and U.S. science teams separately using different DEM generation software and reference databases. The vertical accuracy of the DEM data generated from the Level-1A data is 20 in with 95% confidence without ground control point (GCP) correction for individual scenes. Geolocation accuracy that is important for the DEM datasets is better than 50 m. This appears to be limited by the spacecraft position accuracy. In addition, a slight increase in accuracy is observed by using GCPs to generate the stereo data. C1 Sensor Informat Lab Corp, Ibaraki 3050005, Japan. US Geol Survey, Earth Resources Observ Syst Data Ctr, Sioux Falls, SD 57198 USA. Cent Comp Serv Co Ltd, Tokyo 1050001, Japan. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Fujisada, H (reprint author), Sensor Informat Lab Corp, Ibaraki 3050005, Japan. NR 6 TC 113 Z9 122 U1 2 U2 18 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD DEC PY 2005 VL 43 IS 12 BP 2707 EP 2714 DI 10.1109/TGRS.2005.847924 PG 8 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 986VY UT WOS:000233479000002 ER PT J AU Tonooka, H Palluconi, FD Hook, SJ Matsunaga, T AF Tonooka, H Palluconi, FD Hook, SJ Matsunaga, T TI Vicarious calibration of ASTER thermal infrared bands SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE degradation; field experiment; gain; offset; onboard calibration; radiative transfer; responsivity; spectral emissivity; surface temperature; vicarious calibration ID RADIOMETER CALIBRATION; LAKE TAHOE; VALIDATION; PREFLIGHT; SENSORS AB The Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) on the, Terra satellite has five bands in the thermal infrared (TIR) spectral region between 8-12 mu m. The TIR bands have been regularly validated in-flight using ground validation targets., Validation results are presented from 79 experiments conducted under clear sky conditions. Validation involved predicting the at-sensor radiance for each band using a radiative transfer model, driven by surface and atmospheric measurements from each experiment, and then comparing the predicted radiance with the ASTER measured radiance. The results indicate the average difference between the predicted and the ASTER measured radiances was no more than 0.5% or 0.4 K in any TIR band, demonstrating that the TIR bands have exceeded the preflight design accuracy of < 1 K for an at-sensor brightness temperature range of 270-340 K. The predicted and the ASTER measured radiances were then used to assess how well the onboard calibration accounted for any changes in both the instrument gain and offset over time. The results indicate that the gain and offset were correctly determined using the onboard blackbody, and indicate a responsivity decline over the first 1400 days of the Terra mission. C1 Ibaraki Univ, Ibaraki 3168511, Japan. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Natl Inst Environm Studies, Ibaraki 3058506, Japan. RP Tonooka, H (reprint author), Ibaraki Univ, Ibaraki 3168511, Japan. EM tonooka@mx.ibaraki.ac.jp NR 24 TC 46 Z9 46 U1 0 U2 6 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD DEC PY 2005 VL 43 IS 12 BP 2733 EP 2746 DI 10.1109/TGRS.2005.857885 PG 14 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 986VY UT WOS:000233479000005 ER PT J AU Tonooka, H Palluconi, FD AF Tonooka, H Palluconi, FD TI Validation of ASTER/TIR standard atmospheric correction using water surfaces SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE emissivity; MODTRAN; National Centers for Environmental Prediction (NCEP)/Global Data Assimilation System (GDAS); Naval Research Laboratory (NRL) climatology model; precipitable water vapor (PWV); radiative transfer; temperature; vicarious calibration ID SPLIT-WINDOW ALGORITHM; THERMAL INFRARED DATA; SEA-SURFACE; MU-M; TEMPERATURE; LAND; EMISSIVITY; ABSORPTION; RADIOMETER; SATELLITE AB The standard atmospheric correction algorithm for the five thermal infrared (TIR) bands of the Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) is based on radiative transfer calculation using the MODTRAN code. Atmospheric profiles input to MODTRAN are extracted from either the Global Data Assimilation System (GDAS) product or the Naval Research Laboratory (NRL) climatology model. The present study provides validation results of this algorithm. First, in situ lake surface temperatures measured in 13 vicarious calibration (VC) experiments were compared with surface temperatures retrieved from ASTER data. As the results, the mean bias was 0.8 and 1.8 K for GDAS and NRL, respectively. The NRL model performed worse than GDAS for four experiments at Salton Sea, CA, probably because the model was not suitable for this site, which has typically higher surface temperature and humidity than other VC sites. Next, the algorithm was validated based on the max-min difference (MMD) of water surface emissivity retrieved from each of 163 scenes acquired globally. As a result, the algorithm error increased quadratically with the precipitable water vapor (PWV) content of the atmosphere, and the expected MMD error was 0.049 and 0.067 for GDAS and NRL, respectively, with a PWV of 3 cm, where 0.05 on MMD is roughly corresponding to -0.8 or +2.3 K on the retrieved surface temperature error. The algorithm performance degraded markedly when the surface temperature exceeded about 25 degrees C, particularly for NRL. Consequently, GDAS performs better than NRL as expected, while both will perform less well for humid conditions. C1 Ibaraki Univ, Ibaraki 3168511, Japan. Jet Propuls Lab, Pasadena, CA 91109 USA. RP Ibaraki Univ, Ibaraki 3168511, Japan. EM tonooka@mx.ibaraki.ac.jp NR 40 TC 19 Z9 19 U1 0 U2 7 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0196-2892 EI 1558-0644 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD DEC PY 2005 VL 43 IS 12 BP 2769 EP 2777 DI 10.1109/TGRS.2005.857883 PG 9 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 986VY UT WOS:000233479000009 ER PT J AU Liao, L Meneghini, R AF Liao, L Meneghini, R TI On modeling air/spaceborne radar returns in the melting layer SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE air/spaceborne radar; effective dielectric constant; electric scattering; melting layer; radar bright band ID REMOTE-SENSING APPLICATIONS; MULTIPLE-SCATTERING; PRECIPITATION RADAR; CROSS-SECTIONS; RAIN; HYDROMETEORS; SNOWFLAKES; CONSTANTS; SNOW AB The bright band is the enhanced radar echo associated with the melting of hydrometeors in stratiform rain. To simulate this radar signature, a scattering model of melting snow is proposed in which the fractional water content is prescribed as a function of the radius of a spherical mixed-phase particle consisting of air, ice, and water. The model is based on the observation that melting starts at the surface of the particle and then gradually develops toward the center. To compute the scattering parameters of a nonuniform melting particle, the particle is modeled as a sphere represented by a collection of 64(3) cubic cells of identical size where the probability of water at any cell is prescribed as a function of the radius. The internal held of the particle, used for deriving the effective dielectric constant, is computed by the conjugate gradient and fast Fourier transform (CGFFT) numerical methods. To make computations of the scattering parameters more efficient, a multilayer stratified-sphere scattering model is introduced after demonstrating that the scattering parameters of the nonuniformly melting particle can be accurately reproduced by the stratified sphere. In conjunction with a melting layer model that describes the melting fractions and fall velocities of hydrometeors as a function of the distance from the 0 degrees C isotherm, the stratified-sphere model is used to simulate the radar bright-band profiles. These simulated profiles are shown to compare well with measurements from the Precipitation Radar (PR) aboard the Tropical Rainfall Measuring Mission (TRMM) satellite and a dual-wavelength airborne radar. The results suggest that the proposed model of a melting snow particle may be useful in studying the characteristics of the bright-band in particular and mixed-phase hydrometeors in general. C1 Caelum Res Corp, Rockville, MD 20850 USA. NASA, Goddard Space Flight Ctr, Earth Sci & Technol Ctr, Greenbelt, MD 20771 USA. NASA, Goddard Space Flight Ctr, Instrument Sci Branch, Greenbelt, MD 20771 USA. RP Liao, L (reprint author), Caelum Res Corp, Rockville, MD 20850 USA. EM lliao@neptune.gsfc.nasa.gov NR 34 TC 17 Z9 17 U1 0 U2 5 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD DEC PY 2005 VL 43 IS 12 BP 2799 EP 2809 DI 10.1109/TGRS.2005.848704 PG 11 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 986VY UT WOS:000233479000012 ER PT J AU Crosson, WL Limaye, AS Laymon, CA AF Crosson, WL Limaye, AS Laymon, CA TI Parameter sensitivity of soil moisture retrievals from airborne C- and X-band radiometer measurements in SMEX02 SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE microwave radiometry; parameter space methods; sensitivity; Soil Moisture Experiments in 2002 (SMEX02); soil moisture; vegetation ID PASSIVE MICROWAVE MEASUREMENTS; VEGETATION WATER-CONTENT; EMISSION; POLARIZATION; FIELDS; INDEX AB Among passive microwave frequencies, sensors operating at C- and X-band frequencies have been used with some success to estimate near-surface soil moisture from aircraft and satellite platforms. The objective of this paper is to quantify the sensitivities of soil moisture retrieved via a single-channel single-polarization algorithm to the observed brightness temperature and to retrieval algorithm parameters of surface roughness, vegetation B parameter, and single-scattering albedo. Examination of the regions within the parameter space that produce accurate soil moisture retrievals reveals that reasonably accurate retrievals can be made over a range of conditions using a fixed set of input parameters. Retrievals with horizontally polarized brightness temperature observations are more consistent than with vertically polarized observations. At horizontal polarization, sensitivity to the input parameters is much greater for wet soils than for dry soils, whereas for vertical polarization the moisture dependence is much weaker. At vertical polarization, sensitivities to variations in all parameters are much lower. To ensure that retrieval accuracy specifications are consistently met, high soil moisture conditions should be used in defining parameter accuracy requirements. Given the spatial and temporal variability of vegetation and soil conditions, it seems unlikely that, for regions with substantial rapidly growing vegetation, the accuracy requirements for model parameters in a single-frequency, single-polarization retrieval algorithm can be met with current satellite products. For such conditions, any soil moisture retrieval algorithm using parameterizations similar to those of this study may require multiple frequencies, polarizations, or look angles to produce stable, reliable soil moisture estimates. C1 NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, Global Hydrol & Climate Ctr, Huntsville, AL 35805 USA. RP Crosson, WL (reprint author), NASA, George C Marshall Space Flight Ctr, Univ Space Res Assoc, Global Hydrol & Climate Ctr, Huntsville, AL 35805 USA. EM bill.crosson@msfc.nasa.gov NR 25 TC 12 Z9 12 U1 0 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD DEC PY 2005 VL 43 IS 12 BP 2842 EP 2853 DI 10.1109/TGRS.2005.857916 PG 12 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 986VY UT WOS:000233479000016 ER PT J AU Kaufman, YJ Remer, LA Tanre, D Li, RR Kleidman, R Mattoo, S Levy, RC Eck, TF Holben, BN Ichoku, C Martins, JV Koren, I AF Kaufman, YJ Remer, LA Tanre, D Li, RR Kleidman, R Mattoo, S Levy, RC Eck, TF Holben, BN Ichoku, C Martins, JV Koren, I TI A critical examination of the residual cloud contamination and diurnal sampling effects on MODIS estimates of aerosol over ocean SO IEEE TRANSACTIONS ON GEOSCIENCE AND REMOTE SENSING LA English DT Article DE aerosol; cirrus; cloud; Moderate Resolution Imaging Spectroradiometer (MODIS); remote sensing. ID OPTICAL DEPTH; STRATOSPHERIC AEROSOLS; DUST AEROSOL; AIR-QUALITY; VARIABILITY; RETRIEVALS; AERONET; CLIMATOLOGY; SATELLITE; PRODUCTS AB Observations of the aerosol optical thickness (AOT) by the Moderate Resolution Imaging Spectroradiometer (MODIS) instruments aboard Terra and Aqua satellites are being used extensively for applications to climate and air quality studies. Data quality is essential for these studies. Here we investigate the effects of unresolved clouds on the MODIS measurements of the AOT. The main cloud effect is from residual cirrus that increases the AOT by 0.015 +/- 0.003 at 0.55 mu m. In addition, lower level clouds can add contamination. We examine the effect of lower clouds using the difference between simultaneously measured MODIS and AFRONET AOT. The difference is positively correlated with the cloud fraction. However, interpretation of this difference is sensitive to the definition of cloud contamination versus aerosol growth. If we consider this consistent difference between MODIS and AERONET to be entirely due to cloud contamination we get a total cloud contamination of 0.025 +/- 0.005, though a more likely estimate is closer to 0.020 after accounting for aerosol growth. This reduces the difference between MODIS-observed global aerosol optical thickness over the oceans and model simulations by half, from 0.04 to 0.02. However it is insignificant for studies of aerosol cloud interaction. We also examined how representative are the MODIS data of the diurnal average aerosol. Comparison to monthly averaged sunphotometer data confirms that either the Terra or Aqua estimate of global AOT is a valid representation of the daily average. Though in the vicinity of aerosol sources such as fires, we do not expect this to be true. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Sci & Tech Lille Flandres Artois, CNRS, Opt Atmospher Lab, F-59655 Villeneuve Dascq, France. Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21250 USA. Sci Syst & Appl Inc, Lanham, MD 20706 USA. Univ Maryland Baltimore Cty, Joint Ctr Earth Syst Technol, Baltimore, MD 21250 USA. RP Kaufman, YJ (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. EM kaufman@climate.gsfc.nasa.gov RI ECK, THOMAS/D-7407-2012; Ichoku, Charles/E-1857-2012; Koren, Ilan/K-1417-2012; Levy, Robert/M-7764-2013 OI Ichoku, Charles/0000-0003-3244-4549; Koren, Ilan/0000-0001-6759-6265; Levy, Robert/0000-0002-8933-5303 NR 59 TC 118 Z9 123 U1 1 U2 11 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0196-2892 J9 IEEE T GEOSCI REMOTE JI IEEE Trans. Geosci. Remote Sensing PD DEC PY 2005 VL 43 IS 12 BP 2886 EP 2897 DI 10.1109/TGRS.2005.858430 PG 12 WC Geochemistry & Geophysics; Engineering, Electrical & Electronic; Remote Sensing; Imaging Science & Photographic Technology SC Geochemistry & Geophysics; Engineering; Remote Sensing; Imaging Science & Photographic Technology GA 986VY UT WOS:000233479000021 ER PT J AU Marcin, MR AF Marcin, MR TI Digital receiver phase meter for LISA SO IEEE TRANSACTIONS ON INSTRUMENTATION AND MEASUREMENT LA English DT Article DE demodulation; extraterrestrial measurements; gravity measurement; optical variables measurement; phase measurement AB A study of a commercially available digital receiver configured as a phase meter has been performed. The effort was part of the technology development phase of the Laser Interferometer Space Antenna (LISA) mission. LISA requires that phase measurements on the metrology signals be made at a rate of 10 Hz with root power spectral density of 5 mu cycle/root Hz over the gravitational wave detection band from 1 mHz to 1 Hz. The phase meter must also contend with heterodyne interferometric signals having superposed Doppler shifts as high as 15 MHz. It is found that the off-the-shelf prototype can fulfill these requirements. C1 CALTECH, Jet Propuls Lab, Pasadena, CA 91109 USA. RP Marcin, MR (reprint author), CALTECH, Jet Propuls Lab, Pasadena, CA 91109 USA. EM martin.marcin@jpl.nasa.gov NR 13 TC 2 Z9 2 U1 0 U2 6 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9456 J9 IEEE T INSTRUM MEAS JI IEEE Trans. Instrum. Meas. PD DEC PY 2005 VL 54 IS 6 BP 2446 EP 2453 DI 10.1109/TIM.2005.858125 PG 8 WC Engineering, Electrical & Electronic; Instruments & Instrumentation SC Engineering; Instruments & Instrumentation GA 986HU UT WOS:000233441500040 ER PT J AU Mao, ZH Dugail, D Feron, E Bilimoria, K AF Mao, ZH Dugail, D Feron, E Bilimoria, K TI Stability of intersecting aircraft flows using heading-change maneuvers for conflict avoidance SO IEEE TRANSACTIONS ON INTELLIGENT TRANSPORTATION SYSTEMS LA English DT Article DE aircraft flow; conflict resolution; domino effect; heading-change maneuver ID RESOLUTION; PERFORMANCE; MANAGEMENT; VEHICLES AB This paper analyzes two intersecting flows of aircraft that must avoid each other, utilizing maneuvers modeled by instantaneous heading changes. Sufficient conditions are derived for stable conflict avoidance, whereby one aircraft's conflict-avoidance action does not generate cascaded diverging conflict-avoidance behavior (known as the domino effect) in neighboring aircraft. The mathematics involved with the heading-change model are considerably more complex than those using the simpler offset-maneuver models utilized in the previous work. However, this additional effort is largely compensated by the improved realism of the maneuver model, as well as new insights in the inherent robustness of conflict-avoidance maneuver schemes based on heading changes against specified separation standards. The analytical results are compared with simulations. C1 Univ Pittsburgh, Dept Elect & Comp Engn, Pittsburgh, PA 15261 USA. Dassault Aviat, F-13002 Marseille, France. Georgia Inst Technol, Daniel Guggenheim Sch Aerosp Engn, Atlanta, GA 30332 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Univ Pittsburgh, Dept Elect & Comp Engn, Pittsburgh, PA 15261 USA. EM maozh@engr.pitt.edu; dugail@alum.mit.edu; eric.feron@aerospace.gatech.edu; Karl.Bilimoria@nasa.gov NR 20 TC 19 Z9 23 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 1524-9050 EI 1558-0016 J9 IEEE T INTELL TRANSP JI IEEE Trans. Intell. Transp. Syst. PD DEC PY 2005 VL 6 IS 4 BP 357 EP 369 DI 10.1109/TITS.2005.858789 PG 13 WC Engineering, Civil; Engineering, Electrical & Electronic; Transportation Science & Technology SC Engineering; Transportation GA 998WH UT WOS:000234350100001 ER PT J AU Niu, GF Yang, H Varadharajaperumal, M Shi, Y Cressler, JD Krithivasan, R Marshall, PW Reed, R AF Niu, GF Yang, H Varadharajaperumal, M Shi, Y Cressler, JD Krithivasan, R Marshall, PW Reed, R TI Simulation of a new back junction approach for reducing charge collection in 200 GHz SiGeHBTs SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 42nd Annual Nuclear and Space Radiation Effects Conference (NSREC) CY JUL 11-15, 2005 CL Seattle, WA SP IEEE DE charge collection; charge sharing; SEU; SiGeHBT ID SOI AB We present a new back junction approach for reducing SEU-induced charge collection in SiGe HBTS, and demonstrate its effectiveness in a state-of-the-art 200 GHz SiGe HBT using full 3-D device simulation. An additional n(+) layer is used below the p-type isolation layer to form a back junction. The back junction limits potential funneling to within the p-type layer, which effectively limits the total amount of drift charge collection that is now shared by the collector-to-substrate junction and the back junction. The back junction also cuts off the diffusion charge coming from the substrate, further limiting charge collection by the HBT collector. A thinner p-type "substrate" layer and a better contact to the added n+ layer are shown to help reduce charge collection by the HBT collector, the sensitive node. C1 Auburn Univ, Dept Elect & Comp Engn, Auburn, AL 36849 USA. Georgia Inst Technol, Atlanta, GA 30332 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Vanderbilt Univ, Vanderbilt, TN 37203 USA. RP Auburn Univ, Dept Elect & Comp Engn, Auburn, AL 36849 USA. EM niuguof@auburn.edu RI Shi, Y/G-3964-2010; Krithivasan, Ramkumar/D-3549-2011 NR 12 TC 9 Z9 10 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2005 VL 52 IS 6 BP 2153 EP 2157 DI 10.1109/TNS.2005.860744 PN 1 PG 5 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 017LL UT WOS:000235695000014 ER PT J AU Petersen, EL Pouget, V Massengill, LW Buchner, SP McMorrow, D AF Petersen, EL Pouget, V Massengill, LW Buchner, SP McMorrow, D TI Rate predictions for single-event effects - Critique II SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 42nd Annual Nuclear and Space Radiation Effects Conference (NSREC) CY JUL 11-15, 2005 CL Seattle, WA SP IEEE DE figure of merit (FOM); heavy ion; picosecond pulsed laser; proton; SEU rates; single event simulation; single event upset (SEU) ID CROSS-SECTION MEASUREMENTS; UPSET RATE CALCULATIONS; SEE RATE CALCULATIONS; RAY-INDUCED ERRORS; PULSED-LASER; COSMIC-RAYS; HEAVY-ION; INTEGRATED-CIRCUITS; COMPUTER MEMORIES; FIGURE AB The concept of charge efficacy is introduced as a measure of the effectiveness of incident charge for producing single-event upsets. Efficacy is a measure of the single-event upset (SEU) sensitivity within a cell. It is illustrated how the efficacy curve can be determined from standard heavy-ion or pulsed laser SEU cross-section data, and discussed how it can be calculated from combined charge collection and circuit analysis. Upset rates can be determined using the figure of merit approach, and values determined from the laser cross-sections or from the mixed-mode simulations. The standard integral rectangular parallel-piped (IRPP) method for upset rate calculation is re-examined assuming that the probability of upset depends on the location of the hit on the surface. It is concluded that it is unnecessary to reformulate the IRPP approach. C1 CNRS, UMR 3405, IXL, Talence, France. Vanderbilt Univ, Nashville, TN 37203 USA. NASA, Goddard Space Flight Ctr, QSS Grp Inc, Greenbelt, MD 20771 USA. USN, Res Lab, Washington, DC 20375 USA. RP Petersen, EL (reprint author), 17289 Kettlebrook Landing, Jeffersonton, VA 22724 USA. EM epetersen3@earthlink.net; pouget@ixl.fr; lloyd.niassengill@vanderbilt.edu; sbuchner@pop500.gsfc.nasa.gov; mcmorrow@ccs.nrl.navy.mil NR 48 TC 14 Z9 14 U1 1 U2 6 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2005 VL 52 IS 6 BP 2158 EP 2167 DI 10.1109/TNS.2005.860687 PN 1 PG 10 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 017LL UT WOS:000235695000015 ER PT J AU Howe, CL Weller, RA Reed, RA Mendenhall, MH Schrimpf, RD Warren, KM Ball, DR Massengill, LW LaBel, KA Howard, JW Haddad, NF AF Howe, CL Weller, RA Reed, RA Mendenhall, MH Schrimpf, RD Warren, KM Ball, DR Massengill, LW LaBel, KA Howard, JW Haddad, NF TI Role of heavy-ion nuclear reactions in determining on-orbit single event error rates SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 42nd Annual Nuclear and Space Radiation Effects Conference (NSREC) CY JUL 11-15, 2005 CL Seattle, WA SP IEEE DE charge deposition; Geant4; heavy ion; MRED; single-event upset (SEU); SEU error rate ID ALGORITHM AB Simulations show that neglecting ion-ion interaction processes (both particles having Z > 1) results in an underestimation of the total on-orbit single event upset error rate by more than two orders of magnitude for certain technologies. The inclusion of ion-ion nuclear reactions leads to dramatically different SEU error rates for CMOS devices containing high Z materials compared with direct ionization by the primary ion alone. Device geometry and material composition have a dramatic effect on charge deposition in small sensitive volumes for the spectrum of ion energies found in space, compared with the limited range of energies typical of ground tests. C1 Vanderbilt Univ, Dept Elect Engn & Comp Sci, Nashville, TN 37235 USA. Vanderbilt Univ, Inst Space & Def Elect, Nashville, TN 37235 USA. Vanderbilt Univ, Free Electron Laser Ctr, Nashville, TN 37235 USA. Vanderbilt Univ, Inst Space & Def Elect, Nashville, TN 37203 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Jackson & Tull Chartered Engineers, Washington, DC 20018 USA. BAE Syst, Manassas, VA 20110 USA. RP Howe, CL (reprint author), Vanderbilt Univ, Dept Elect Engn & Comp Sci, Nashville, TN 37235 USA. EM christina.l.howe@vanderbilt.edu RI Schrimpf, Ronald/L-5549-2013 OI Schrimpf, Ronald/0000-0001-7419-2701 NR 13 TC 49 Z9 50 U1 0 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2005 VL 52 IS 6 BP 2182 EP 2188 DI 10.1109/TNS.2005.860683 PN 1 PG 7 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 017LL UT WOS:000235695000018 ER PT J AU Jun, I Garrett, HB Evans, RW AF Jun, I Garrett, HB Evans, RW TI High-energy trapped particle environments at Jupiter: An update SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 42nd Annual Nuclear and Space Radiation Effects Conference (NSREC) CY JUL 11-15, 2005 CL Seattle, WA SP IEEE DE Jupiter; Galileo energetic particle detector; Galileo heavy ion counter ID MAGNETOSPHERE; DETECTOR AB The particle data measured by the energetic particle detector (EPD) and heavy ion counter (HIC) on board Galileo were used to update the radiation environments at Jupiter: EPD data for trapped electrons and HIC data for trapped carbon, oxygen, and sulfur ions. The models developed in this study were successfully used to generate the total dose and single event effect environments for a sample mission to Europa. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Gibbel Corp, Montrose, CA 91020 USA. RP Jun, I (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM insoo.jun@jpl.nasa.gov; henry.b.garrett@jpl.nasa.gov; robin.w.evans@jpl.nasa.gov NR 13 TC 7 Z9 7 U1 0 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2005 VL 52 IS 6 BP 2281 EP 2286 DI 10.1109/TNS.2005.860747 PN 1 PG 6 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 017LL UT WOS:000235695000034 ER PT J AU Scheick, LZ Blake, B McNulty, PJ AF Scheick, LZ Blake, B McNulty, PJ TI Microdosimetry of the ultraviolet erasable programmable read-only memory experiment on the microelectronics and photonics test bed: Recent advances in small-volume analysis SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 42nd Annual Nuclear and Space Radiation Effects Conference (NSREC) CY JUL 11-15, 2005 CL Seattle, WA SP IEEE DE extreme value; extreme value analysis; extreme value theory; floating gate; microdose; MPTB; non-volatile; NVM; UVPROM; satellite; single event; stuck bit; transfer orbit ID CHARGE; SPACE AB A commercial ultraviolet erasable programmable read-only memory (UVPROM) was used to demonstrate a dosimetry technique for both ground and space applications. An equivalent amount of UV to reproduce the same amount of erasure was used to calibrate dose. The new method of readout, unlike other methods, does not require the evidence of exposure to be destroyed in the course of a measurement. It requires power only during readout. Results from an experiment using this technique aboard the Microelectronics and Photonics Test Bed (MPTB) satellite are discussed. Application of Extreme Value Theory is used to analyze whether early failures in the device were statistically feasible or more likely due to large, rare energy depositions. A new dosimeter approach using a change injection method that will eliminate the need for UV as a-metric is also presented as well new experiments for the devices under test aboard MPTB. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Aerosp Corp, El Segundo, CA 90245 USA. Clemson Univ, Clemson, SC 29603 USA. RP Scheick, LZ (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM leif.scheick@jpl.nasa.gov; JBernard.Blake@aero.org; mpeter@clemson.edu NR 14 TC 3 Z9 3 U1 0 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2005 VL 52 IS 6 BP 2300 EP 2306 DI 10.1109/TNS.2005.860750 PN 1 PG 7 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 017LL UT WOS:000235695000037 ER PT J AU Spratt, JP Aghara, S Fu, B Lichtenhan, JD Leadon, R AF Spratt, JP Aghara, S Fu, B Lichtenhan, JD Leadon, R TI A Conformal coating for shielding against naturally occurring thermal neutrons SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 42nd Annual Nuclear and Space Radiation Effects Conference (NSREC) CY JUL 11-15, 2005 CL Seattle, WA SP IEEE DE boron fission; conformal coating; neutron induced upset; thermal neutron shields AB Calculations and experimental data on the shielding effectiveness of a new kind of conformal coating against thermal neutrons typical of the natural environment are presented. This coating is shown to be capable of significantly reducing the thermal neutron threat to COTS ICs in a cost-effective manner. C1 Full Circle Res Inc, Redondo Beach, CA 90277 USA. NASA, Ctr Appl Radiat Res, Prairie View, TX 77446 USA. Hybrid Plast Inc, Hattiesburg, MS 39401 USA. RP Spratt, JP (reprint author), Full Circle Res Inc, Redondo Beach, CA 90277 USA. NR 10 TC 1 Z9 1 U1 1 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2005 VL 52 IS 6 BP 2340 EP 2344 DI 10.1109/TNS.2005.860752 PN 1 PG 5 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 017LL UT WOS:000235695000043 ER PT J AU Chen, TB Sutton, AK Bellini, M Haugerud, BM Comeau, JP Liang, QQ Cressler, JD Cai, J Ning, TH Marshall, PW Marshall, CJ AF Chen, TB Sutton, AK Bellini, M Haugerud, BM Comeau, JP Liang, QQ Cressler, JD Cai, J Ning, TH Marshall, PW Marshall, CJ TI Proton radiation effects in vertical SiGeHBTs fabricated on CMOS-compatible SOI SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 42nd Annual Nuclear and Space Radiation Effects Conference (NSREC) CY JUL 11-15, 2005 CL Seattle, WA SP IEEE DE HBT; radiation; SiGe; SOI AB Proton radiation effects in vertical SiGe HBTs fabricated on CMOS-compatible silicon-on-insulator (SOI) are investigated for the first time. Proton irradiation at 63 MeV is found to introduce base leakage current at low base-emitter voltage, delay the onset of Kirk effect at high injection, and increase the frequency response of SiGe HBTs on SOL The latter two effects are in contrast to those found in conventional bulk SiGe HBTs. Proton irradiation also generates positive fixed oxide and interface charge in the buried oxide, which alters both M-1 and BVCEO in the SiGe HBT by modulating the electric field in the collector region. C1 Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA. IBM Res Corp, Yorktown Hts, NY 10598 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30332 USA. EM tianbing@ece.gatech.edu NR 13 TC 11 Z9 12 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2005 VL 52 IS 6 BP 2353 EP 2357 DI 10.1109/TNS.2005.860726 PN 1 PG 5 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 017LL UT WOS:000235695000045 ER PT J AU Sutton, AK Haugerud, BM Prakash, APG Jun, B Cressler, JD Marshall, CJ Marshall, PW Ladbury, R Guarin, F Joseph, AJ AF Sutton, AK Haugerud, BM Prakash, APG Jun, B Cressler, JD Marshall, CJ Marshall, PW Ladbury, R Guarin, F Joseph, AJ TI A comparison of gamma and proton radiation effects in 200 GHz SiGeHBTs SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 42nd Annual Nuclear and Space Radiation Effects Conference (NSREC) CY JUL 11-15, 2005 CL Seattle, WA SP IEEE DE EB spacer; ELDRS; gamma radiation; proton radiation; radiation sources; SiGe; SiGeHBT; shallow trench isolation; technology scaling ID X-RAY; BIPOLAR-TRANSISTORS; GAIN DEGRADATION; MOS STRUCTURES; TECHNOLOGY; TOLERANCE; DEVICES; CO-60; IRRADIATIONS; ENVIRONMENTS AB We present the results of gamma irradiation on third-generation, 200 GHz SiGe HBTs. Pre- and post-radiation dc figures-of-merit are used to quantify the tolerance of the raised extrinsic base structure to Co-60 gamma rays for varying device geometries. Additionally, the impact of technology scaling on the observed radiation response is addressed through comparisons to second generation, 120 GHz SiGe HBTs. Comparisons to previous proton-induced degradation results in these 200 GHz SiGe HBTs are also made, and indicate that the STE isolation oxide of the device shows increased degradation following Co-60 irradiation. The EB spacer oxide, on the other hand, demonstrates increased susceptibility to proton damage. Low dose rate proton testing was also performed and indicate that although there is a proton dose rate effect present in these devices, it cannot fully explain the observed trends. Similar trends have previously been observed for buried oxides and isolation oxides in several MOS technologies and have been attributed to increased charge yield in these oxides for 1.2 MeV Co-60 gamma rays when compared to 63 MeV protons. C1 Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30308 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Muinez Engn, Houston, TX 77001 USA. IBM Microelect, Fishkill, NY 12533 USA. IBM Microelect, Essex Jct, VT 05452 USA. RP Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30308 USA. EM asutton@ece.gatech.edu RI A P, Gnana Prakash/G-8054-2012 NR 27 TC 30 Z9 31 U1 0 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2005 VL 52 IS 6 BP 2358 EP 2365 DI 10.1109/TNS.2005.860728 PN 1 PG 8 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 017LL UT WOS:000235695000046 ER PT J AU Oldham, TR Suhail, M Kuhn, P Prinz, E Kim, HS LaBel, KA AF Oldham, TR Suhail, M Kuhn, P Prinz, E Kim, HS LaBel, KA TI Effects of heavy ion exposure on nanocrystal nonvolatile memory SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 42nd Annual Nuclear and Space Radiation Effects Conference (NSREC) CY JUL 11-15, 2005 CL Seattle, WA SP IEEE DE component; electronics; nanocrystals; nonvolatile memory; radiation effects ID THIN GATE OXIDES; SPIN-RESONANCE EVIDENCE; BREAKDOWN; IRRADIATION; GENERATION; CELLS; TRAP AB Advanced nanocrystal nonvolatile memories have been exposed to heavy ion bombardment. They appear to be promising candidates for future spacecraft electronics. C1 QSS Inc, Seabrook, MD 20706 USA. Freescale Semicond, Technol Solut Org, Austin, TX 78735 USA. Jackson & Tull Chartered Engineers, Aerosp Engn Div, Greenbelt, MD 20771 USA. NASA, Goddard Space Flight Ctr, Radiat Effects & Anal Grp, Greenbelt, MD 20771 USA. RP Oldham, TR (reprint author), QSS Inc, Seabrook, MD 20706 USA. EM Timothy.Oldham@pop500.gsfc.nasa.gov; Ken.LaBel@nasa.gov NR 25 TC 8 Z9 9 U1 0 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2005 VL 52 IS 6 BP 2366 EP 2371 DI 10.1109/TNS.2005.860723 PN 1 PG 6 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 017LL UT WOS:000235695000047 ER PT J AU Grens, CM Haugerud, BM Sutton, AK Chen, TB Cressler, JD Marshall, PW Marshall, CJ Joseph, AJ AF Grens, CM Haugerud, BM Sutton, AK Chen, TB Cressler, JD Marshall, PW Marshall, CJ Joseph, AJ TI The effects of proton irradiation on the operating voltage constraints of SiGeHBTs SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 42nd Annual Nuclear and Space Radiation Effects Conference (NSREC) CY JUL 11-15, 2005 CL Seattle, WA SP IEEE DE breakdown voltage; proton irradiation; radiation hardness assurance; SiGeHBTs ID HETEROJUNCTION BIPOLAR-TRANSISTORS; TECHNOLOGY; RELIABILITY; TOLERANCE AB The effect of proton irradiation on operating voltage constraints in SiGe HBTs is investigated for the first time in 120 GHz and 200 GHz SiGe HBTs. A variety of operating bias conditions was examined during irradiation, including terminals grounded, terminals floating, and forward active (FA) bias operation. The excess base current degradation at 5.0 X 10(13) p/cm(2) was similar in all cases. BVCEO and BVCBO showed no significant signs of degradation with irradiation. We also investigated for the first time the impact of radiation on SiGe HBTs biased under so-called "unstable" conditions (i.e., operating point instabilities). In the case of unstable bias conditions, device degradation under proton exposure is significantly different than for stable bias, and bias conditions can play a significant role in the damage process, potentially raising issues from a hardness assurance perspective. C1 Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30308 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. IBM Microelect, Essex Jct, VT 05452 USA. RP Grens, CM (reprint author), Georgia Inst Technol, Sch Elect & Comp Engn, Atlanta, GA 30308 USA. EM cmgrens@ece.gatech.edu NR 14 TC 2 Z9 3 U1 0 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2005 VL 52 IS 6 BP 2403 EP 2407 DI 10.1109/TNS.2005.860700 PN 1 PG 5 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 017LL UT WOS:000235695000053 ER PT J AU Marshall, P Carts, M Currie, S Reed, R Randall, B Fritz, K Kennedy, K Berg, M Krithivasan, R Siedleck, C Ladbury, R Marshall, C Cressler, J Niu, GF LaBel, K Gilbert, B AF Marshall, P Carts, M Currie, S Reed, R Randall, B Fritz, K Kennedy, K Berg, M Krithivasan, R Siedleck, C Ladbury, R Marshall, C Cressler, J Niu, GF LaBel, K Gilbert, B TI Autonomous bit error rate testing at multi-gbit/s rates implemented in a 5AM SiGe circuit for radiation effects self test (CREST) SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 42nd Annual Nuclear and Space Radiation Effects Conference (NSREC) CY JUL 11-15, 2005 CL Seattle, WA SP IEEE DE built in self test; high speed bit error rate testing SiGe; single event effects (SEEs) ID HEAVY-ION; DIGITAL LOGIC AB SEE testing at multi-Gbit/s data rates has traditionally involved elaborate high speed test equipment setups for at-speed testing. We demonstrate a generally applicable self test circuit approach implemented in IBM's 5AM SiGe process, and describe its ability to capture complex error signatures during circuit operation at data rates exceeding 5 Gbit/s. Comparisons of data acquired with FPGA control of the CREST ASIC versus conventional bit error rate test equipment validate the approach. In addition, we describe SEE characteristics of the IBM 5AM process implemented in five variations of the D Hip-Hop based serial register. Heavy ion SEE data acquired at angles follow the traditional RPP-based analysis approach in one case, but deviate by orders on magnitude in others, even though all circuits are implemented in the same 5AM SiGe HBT process. C1 NASA, Brookneal, VA 24528 USA. Muniz Engn Inc, Houston, TX 77058 USA. Mayo Clin & Mayo Fdn, Rochester, MN 55905 USA. Vanderbilt Univ, Nashville, TN 37235 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Georgia Inst Technol, Atlanta, GA 30308 USA. Auburn Univ, Auburn, AL 36849 USA. RP Marshall, P (reprint author), NASA, Brookneal, VA 24528 USA. EM pwmarshall@aol.com RI Krithivasan, Ramkumar/D-3549-2011 NR 7 TC 44 Z9 44 U1 0 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2005 VL 52 IS 6 BP 2446 EP 2454 DI 10.1109/TNS.2005.860740 PN 1 PG 9 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 017LL UT WOS:000235695000060 ER PT J AU Rezgui, S Swift, G Somervill, K George, J Carn-Iichael, C Allen, G AF Rezgui, S Swift, G Somervill, K George, J Carn-Iichael, C Allen, G TI Complex upset mitigation applied to a re-configurable embedded processor SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 42nd Annual Nuclear and Space Radiation Effects Conference (NSREC) CY JUL 11-15, 2005 CL Seattle, WA SP IEEE DE embedded processors; field-programmable-gate-arrays (FPGAs); radiation testing AB Soft-core processors implemented in static random access memory-based field-programmable-gate-arrays, while attractive to spacecraft designers, require upset mitigation. We investigate a proposed solution involving two levels of scrubbing plus triple modular redundancy and measure its in-beam performance. C1 Xilinx Inc, San Jose, CA 95124 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. NASA, Langley Res Ctr, Elect Syst Branch, Hampton, VA 23681 USA. Aerosp Corp, El Segundo, CA 90245 USA. RP Xilinx Inc, San Jose, CA 95124 USA. EM sana.rezgui@xilinx.com; gary.m.swift@jpl.nasa.gov; kevin.m.somervill@nasa.gov; Jeffrey.s.george@aero.org NR 9 TC 6 Z9 6 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2005 VL 52 IS 6 BP 2468 EP 2474 DI 10.1109/TNS.2005.860743 PN 1 PG 7 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 017LL UT WOS:000235695000063 ER PT J AU Irom, F Miyahira, TF AF Irom, F Miyahira, TF TI Catastrophic latchup in a CMOS operational amplifier SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 42nd Annual Nuclear and Space Radiation Effects Conference (NSREC) CY JUL 11-15, 2005 CL Seattle, WA SP IEEE DE amplifier; cyclotron; heavy ion; latchup; LTC2052; SEE ID SINGLE-EVENT LATCHUP; INTEGRATED-CIRCUITS; DEVICES; TEMPERATURE AB We report catastrophic single-event latchup results for a CMOS operational amplifier. Thermal and optical imagings in conjunction with current distributions were used to identify latchup-sensitive regions. Differences in cross section for various ions show that charge is collected at depths beyond 40 mu m, causing the cross section to be underestimated unless long-range ions are used. Latchup testing with short-range ions may underestimate the cross section or even fail to trigger a latchup event that would occur with more energetic ions. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Irom, F (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM farokh.irom@jpl.nasa.gov; testsuo.f.miyahira@jpl.nasa.gov NR 16 TC 2 Z9 2 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2005 VL 52 IS 6 BP 2475 EP 2480 DI 10.1109/TNS.2005.860676 PN 1 PG 6 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 017LL UT WOS:000235695000064 ER PT J AU Shuler, RL Kouba, C O'Neill, PM AF Shuler, RL Kouba, C O'Neill, PM TI SEU performance of TAG based flip-flops SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 42nd Annual Nuclear and Space Radiation Effects Conference (NSREC) CY JUL 11-15, 2005 CL Seattle, WA SP IEEE DE single-event effects; soft errors AB We describe heavy-ion test results for two new single-event upset (SEU)-tolerant latches based on transition nand gates, one for single rail asynchronous and the other for dual rail synchronous designs, implemented in AMI 0.5 mu process. C1 NASA, Lyndon B Johnson Space Ctr, Avion Syst Div, Houston, TX 77058 USA. RP Shuler, RL (reprint author), NASA, Lyndon B Johnson Space Ctr, Avion Syst Div, Houston, TX 77058 USA. EM robert.l.shuler@nasa.gov; coy.kouba-1@nasa.gov; patrick.m.oneill@nasa.gov OI Shuler, Robert/0000-0002-6129-6867 NR 7 TC 12 Z9 13 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2005 VL 52 IS 6 BP 2550 EP 2553 DI 10.1109/TNS.2005.860712 PN 1 PG 4 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 017LL UT WOS:000235695000075 ER PT J AU Wroe, AJ Cornelius, IM Rosenfeld, AB Pisacane, VL Ziegler, JF Nelson, E Cucinotta, F Zaider, M Dicello, JF AF Wroe, AJ Cornelius, IM Rosenfeld, AB Pisacane, VL Ziegler, JF Nelson, E Cucinotta, F Zaider, M Dicello, JF TI Microdosimetry simulations of solar protons within a spacecraft SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 42nd Annual Nuclear and Space Radiation Effects Conference (NSREC) CY JUL 11-15, 2005 CL Seattle, WA SP IEEE DE GEANT4; microdosimetry; protons ID BEAMS AB The microdosimetric spectra derived by silicon microdosimeter in a proton radiation field traversing heterogeneous structures were simulated using the GEANT4 toolkit. C1 Univ Wollongong, Ctr Med Radiat Phys, Wollongong, NSW 2087, Australia. USN Acad, Annapolis, MD 21402 USA. NASA, Radiat Res Dept, Houston, TX USA. Mem Sloan Kettering Canc Ctr, Dept Med Phys, New York, NY 10021 USA. Johns Hopkins Univ, Sch Med, Baltimore, MD USA. RP Wroe, AJ (reprint author), Univ Wollongong, Ctr Med Radiat Phys, Wollongong, NSW 2087, Australia. EM ajw16@uow.edu.au; iwan@uow.edu.au; anatoly@uow.edu.au; pisacane@usna.edu; ziegler@aya.yale.edu; nelson@usna.edu; francis.a.cucinotta@nasa.gov; zaiderm@mskcc.org; diceljo@jhmi.edu RI Rosenfeld, Anatoly/D-1989-2014; OI Zaider, Marco/0000-0002-5113-7862 NR 15 TC 7 Z9 7 U1 0 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2005 VL 52 IS 6 BP 2591 EP 2596 DI 10.1109/TNS.2005.860706 PN 1 PG 6 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 017LL UT WOS:000235695000081 ER PT J AU Ladbury, R Gorelick, JL AF Ladbury, R Gorelick, JL TI Statistical methods for large flight lots and ultra-high reliability applications SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 42nd Annual Nuclear and Space Radiation Effects Conference (NSREC) CY JUL 11-15, 2005 CL Seattle, WA SP IEEE DE probability; quality assurance; radiation effects; reliability estimation; statistics ID HARDNESS ASSURANCE AB We present statistical techniques for evaluating random and systematic errors for use in flight performance predictions for large flight lots and ultra-high reliability applications. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Boeing Space & Intelligent Syst, Los Angeles, CA 90009 USA. RP Ladbury, R (reprint author), NASA, Goddard Space Flight Ctr, Code 661, Greenbelt, MD 20771 USA. EM Raymond.L.Ladbury@nasa.gov; jerry.l.gorelick@boeing.com NR 7 TC 7 Z9 7 U1 0 U2 3 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2005 VL 52 IS 6 BP 2630 EP 2637 DI 10.1109/TNS.2005.861080 PN 1 PG 8 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 017LL UT WOS:000235695000087 ER PT J AU Johnston, AH Miyahira, TF AF Johnston, AH Miyahira, TF TI Hardness assurance methods for radiation degradation of optocouplers SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 42nd Annual Nuclear and Space Radiation Effects Conference (NSREC) CY JUL 11-15, 2005 CL Seattle, WA SP IEEE DE hardness assurance; light-emitting diode (LED); optocoupler; space radiation ID LIGHT-EMITTING-DIODES; PROTON DAMAGE; ENERGY-DEPENDENCE; GAAS LEDS AB Hardness assurance methods are examined for several types of optocouplers. A new diagnostic method using reverse-recovery time has a strong correlation with damage in the internal light emitting diode (LED). It depends only on electrical measurements, and can be used as a first-order parameter to determine LED properties when the LED technology of the optocoupler is unknown, as well as for evaluating unit and lot variability. For devices with internal LEDs that are highly sensitive to displacement damage, the dependence of phototransistor gain on operating conditions can impact post-radiation performance. For devices with radiation-tolera nt LEDs, phototransistor characteristics and gain degradation are both important in determining the net effect of displacement damage. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Miyahira, TF (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 11 TC 8 Z9 9 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2005 VL 52 IS 6 BP 2649 EP 2656 DI 10.1109/TNS.2005.860733 PN 1 PG 8 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 017LL UT WOS:000235695000090 ER PT J AU Pickel, JC Reed, RA Ladbury, R Marshall, PW Jordan, TM Gee, G Fodness, B McKelvey, M McMurray, R Ennico, K McCreight, C Waczynski, A Polidan, EJ Johnson, SD Weller, RA Mendenhall, MH Schrimpf, RD AF Pickel, JC Reed, RA Ladbury, R Marshall, PW Jordan, TM Gee, G Fodness, B McKelvey, M McMurray, R Ennico, K McCreight, C Waczynski, A Polidan, EJ Johnson, SD Weller, RA Mendenhall, MH Schrimpf, RD TI Transient radiation effects in ultra-low noise HgCdTeIR detector arrays for space-based astronomy SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 42nd Annual Nuclear and Space Radiation Effects Conference (NSREC) CY JUL 11-15, 2005 CL Seattle, WA SP IEEE DE HgCdTe; IR detectors; single event transients; space-based astronomy; transient noise AB We present measurements of proton-induced single event transients in ultra-low noise HgCdTe IR detector arrays being developed for space-based astronomy and compare to modeling results. C1 PR&T Inc, Fallbrook, CA 92028 USA. Vanderbilt Univ, Nashville, TN 37203 USA. Orbital Sci Corp, Mclean, VA 22102 USA. NASA, Goddard Space Flight Ctr, SGT, Greenbelt, MD 20770 USA. EMP Consultants, Greenbelt, MD 20770 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. NASA, Goddard Space Flight Ctr, GST, Greenbelt, MD 20770 USA. RP PR&T Inc, Fallbrook, CA 92028 USA. EM jim@pickel.net RI Schrimpf, Ronald/L-5549-2013; Ennico, Kimberly/L-9606-2014 OI Schrimpf, Ronald/0000-0001-7419-2701; NR 9 TC 5 Z9 5 U1 0 U2 2 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0018-9499 EI 1558-1578 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2005 VL 52 IS 6 BP 2657 EP 2663 DI 10.1109/TNS.2005.860732 PN 1 PG 7 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 017LL UT WOS:000235695000091 ER PT J AU Marshall, CJ Marshall, PW Waczynski, A Polidan, EJ Johnson, SD Kimble, RA Reed, RA Delo, G Schlossberg, D Russell, AM Beck, T Wen, Y Yagelowich, J Hill, RJ AF Marshall, CJ Marshall, PW Waczynski, A Polidan, EJ Johnson, SD Kimble, RA Reed, RA Delo, G Schlossberg, D Russell, AM Beck, T Wen, Y Yagelowich, J Hill, RJ TI Hot pixel annealing behavior in CCDs irradiated at-84 degrees C SO IEEE TRANSACTIONS ON NUCLEAR SCIENCE LA English DT Article; Proceedings Paper CT 42nd Annual Nuclear and Space Radiation Effects Conference (NSREC) CY JUL 11-15, 2005 CL Seattle, WA SP IEEE DE CCDs; displacement damage; hot pixels; radiation effects ID SILICON DEVICES; DARK CURRENT; DAMAGE; TRANSIENT; EXTREMES AB A Hubble space telescope wide field camera 3 e2v CCD was irradiated while operating at -84 degrees C and the dark current studied as a function of temperature while the charge coupled device was warmed to a sequence of temperatures up to a maximum of +30 degrees C. The device was then cooled back down to -84 degrees and remeasured. Hot pixel populations were tracked during the warm up and cool down. Hot pixel annealing began below -40 degrees C and the anneal process was largely completed by the time the detector reached +20 degrees C. There was no apparent sharp annealing temperature. Although a large fraction of the hot pixels fell below the threshold to be counted as a hot pixel, they nevertheless sustained a higher leakage rate than the remaining population. The mechanism for hot pixel annealing is not presently understood. Room temperature irradiations do not adequately characterize the hot pixel distributions for cooled applications. C1 NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Global Sci & Technol, Greenbelt, MD 20771 USA. Vanderbilt Univ, Nashville, TN 37235 USA. Sigma, Greenbelt, MD 20771 USA. SSAI, Greenbelt, MD 20771 USA. RP Marshall, CJ (reprint author), NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. EM cmarshall2@aol.com RI Kimble, Randy/D-5317-2012 NR 16 TC 13 Z9 13 U1 0 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855 USA SN 0018-9499 J9 IEEE T NUCL SCI JI IEEE Trans. Nucl. Sci. PD DEC PY 2005 VL 52 IS 6 BP 2672 EP 2677 DI 10.1109/TNS.2005.860731 PN 1 PG 6 WC Engineering, Electrical & Electronic; Nuclear Science & Technology SC Engineering; Nuclear Science & Technology GA 017LL UT WOS:000235695000093 ER PT J AU Jefferts, SR Shirley, JH Ashby, N Burt, EA Dick, GJ AF Jefferts, SR Shirley, JH Ashby, N Burt, EA Dick, GJ TI Power dependence of distributed cavity phase-induced frequency biases in atomic fountain frequency standards SO IEEE TRANSACTIONS ON ULTRASONICS FERROELECTRICS AND FREQUENCY CONTROL LA English DT Article ID CESIUM FOUNTAIN; ACCURACY EVALUATION; MICROWAVE CAVITIES; UNCERTAINTY; SHIFTS; PTB AB We discuss the implications of using high-power microwave tests in a fountain frequency standard to measure the frequency bias resulting from distributed cavity-phase shifts. We develop a theory which shows that the frequency bias from distributed cavity phase depends on the amplitude of the microwave field within the cavity. The dependence leads to the conclusion that the frequency bias associated with the distributed cavity phase is typically both misestimated and counted twice within the error budget of fountain frequency standards. C1 Natl Inst Stand & Technol, Div Time & Frequency, Boulder, CO 80305 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Jefferts, SR (reprint author), Natl Inst Stand & Technol, Div Time & Frequency, Boulder, CO 80305 USA. EM jefferts@boulder.nist.gov NR 25 TC 25 Z9 25 U1 0 U2 4 PU IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC PI PISCATAWAY PA 445 HOES LANE, PISCATAWAY, NJ 08855-4141 USA SN 0885-3010 J9 IEEE T ULTRASON FERR JI IEEE Trans. Ultrason. Ferroelectr. Freq. Control PD DEC PY 2005 VL 52 IS 12 BP 2314 EP 2321 DI 10.1109/TUFFC.2005.1563276 PG 8 WC Acoustics; Engineering, Electrical & Electronic SC Acoustics; Engineering GA 999OI UT WOS:000234398700018 PM 16463499 ER PT J AU Brower, LP Fink, LS Ramirez, LR Weiss, SB Slayback, D Perault, DR AF Brower, LP Fink, LS Ramirez, LR Weiss, SB Slayback, D Perault, DR TI The physiological ecology of overwintering monarch butterflies SO INTEGRATIVE AND COMPARATIVE BIOLOGY LA English DT Meeting Abstract CT Annual Meeting of the Society-for-Integrative-and-Comparative-Biology CY JAN 04-08, 2006 CL Orlando, FL C1 Sweet Briar Coll, Sweet Briar, VA 24595 USA. Univ Nacl Autonoma Mexico, Mexico City 04510, DF, Mexico. NASA, Goddard Space Flight Ctr, Creekside Ctr Earth Observat, Greenbelt, MD 20771 USA. Lynchburg Coll, Lynchburg, VA 24501 USA. EM brower@sbc.edu RI Slayback, Daniel/E-7465-2011 NR 0 TC 0 Z9 0 U1 1 U2 3 PU OXFORD UNIV PRESS INC PI CARY PA JOURNALS DEPT, 2001 EVANS RD, CARY, NC 27513 USA SN 1540-7063 J9 INTEGR COMP BIOL JI Integr. Comp. Biol. PD DEC PY 2005 VL 45 IS 6 BP 970 EP 970 PG 1 WC Zoology SC Zoology GA 012KH UT WOS:000235337600065 ER PT J AU Wang, P Song, YT Chao, Y Zhang, HC AF Wang, P Song, YT Chao, Y Zhang, HC TI Parallel computation of the Regional Ocean Modeling System SO INTERNATIONAL JOURNAL OF HIGH PERFORMANCE COMPUTING APPLICATIONS LA English DT Article DE regional ocean modeling; parallelization; scalability; performance AB The Regional Ocean Modeling System (ROMS) is a regional ocean general circulation modeling system solving the free surface, hydrostatic, primitive equations over varying topography. It is free software distributed worldwide for studying both complex coastal ocean problems and the basin-to-global scale ocean circulation. The original ROMS code could only be run on shared-memory systems. With the increasing need to simulate larger model domains with finer resolutions and on a variety of computer platforms, there is a need in the ocean-modeling community to have a ROMS code that can be run on any parallel computer ranging from 10 to hundreds of processors. Recently, we have explored parallelization for ROMS using the Message-Passing Interface (MPI) programming model. In this paper, we present an efficient parallelization strategy for such a large-scale scientific software package, based on an existing shared-memory computing model. In addition, we discuss scientific applications and clata-performance issues on a couple of SGI systems, including Columbia, the world's third-fastest supercomputer. C1 Lawrence Livermore Natl Lab, Livermore, CA 94551 USA. CALTECH, Jet Propuls Lab, Pasadena, CA 91125 USA. Raytheon ITSS, Pasadena, CA USA. RP Wang, P (reprint author), Lawrence Livermore Natl Lab, Livermore, CA 94551 USA. EM WANG32@LLNL.GOV NR 12 TC 18 Z9 19 U1 0 U2 3 PU SAGE PUBLICATIONS LTD PI LONDON PA 1 OLIVERS YARD, 55 CITY ROAD, LONDON EC1Y 1SP, ENGLAND SN 1094-3420 J9 INT J HIGH PERFORM C JI Int. J. High Perform. Comput. Appl. PD WIN PY 2005 VL 19 IS 4 BP 375 EP 385 DI 10.1177/1094342005059115 PG 11 WC Computer Science, Hardware & Architecture; Computer Science, Interdisciplinary Applications; Computer Science, Theory & Methods SC Computer Science GA 982XE UT WOS:000233194400003 ER PT J AU Jones, JA Jennings, R Pietryzk, R Ciftcioglu, N Stepaniak, P AF Jones, JA Jennings, R Pietryzk, R Ciftcioglu, N Stepaniak, P TI Genitourinary issues during spaceflight: a review SO INTERNATIONAL JOURNAL OF IMPOTENCE RESEARCH LA English DT Review DE spaceflight; genitourinary; reproduction; calculi; urinary retention AB The genitourinary (GU) system is not uncommonly affected during previous spaceflights. GU issues that have been observed during spaceflight include urinary calculi, infections, retention, waste management, and reproductive. In-flight countermeasures for each of these issues are being developed to reduce the likelihood of adverse sequelae, due to GU issues during exploration-class spaceflight, to begin in 2018 with flights back to the Moon and on to Mars, according to the February 2004 Presendent's Vision for US Space Exploration. With implementation of a robust countermeasures program, GU issues should not have a significant threat for mission impact during future spaceflights. C1 NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Univ Texas, Med Branch, Galveston, TX 77550 USA. MS Enterprise Advisory Serv Inc, Houston, TX USA. Nanobac Life Sci Inc, Tampa, FL USA. RP Jones, JA (reprint author), NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. NR 9 TC 14 Z9 14 U1 0 U2 0 PU NATURE PUBLISHING GROUP PI LONDON PA MACMILLAN BUILDING, 4 CRINAN ST, LONDON N1 9XW, ENGLAND SN 0955-9930 J9 INT J IMPOT RES JI Int. J. Impot. Res. PD DEC PY 2005 VL 17 SU 1 BP S64 EP S67 DI 10.1038/sj.ijir.3901431 PG 4 WC Urology & Nephrology SC Urology & Nephrology GA 010KO UT WOS:000235193800011 PM 16391546 ER PT J AU Simpanya, MF Ansari, RR Suh, KI Leverenz, VR Giblin, FJ AF Simpanya, MF Ansari, RR Suh, KI Leverenz, VR Giblin, FJ TI Aggregation of lens crystallins in an in vivo hyperbaric oxygen guinea pig model of nuclear cataract: Dynamic light-scattering and HPLC analysis SO INVESTIGATIVE OPHTHALMOLOGY & VISUAL SCIENCE LA English DT Article ID HIGH-MOLECULAR-WEIGHT; RAY-INDUCED CATARACT; LIVING HUMAN LENS; ALPHA-CRYSTALLIN; RABBIT LENSES; PROTEIN DIFFUSIVITY; CYTOPLASMIC TEXTURE; INVIVO OBSERVATION; FOURIER-ANALYSIS; CROSS-LINKING AB PURPOSE. The role of oxygen in the formation of lens high-molecular-weight (HMW) protein aggregates during the development of human nuclear cataract is not well understood. The purpose of this study was to investigate lens crystallin aggregate formation in hyperbaric oxygen (HBO)- treated guinea pigs by using in vivo and in vitro methods. METHODS. Guinea pigs were treated three times weekly for 7 months with HBO, and lens crystallin aggregation was investigated in vivo with the use of dynamic light-scattering (DLS) and in vitro by HPLC analysis of water-insoluble (WI) proteins. DLS measurements were made every 0.1 mm across the 4.5- to 5.0-mm optical axis of the guinea pig lens. RESULTS. The average apparent diameter of proteins in the nucleus ( the central region) of lenses of HBO-treated animals was nearly twice that of the control animals ( P < 0.001). Size distribution analysis conducted at one selected point in the nucleus and cortex ( the outer periphery of the lens) after dividing the proteins into small-diameter and large-diameter groups, showed in the O-2-treated nucleus a threefold increase in intensity ( P < 0.001) and a doubling in apparent size ( P = 0.03) of large-diameter aggregate proteins, compared with the same control group. No significant changes in apparent protein diameter were detected in the O-2-treated cortex, compared with the control. The average diameter of protein aggregates at the single selected location in the O-2-treated nucleus was estimated to be 150 nm, a size capable of scattering light and similar to the size of aggregates found in human nuclear cataracts. HPLC analysis indicated that one half of the experimental nuclear WI protein fraction ( that had been dissolved in guanidine) consisted of disulfide cross-linked 150- to 1000-kDa aggregates, not present in the control. HPLC-isolated aggregates contained alpha A-, beta-, gamma-, and zeta-crystallins, but not alpha B-crystallin, which is devoid of - SH groups and thus does not participate in disulfide cross-linking. All zeta-crystallin present in the nuclear WI fraction appeared to be there as a result of disulfide cross-linking. CONCLUSIONS. The results indicate that molecular oxygen in vivo can induce the cross-linking of guinea pig lens nuclear crystallins into large disulfide-bonded aggregates capable of scattering light. A similar process may be involved in the formation of human nuclear cataract. C1 Oakland Univ, Eye Res Inst, Rochester, MI 48309 USA. NASA, Glenn Res Ctr, Cleveland, OH USA. RP Oakland Univ, Eye Res Inst, Rochester, MI 48309 USA. EM giblin@oakland.edu FU NEI NIH HHS [EY014803, EY02027, R01 EY002027, R24 EY014803] NR 83 TC 38 Z9 43 U1 2 U2 5 PU ASSOC RESEARCH VISION OPHTHALMOLOGY INC PI ROCKVILLE PA 12300 TWINBROOK PARKWAY, ROCKVILLE, MD 20852-1606 USA SN 0146-0404 EI 1552-5783 J9 INVEST OPHTH VIS SCI JI Invest. Ophthalmol. Vis. Sci. PD DEC PY 2005 VL 46 IS 12 BP 4641 EP 4651 DI 10.1167/iovs.05-0843 PG 11 WC Ophthalmology SC Ophthalmology GA 988FV UT WOS:000233578600043 PM 16303961 ER PT J AU Arepalli, S Fireman, H Huffman, C Moloney, P Nikolaev, P Yowell, L Higgins, CD Kim, K Kohl, PA Turano, SP Ready, WJ AF Arepalli, S Fireman, H Huffman, C Moloney, P Nikolaev, P Yowell, L Higgins, CD Kim, K Kohl, PA Turano, SP Ready, WJ TI Carbon-nanotube-based electrochemical double-layer capacitor technologies for spaceflight applications SO JOM LA English DT Article ID SUPERCAPACITORS; ELECTRODES; OXIDE AB Electrochemical double layer capacitors or supercapacitors, have tremendous potential as high-power energy sources for use in low-weight hybrid systems for space exploration. Electrodes based on single-wall carbon nanotubes (SWCNTs) offer exceptional power and energy performance due to the high surface area, high conductivity, and the ability to functionalize the SWCNTs to optimize capacitor properties. This paper will report on the preparation of electrochemical capacitors incorporating SWCNT electrodes and their performance compared with existing commercial technology. Preliminary results indicate that substantial increases in power and energy density are possible. The effects of nanotube growth and processing methods on electrochemical capacitor performance is also presented. The compatibility of different SWCNTs and electrolytes was studied by varying the type of electrolyte ions that accumulate on the high-surface-area electrodes. C1 Georgia Tech Res Inst, Atlanta, GA 30332 USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. RP Ready, WJ (reprint author), Georgia Tech Res Inst, 925 Dalney St, Atlanta, GA 30332 USA. EM jud.ready@gtri.gatech.edu RI Arepalli, Sivaram/A-5372-2010; Nikolaev, Pavel/B-9960-2009 NR 28 TC 20 Z9 20 U1 0 U2 7 PU SPRINGER PI NEW YORK PA 233 SPRING ST, NEW YORK, NY 10013 USA SN 1047-4838 J9 JOM-US JI JOM PD DEC PY 2005 VL 57 IS 12 BP 26 EP 31 DI 10.1007/s11837-005-0179-x PG 6 WC Materials Science, Multidisciplinary; Metallurgy & Metallurgical Engineering; Mineralogy; Mining & Mineral Processing SC Materials Science; Metallurgy & Metallurgical Engineering; Mineralogy; Mining & Mineral Processing GA 996PF UT WOS:000234185800003 ER PT J AU Arzoumanian, Z Holmberg, J Norman, B AF Arzoumanian, Z Holmberg, J Norman, B TI An astronomical pattern-matching algorithm for computer-aided identification of whale sharks Rhincodon typus SO JOURNAL OF APPLIED ECOLOGY LA English DT Article DE conservation; marine and fisheries management; mark-recapture; photographic identification; population studies ID FISH AB 1. The formulation of conservation policy relies heavily on demographic, biological and ecological knowledge that is often elusive for threatened species. Essential estimates of abundance, survival and life-history parameters are accessible through mark and recapture studies given a sufficiently large sample. Photographic identification of individuals is an established mark and recapture technique, but its full potential has rarely been exploited because of the unmanageable task of making visual identifications in large data sets. 2. We describe a novel technique for identifying individual whale sharks Rhincodon typus through numerical pattern matching of their natural surface 'spot' colourations. Together with scarring and other markers, spot patterns captured in photographs of whale shark flanks have been used, in the past, to make identifications by eye. We have automated this process by adapting a computer algorithm originally developed in astronomy for the comparison of star patterns in images of the night sky. 3. In tests using a set of previously identified shark images, our method correctly matched pairs exhibiting the same pattern in more than 90% of cases. From a larger library of previously unidentified images, it has to date produced more than 100 new matches. Our technique is robust in that the incidence of false positives is low, while failure to match images of the same shark is predominantly attributable to foreshortening in photographs obtained at oblique angles of more than 30 degrees. 4. We describe our implementation of the pattern-matching algorithm, estimates of its efficacy, its incorporation into the new ECOCEAN Whale Shark Photo-identification Library, and prospects for its further refinement. We also comment on the biological and conservation implications of the capability of identifying individual sharks across wide geographical and temporal spans. 5. Synthesis and applications. An automated photo-identification technique has been developed that allows for efficient 'virtual tagging' of spotted animals. The pattern-matching software has been implemented within a Web-based library created for the management of generic encounter photographs and derived data. The combined capabilities have demonstrated the reliability of whale shark spot patterns for long-term identifications, and promise new ecological insights. Extension of the technique to other species is anticipated, with attendant benefits to management and conservation through improved understanding of life histories, population trends and migration routes, as well as ecological factors such as exploitation impact and the effectiveness of wildlife reserves. C1 NASA, Univ Space Res Assoc, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA. Murdoch Univ, Ctr Fish & Fisheries Res, ECOCEAN, Murdoch, WA 6150, Australia. RP Arzoumanian, Z (reprint author), NASA, Univ Space Res Assoc, Goddard Space Flight Ctr, Greenbelt, MD 20770 USA. EM zaven@milkyway.gsfc.nasa.gov NR 21 TC 111 Z9 126 U1 4 U2 47 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0021-8901 J9 J APPL ECOL JI J. Appl. Ecol. PD DEC PY 2005 VL 42 IS 6 BP 999 EP 1011 DI 10.1111/j.1365-2664.2005.01117.x PG 13 WC Biodiversity Conservation; Ecology SC Biodiversity & Conservation; Environmental Sciences & Ecology GA 987JW UT WOS:000233515200001 ER PT J AU Baum, BA Heymsfield, AJ Yang, P Bedka, ST AF Baum, BA Heymsfield, AJ Yang, P Bedka, ST TI Bulk scattering properties for the remote sensing of ice clouds. Part I: Microphysical data and models SO JOURNAL OF APPLIED METEOROLOGY LA English DT Article ID NATURAL CLOUDS; CIRRUS; CRYSTALS; PARAMETERIZATIONS AB This study reports on the use of in situ data obtained in midlatitude and tropical ice clouds from airborne sampling probes and balloon-borne replicators as the basis for the development of bulk scattering models for use in satellite remote sensing applications. Airborne sampling instrumentation includes the two-dimensional cloud (2D-C), two-dimensional precipitation (2D-P), high-volume precipitation spectrometer (HVPS), cloud particle imager (CPI), and NCAR video ice particle sampler (VIPS) probes. Herein the development of a comprehensive set of microphysical models based on in situ measurements of particle size distributions (PSDs) is discussed. Two parameters are developed and examined: ice water content (IWC) and median mass diameter D-m. Comparisons are provided between the IWC and D-m values derived from in situ measurements obtained during a series of field campaigns held in the midlatitude and tropical regions and those calculated from a set of modeled ice particles used for light-scattering calculations. The ice particle types considered in this study include droxtals, hexagonal plates, solid columns, hollow columns, aggregates, and D bullet rosettes. It is shown that no single habit accurately replicates the derived IWC and D-m values, but a mixture of habits can significantly improve the comparison of these bulk microphysical properties. In addition, the relationship between D-m and the effective particle size D-eff, defined as 1.5 times the ratio of ice particle volume to projected area for a given PSD, is investigated. Based on these results, a subset of microphysical models is chosen as the basis for the development of ice cloud bulk scattering models in Part II of this study. C1 NASA, Langley Res Ctr, Hampton, VA 23665 USA. Natl Ctr Atmospher Res, Boulder, CO 80307 USA. Texas A&M Univ, College Stn, TX USA. Cooperat Inst Meteorol Satellite Studies, Madison, WI USA. RP Baum, BA (reprint author), NASA, LaRC, 1225 W Dayton St, Madison, WI 53706 USA. EM bryan.baum@ssec.wisc.edu RI Yang, Ping/B-4590-2011; Baum, Bryan/B-7670-2011; Heymsfield, Andrew/E-7340-2011 OI Baum, Bryan/0000-0002-7193-2767; NR 21 TC 176 Z9 183 U1 3 U2 17 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8763 J9 J APPL METEOROL JI J. Appl. Meteorol. PD DEC PY 2005 VL 44 IS 12 BP 1885 EP 1895 DI 10.1175/JAM2308.1 PG 11 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 005EI UT WOS:000234805000008 ER PT J AU Baum, BA Yang, P Heymsfield, AJ Platnick, S King, MD Hu, YX Bedka, ST AF Baum, BA Yang, P Heymsfield, AJ Platnick, S King, MD Hu, YX Bedka, ST TI Bulk scattering properties for the remote sensing of ice clouds. Part II: Narrowband models SO JOURNAL OF APPLIED METEOROLOGY LA English DT Article ID SINGLE-SCATTERING; LIGHT-SCATTERING; CRYSTALS; CIRRUS; MODIS; WATER; PHASE AB This study examines the development of bulk single-scattering properties of ice clouds, including single-scattering albedo, asymmetry factor, and phase function, for a set of 1117 particle size distributions obtained from analysis of the First International Satellite Cloud Climatology Project Regional Experiment (FIRE)-I, FIRE-II, Atmospheric Radiation Measurement Program intensive observation period, Tropical Rainfall Measuring Mission Kwajalein Experiment (KWAJEX), and the Cirrus Regional Study of Tropical Anvils and Cirrus Layers (CRYSTAL) Florida Area Cirrus Experiment (FACE) data. The primary focus is to develop band-averaged models appropriate for use by the Moderate Resolution Imaging Spectroradiometer (MODIS) imager on the Earth Observing System Terra and Aqua platforms, specifically for bands located at wavelengths of 0.65, 1.64, 2.13, and 3.75 mu m. The results indicate that there are substantial differences in the bulk scattering properties of ice clouds formed in areas of deep convection and those that exist in areas of much lower updraft velocities. Band-averaged bulk scattering property results obtained from a particle-size-dependent mixture of ice crystal habits are compared with those obtained assuming only solid hexagonal columns. The single-scattering albedo is lower for hexagonal columns than for a habit mixture for the 1.64-, 2.13-, and 3.75-gm bands, with the differences increasing with wavelength. In contrast, the asymmetry factors obtained from the habit mixture and only the solid hexagonal column are most different at 0.65 mu m, with the differences decreasing as wavelength increases. At 3.75 Am, the asymmetry factor results from the two habit assumptions are almost indistinguishable. The asymmetry factor, single-scattering albedo, and scattering phase functions are also compared with the MODIS version-1 (V1) models. Differences between the current and V1 models can be traced to the microphysical models and specifically to the number of both the smallest and the largest particles assumed in the size distributions. C1 NASA, Langley Res Ctr, Hampton, VA 23665 USA. Texas A&M Univ, College Stn, TX USA. Natl Ctr Atmospher Res, Boulder, CO 80307 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Cooperat Inst Meteorol Satellite Studies, Madison, WI USA. RP Baum, BA (reprint author), NASA, LaRC, 1225 W Dayton St, Madison, WI 53706 USA. EM bryan.baum@ssec.wisc.edu RI Yang, Ping/B-4590-2011; Baum, Bryan/B-7670-2011; Heymsfield, Andrew/E-7340-2011; King, Michael/C-7153-2011; Platnick, Steven/J-9982-2014; Hu, Yongxiang/K-4426-2012 OI Baum, Bryan/0000-0002-7193-2767; King, Michael/0000-0003-2645-7298; Platnick, Steven/0000-0003-3964-3567; NR 21 TC 167 Z9 169 U1 3 U2 11 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8763 J9 J APPL METEOROL JI J. Appl. Meteorol. PD DEC PY 2005 VL 44 IS 12 BP 1896 EP 1911 DI 10.1175/JAM2309.1 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 005EI UT WOS:000234805000009 ER PT J AU Goebel, DM Jameson, KK Watkins, RM Katz, I Mikellides, IG AF Goebel, DM Jameson, KK Watkins, RM Katz, I Mikellides, IG TI Hollow cathode theory and experiment. I. Plasma characterization using fast miniature scanning probes SO JOURNAL OF APPLIED PHYSICS LA English DT Article ID IONS AB A detailed study of the spatial variation of plasma density, temperature, and potential in hollow cathodes using miniature fast scanning probes has been undertaken in order to better understand the cathode operation and to provide benchmark data for the modeling of the cathode performance and life described in a companion paper. Profiles are obtained throughout the discharge and in the very high-density orifice region by pneumatically driven Langmuir probes, which are inserted directly into the hollow cathode orifice from either the upstream insert region inside the hollow cathode or from the downstream anode-plasma region. A fast transverse-scanning probe is also used to provide radial profiles of the cathode plume as a function of position from the cathode exit. The probes are extremely small to avoid perturbing the plasma; the ceramic tube insulator is 0.05 cm in diameter with a probe tip area of 0.002 cm(2). A series of current-voltage characteristics are obtained by applying a rapid sawtooth voltage wave form to the probe as it is scanned through the plasma at speeds of up to 2 m/s to produce the profiles with a spatial resolution of about 0.05 cm. At discharge currents of 10-25 A from the 1.5-cm-diameter hollow cathode, the plasma density inside the cathode is found to exceed 10(14) cm(-3), with the peak density occurring upstream of the orifice. The plasma potentials on axis inside the cathode are found to be in the 10-20 V range with electron temperatures of 2-5 eV, depending on the discharge current and gas flow rate. A potential discontinuity or double layer of less than 10 V is observed in the orifice region, and under certain conditions appears in the bright "plasma ball" in front of the cathode. This structure tends to change location and magnitude with discharge current, gas flow, and orifice size. A potential maximum proposed in the literature to exist in or near the cathode orifice is not observed. Instead, the plasma potential increases from the orifice exit both radially and axially over several centimeters to values of 5-10 V above the anode voltage. The potential and temperature profiles inside the cathode are insensitive to anode configuration changes that alter the discharge voltage at a given flow. Application of an axial magnetic-field characteristic of the cathode region found in ring-cusp ion thrusters increases the plasma density in the cathode plume, but does not significantly change the potential or temperature. Measurements of the plasma profiles and the internal cathode parameters for a hollow cathode operating at discharge currents of up to 25 A in xenon are shown and discussed. (c) 2005 American Institute of Physics. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Goebel, DM (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM dan.m.goebel@jpl.nasa.gov NR 20 TC 28 Z9 28 U1 2 U2 12 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-8979 J9 J APPL PHYS JI J. Appl. Phys. PD DEC 1 PY 2005 VL 98 IS 11 AR 113302 DI 10.1063/1.2135417 PG 9 WC Physics, Applied SC Physics GA 995QT UT WOS:000234119600005 ER PT J AU Mikellides, IG Katz, I Goebel, DM Polk, JE AF Mikellides, IG Katz, I Goebel, DM Polk, JE TI Hollow cathode theory and experiment. II. A two-dimensional theoretical model of the emitter region SO JOURNAL OF APPLIED PHYSICS LA English DT Article ID CROSS-SECTIONS; EMISSION; PLASMA AB Despite their long history and wide range of applicability that includes electric propulsion, detailed understanding of the driving physics inside orificed hollow cathodes remains elusive. The theoretical complexity associated with the multicomponent fluid inside the cathode, and the difficulty of accessing empirically this region, have limited our ability to design cathodes that perform better and last longer. A two-dimensional axisymmetric theoretical model of the multispecies fluid inside an orificed hollow cathode is presented. The level of detail attained by the model is allowed by its extended system of governing equations not solved for in the past within the hollow cathode. Such detail is motivated in part by the need to quantify the effect(s) of the plasma on the emitter life, and by the need to build the foundation for future modeling that will assess erosion of the keeper plate. Results from numerical simulations of a 1.2-cm-diam cathode operating at a discharge current of 25 A and a gas flow rate of 5 SCCM show that approximately 10 A of electron current, and 3.45 A of ion current return back to the emitter surface. The total emitted electron current is 33.8 A and the peak emitter temperature is found to be 1440 K. Comparisons with the measurements suggest that anomalous heating of the plasma is possible near the orifice region. The model predicts heavy species temperatures as high as 2034 K and peak voltage drops near the emitting surface not exceeding 8 V. (c) 2005 American Institute of Physics. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Mikellides, IG (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM ioannis.g.mikellides@jpl.nasa.gov; dan.m.goebel@jpl.nasa.gov NR 31 TC 29 Z9 29 U1 3 U2 17 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0021-8979 J9 J APPL PHYS JI J. Appl. Phys. PD DEC 1 PY 2005 VL 98 IS 11 AR 113303 DI 10.1063/1.2135409 PG 14 WC Physics, Applied SC Physics GA 995QT UT WOS:000234119600006 ER PT J AU Pandey, JC Singh, KP Drake, SA Sagar, R AF Pandey, JC Singh, KP Drake, SA Sagar, R TI Unravelling the nature of HD 81032 - A new RS CVn binary SO JOURNAL OF ASTROPHYSICS AND ASTRONOMY LA English DT Article DE star-X-ray; star-variable; star-late-type; star-HD 81032 ID CHROMOSPHERICALLY ACTIVE STARS; EINSTEIN SLEW SURVEY; X-RAY-EMISSION; ALL-SKY SURVEY; CANUM-VENATICORUM; BV PHOTOMETRY; CATALOG; SYSTEMS; SOLAR AB BVR photometric and quasi-simultaneous optical spectroscopic observations of the star HD 81032 have been carried out during the years 2000-2004. A photometric period of 18.802 +/- 0.07d has been detected for this star. A large group of spots with a migration period of 7.43 +/- 0.07 years is inferred from the first three years of the data. H alpha and CaII H and K emissions from the star indicate high chromospheric activity. The available photometry in the BVRIJHK bands is consistent with the spectral type of KO IV previously found for this star. We have also examined the spectral energy distribution of HD 81032 for the presence of an infrared colour excess using the 2MASS JHK and IRAS photometry, but found no significant excess in any band above the normal values expected for a star with this spectral type. We have also analyzed the X-ray emission properties of this star using data obtained by the ROSAT X-ray observatory during its All-Sky Survey phase. An X-ray flare of about 12 hours duration was detected during the two days of X-ray coverage obtained for this star. Its X-ray spectrum, while only containing 345 counts, is inconsistent with a single-temperature component solar-abundance coronal plasma model, but implies either the presence of two or more plasma components, non-solar abundances, or a combination of both of these properties. All of the above properties of HD 81032 suggest that it is a newly identified, evolved RS CVn binary. C1 Aryabhatta Res Inst Observ Sci, Naini Tal 263129, India. Tata Inst Fundamental Res, Bombay 400005, Maharashtra, India. NASA, Goddard Space Flight Ctr, USRA, Greenbelt, MD 20771 USA. NASA, Goddard Space Flight Ctr, Code 662, Greenbelt, MD 20771 USA. RP Pandey, JC (reprint author), Aryabhatta Res Inst Observ Sci, Naini Tal 263129, India. EM jeewan@aries.ernet.in; singh@tifr.res.in; drake@olegacy.gsfc.nasa.gov; sagar@aries.ernet.in NR 40 TC 2 Z9 3 U1 0 U2 1 PU INDIAN ACADEMY SCIENCES PI BANGALORE PA C V RAMAN AVENUE, SADASHIVANAGAR, P B #8005, BANGALORE 560 080, INDIA SN 0250-6335 J9 J ASTROPHYS ASTRON JI J. Astrophys. Astron. PD DEC PY 2005 VL 26 IS 4 BP 359 EP 376 DI 10.1007/BF02702444 PG 18 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 014NT UT WOS:000235487600001 ER PT J AU Bertucci, C Mazelle, C Acuna, MH AF Bertucci, C Mazelle, C Acuna, MH TI Interaction of the solar wind with Mars from Mars Global Surveyor MAG/ER observations SO JOURNAL OF ATMOSPHERIC AND SOLAR-TERRESTRIAL PHYSICS LA English DT Article; Proceedings Paper CT 7th Latin-American Conference on Space Geophysics CY MAR 29-APR 02, 2004 CL Atibaia, BRAZIL SP CAPES, CLAF, COSPAR, CNPq, FAPESP, FINEP, ICTP, SBGF DE solar wind interaction with unmagnetized bodies; plasma waves; discontinuities; Mars ID MAGNETIC PILEUP BOUNDARY; FIELD DRAPING ENHANCEMENT; PLASMA ENVIRONMENT; VENUS; MAGNETOSPHERE; MAGNETOTAIL; WAVES AB The observations of the magnetometer/electron reflectometer (MAG/ER) investigation onboard the Mars Global Surveyor (MGS) have greatly contributed to improve our understanding of the interaction of the solar wind with Mars. These observations established conclusively that a global dynamo-generated magnetic field does not exist at Mars, and that the interaction with solar wind is of the atmospheric type. This article reviews the most important results obtained from MGS MAG/ER on the study of two major features in the Mars solar wind interaction. The first feature is the occurrence of large-amplitude, highly coherent waves at the proton cyclotron frequency in the region upstream from the Martian bow shock. The second feature is the magnetic pileup boundary (MPB), a well-defined plasma boundary inside of which the planetary exospheric ions outnumber the solar wind ions. The study of these two elements is crucial to characterize the properties of the Martian exosphere. In addition, the occurrence of an MPB at comets and Venus reveals common processes to all these unmagnetized atmospheric bodies in spite of their different physical nature and characteristic scales. (c) 2005 Elsevier Ltd. All rights reserved. C1 Ctr Etud Spatiale Rayonnements, Toulouse, France. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. RP Bertucci, C (reprint author), Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Prince Consort Rd, London, England. EM c.bertucci@imperial.ac.uk OI Bertucci, Cesar/0000-0002-2540-5384 NR 34 TC 18 Z9 18 U1 0 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 1364-6826 EI 1879-1824 J9 J ATMOS SOL-TERR PHY JI J. Atmos. Sol.-Terr. Phys. PD DEC PY 2005 VL 67 IS 17-18 BP 1797 EP 1808 DI 10.1016/j.jastp.2005.04.007 PG 12 WC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences SC Geochemistry & Geophysics; Meteorology & Atmospheric Sciences GA 000GM UT WOS:000234449000023 ER PT J AU Oreopoulos, L Cahalan, RF AF Oreopoulos, L Cahalan, RF TI Cloud inhomogeneity from MODIS SO JOURNAL OF CLIMATE LA English DT Article ID SOLAR RADIATIVE-TRANSFER; PARALLEL ALBEDO BIASES; BOUNDARY-LAYER CLOUDS; LARGE-SCALE MODELS; LIQUID-WATER PATH; SATELLITE-OBSERVATIONS; EFFECTIVE RADIUS; PARAMETERIZATION; VARIABILITY; FLUXES AB Two full months ( July 2003 and January 2004) of Moderate Resolution Imaging Spectroradiometer ( MODIS) Atmosphere Level-3 data from the Terra and Aqua satellites are analyzed in order to characterize the horizontal variability of vertically integrated cloud optical thickness ("cloud inhomogeneity") at global scales. The monthly climatology of cloud inhomogeneity is expressed in terms of standard parameters, initially calculated for each day of the month at spatial scales of 1 degrees X 1 degrees and subsequently averaged at monthly, zonal, and global scales. Geographical, diurnal, and seasonal changes of inhomogeneity parameters are examined separately for liquid and ice phases and separately over land and ocean. It is found that cloud inhomogeneity is overall weaker in summer than in winter. For liquid clouds, it is also consistently weaker for local morning than local afternoon and over land than ocean. Cloud inhomogeneity is comparable for liquid and ice clouds on a global scale, but with stronger spatial and temporal variations for the ice phase, and exhibits an average tendency to be weaker for near- overcast or overcast grid points of both phases. Depending on cloud phase, hemisphere, surface type, season, and time of day, hemispheric means of the inhomogeneity parameter nu( roughly the square of the ratio of optical thickness mean to standard deviation) have a wide range of similar to 1.7 to 4, while for the inhomogeneity parameter chi( the ratio of the logarithmic to linear mean) the range is from similar to 0.65 to 0.8. The results demonstrate that the MODIS Level- 3 dataset is suitable for studying various aspects of cloud inhomogeneity and may prove invaluable for validating future cloud schemes in large- scale models capable of predicting subgrid variability. C1 NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. Univ Maryland Baltimore Cty, JCET, Baltimore, MD 21228 USA. NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. RP Oreopoulos, L (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Code 613-2, Greenbelt, MD 20771 USA. EM lazaros@climate.gsfc.nasa.gov RI Oreopoulos, Lazaros/E-5868-2012; Cahalan, Robert/E-3462-2012 OI Oreopoulos, Lazaros/0000-0001-6061-6905; Cahalan, Robert/0000-0001-9724-1270 NR 22 TC 21 Z9 21 U1 0 U2 5 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0894-8755 J9 J CLIMATE JI J. Clim. PD DEC PY 2005 VL 18 IS 23 BP 5110 EP 5124 DI 10.1175/JCLI3591.1 PG 15 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 998EW UT WOS:000234302400012 ER PT J AU Lamahewa, TA Simon, MK Kennedy, RA Abhayapala, TD AF Lamahewa, TA Simon, MK Kennedy, RA Abhayapala, TD TI Performance analysis of space-time codes in realistic propagation environments: A moment generating function-based approach SO JOURNAL OF COMMUNICATIONS AND NETWORKS LA English DT Article DE Gaussian Q-function; multi-input multi-output (MIMO) system; modal correlation; moment-generating function; non-isotropic scattering; space-time coding ID RAYLEIGH-FADING CHANNELS; ERROR PERFORMANCE; RADIO AB In this paper, we derive analytical expressions for the exact pairwise error probability (PEP) of a space-time coded system operating over spatially correlated fast (constant over the duration of a symbol) and slow (constant over the length of a code word) fading channels using a moment-generating function-based approach. We discuss two analytical techniques that can be used to evaluate the exact-PEPs (and therefore, approximate the average bit error probability (BEP)) in closed form. These analytical expressions are more realistic than previously published PEP expressions as they fully account for antenna spacing, antenna geometries (uniform linear array, uniform grid array, uniform circular array, etc.) and scattering models (uniform, Gaussian, Laplacian, Von-mises, etc.). Inclusion of spatial information in these expressions provides valuable insights into the physical factors determining the performance of a space-time code. Using these new PEP expressions, we investigate the effect of antenna spacing, antenna geometries and azimuth power distribution parameters (angle of arrival/departure and angular spread) on the performance of a four-state QPSK space-time trellis code proposed by Tarokh et al. for two transmit antennas. C1 Australian Natl Univ, Res Sch Informat Sci & Engn, Dept Informat Engn, Canberra, ACT 0200, Australia. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Lamahewa, TA (reprint author), Australian Natl Univ, Res Sch Informat Sci & Engn, Dept Informat Engn, Canberra, ACT 0200, Australia. EM tharaka.lamahewa@anu.edu.au; marvin.k.simon@jpl.nasa.gov; rodney.kennedy@anu.edu.au; thushara.abhayapala@anu.edu.au RI Abhayapala, Thushara/B-8483-2008; Kennedy, Rodney/B-8215-2009; OI Kennedy, Rodney/0000-0002-3946-3673; Abhayapala, Thushara/0000-0001-6937-7218 NR 23 TC 3 Z9 3 U1 0 U2 0 PU KOREAN INST COMMUNICATIONS SCIENCES (K I C S) PI SEOUL PA HYUNDAI KIRIM OFFICETEL 1504-6 SEOCHODONG 1330-18, SEOCHOKU, SEOUL 137-070, SOUTH KOREA SN 1229-2370 J9 J COMMUN NETW-S KOR JI J. Commun. Netw. PD DEC PY 2005 VL 7 IS 4 BP 450 EP 461 PG 12 WC Computer Science, Information Systems; Telecommunications SC Computer Science; Telecommunications GA 000JW UT WOS:000234458800007 ER PT J AU Chen, JL Wilson, CR Tapley, BD Famiglietti, JS Rodell, M AF Chen, JL Wilson, CR Tapley, BD Famiglietti, JS Rodell, M TI Seasonal global mean sea level change from satellite altimeter, GRACE, and geophysical models SO JOURNAL OF GEODESY LA English DT Article DE sea level change; global; seasonal; GRACE; altimeter; hydrology ID ICE-SHEET; MASS; RISE; VARIABILITY; GRAVITY; SYSTEM AB We estimate seasonal global mean sea level changes using different data resources, including sea level anomalies from satellite radar altimetry, ocean temperature and salinity from the World Ocean Atlas 2001, time-variable gravity observations from the Gravity Recovery and Climate Experiment (GRACE) mission, and terrestrial water storage and atmospheric water vapor changes from the NASA global land data assimilation system and National Centers for Environmental Prediction reanalysis atmospheric model. The results from all estimates are consistent in amplitude and phase at the annual period, in some cases with remarkably good agreement. The results provide a good measure of average annual variation of water stored within atmospheric, land, and ocean reservoirs. We examine how varied treatments of degree-2 and degree-1 spherical harmonics from GRACE, laser ranging, and Earth rotation variations affect GRACE mean sea level change estimates. We also show that correcting the standard equilibrium ocean pole tide correction for mass conservation is needed when using satellite altimeter data in global mean sea level studies. These encouraging results indicate that is reasonable to consider estimating longer-term time series of water storage in these reservoirs, as a way of tracking climate change. C1 Univ Texas, Ctr Space Res, Austin, TX 78759 USA. Univ Texas, Dept Geol Sci, Austin, TX 78712 USA. Univ Calif Irvine, Dept Earth Syst Sci, Irvine, CA 92697 USA. NASA, Goddard Space Flight Ctr, Hydrol Sci Branch, Greenbelt, MD 20771 USA. RP Chen, JL (reprint author), Univ Texas, Ctr Space Res, 3925 W Braker Lane,Suite 200, Austin, TX 78759 USA. EM chen@csr.utexas.edu; crwilson@mail.utexas.edu; jfamigli@uci.edu; Matthew.Rodell@nasa.gov RI Rodell, Matthew/E-4946-2012 OI Rodell, Matthew/0000-0003-0106-7437 NR 34 TC 35 Z9 44 U1 2 U2 19 PU SPRINGER PI NEW YORK PA 233 SPRING STREET, NEW YORK, NY 10013 USA SN 0949-7714 J9 J GEODESY JI J. Geodesy PD DEC PY 2005 VL 79 IS 9 BP 532 EP 539 DI 10.1007/s00190-005-0005-9 PG 8 WC Geochemistry & Geophysics; Remote Sensing SC Geochemistry & Geophysics; Remote Sensing GA 990IY UT WOS:000233737600004 ER PT J AU Frey, MM Stewart, RW McConnell, JR Bales, RC AF Frey, MM Stewart, RW McConnell, JR Bales, RC TI Atmospheric hydroperoxides in West Antarctica: Links to stratospheric ozone and atmospheric oxidation capacity SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID HYDROGEN-PEROXIDE H2O2; ARCTIC BOUNDARY-LAYER; SOUTH-POLE; ISCAT 2000; PHOTOCHEMICAL PRODUCTION; SURFACE SNOW; ICE CORES; GREENLAND; FORMALDEHYDE; CHEMISTRY AB The troposphere above the West Antarctic Ice Sheet (WAIS) was sampled for hydroperoxides at 21 locations during 2-month-long summer traverses from 2000 to 2002, as part of the U. S. International Trans-Antarctic Scientific Expedition (US ITASE). First-time quantitative measurements using a high-performance liquid chromatography method showed that methylhydroperoxide (MHP) is the only important organic hydroperoxide occurring in the Antarctic troposphere and that it is found at levels 10 times those previously predicted by photochemical models. During three field seasons, means and standard deviations for hydrogen peroxide (H2O2) were 321 +/- 158 pptv, 650 +/- 176 pptv, and 330 +/- 147 pptv. While MHP was detected but not quantified in December 2000, levels in summer 2001 and 2002 were 317 +/- 128 pptv and 304 +/- 172 pptv. Results from firm air experiments and diurnal variability of the two species showed that atmospheric H2O2 is significantly impacted by a physical snow pack source between 76 degrees and 90 degrees S, whereas MHP is not. We show strong evidence of a negative correlation between stratospheric ozone and H2O2 at the surface. Between 27 November and 12 December in 2001, when ozone column densities dropped below 220 Dobson units (DU) (means in 2000 and 2001 were 318 DU and 334 DU, respectively), H2O2 was 1.7 times that observed in the same period in 2000 and 2002, while MHP was only 80% of the levels encountered in 2002. Photochemical box model runs match MHP observations only when the production rate from CH3O2 + HO2 was increased to the upper limit of its estimated range of uncertainty. Model results suggest that NO and OH levels on WAIS are closer to coastal values, while Antarctic Plateau levels are higher, confirming that region to be a highly oxidizing environment. The modeled sensitivity of H2O2 and particularly MHP to NO offers the potential to use atmospheric hydroperoxides to constrain the NO background and thus estimate the past oxidation capacity of the remote atmosphere using ice cores. C1 Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA. Univ Calif Merced, Sch Engn, Atwater, CA 95301 USA. NASA, Goddard Space Flight Ctr, Atmospher Chem & Dynam Branch, Greenbelt, MD 20771 USA. Desert Res Inst, Div Hydrol Sci, Reno, NV 89512 USA. RP Frey, MM (reprint author), Univ Arizona, Dept Hydrol & Water Resources, Tucson, AZ 85721 USA. EM mfrey@ucmerced.edu RI Frey, Markus/G-1756-2012 OI Frey, Markus/0000-0003-0535-0416 NR 63 TC 36 Z9 36 U1 3 U2 13 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X EI 2169-8996 J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 1 PY 2005 VL 110 IS D23 AR D23301 DI 10.1029/2005JD006110 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 993EM UT WOS:000233936300004 ER PT J AU Slanger, TG Cosby, PC Huestis, DL Saiz-Lopez, A Murray, BJ O'Sullivan, DA Plane, JMC Prieto, CA Martin-Torres, FJ Jenniskens, P AF Slanger, TG Cosby, PC Huestis, DL Saiz-Lopez, A Murray, BJ O'Sullivan, DA Plane, JMC Prieto, CA Martin-Torres, FJ Jenniskens, P TI Variability of the mesospheric nightglow sodium D-2/D-1 ratio SO JOURNAL OF GEOPHYSICAL RESEARCH-ATMOSPHERES LA English DT Article ID ATMOSPHERIC SODIUM; SEASONAL-VARIATIONS; ATOMIC OXYGEN; LAYER; EXCITATION; CHEMISTRY; MECHANISM; PROFILES; EMISSION; DENSITY AB Measurements of the intensity ratio of the 589.0/589.6 nm sodium doublet in the terrestrial nightglow over an 8-year period, involving >300 separate determinations, have established that it is variable, the value R-D = I(D-2)/I(D-1) lying between 1.2 and 1.8. Sky spectra from the Keck I telescope with the High-Resolution Echelle Spectrometer ( HIRES) echelle spectrograph and the Keck II telescope with the Echellette Spectrograph and Imager (ESI) echelle spectrograph were used in this analysis. The result contrasts with the accepted view, from earlier measurements at midlatitude, that the ratio is 2.0, as expected on statistical grounds. The lack of dependence of the ratio on viewing elevation angle, and hence Na slant column, allows self-absorption to be ruled out as a cause of the variability. The data suggest a semiannual oscillation in the ratio, maximum at the equinoxes and minimum at the solstices. Airborne measurements over the North Atlantic (40 degrees-50 degrees N) in 2002 show an even larger range in the nightglow ratio and no correlation with the upper mesospheric temperature determined from the OH 6-2 bands. A laboratory study confirms that the ratio does not depend on temperature; however, it is shown to be sensitive to the [O]/[O-2] ratio. It is therefore postulated that the variable ratio arises from a competition between O reacting with NaO(A(3)Sigma(+)), produced from the reaction of Na with O-3, to yield D-line emission with a D-2/D-1 ratio greater than about 2.0, and quenching by O-2 to produce NaO(X-2 Pi), possibly with vibrational excitation, which then reacts with O to produce emission with a ratio of less than 1.3. C1 SRI Int, Mol Phys Lab, Menlo Pk, CA 94025 USA. NASA, Ames Res Ctr, Mountain View, CA 94043 USA. Univ E Anglia, Sch Environm Sci, Norwich NR4 7TJ, Norfolk, England. AS&M Inc, NASA, Langley Res Ctr, Hampton, VA 23666 USA. Univ Texas, McDonald Observ, Austin, TX 78712 USA. Univ Texas, Dept Astron, Austin, TX 78712 USA. RP Slanger, TG (reprint author), SRI Int, Mol Phys Lab, 333 Ravenswood Ave, Menlo Pk, CA 94025 USA. EM tom.slanger@sri.com RI Murray, Benjamin/C-1219-2010; Saiz-Lopez, Alfonso/B-3759-2015; Plane, John/C-7444-2015; Martin-Torres, Francisco Javier/G-6329-2015 OI Murray, Benjamin/0000-0002-8198-8131; Saiz-Lopez, Alfonso/0000-0002-0060-1581; Plane, John/0000-0003-3648-6893; Martin-Torres, Francisco Javier/0000-0001-6479-2236 NR 40 TC 16 Z9 16 U1 0 U2 2 PU AMER GEOPHYSICAL UNION PI WASHINGTON PA 2000 FLORIDA AVE NW, WASHINGTON, DC 20009 USA SN 2169-897X J9 J GEOPHYS RES-ATMOS JI J. Geophys. Res.-Atmos. PD DEC 1 PY 2005 VL 110 IS D23 AR D23302 DI 10.1029/2005JD006078 PG 8 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 993EM UT WOS:000233936300003 ER PT J AU Rothman, LS Jacquemart, D Barbe, A Benner, DC Birk, M Brown, LR Carleer, MR Chackerian, C Chance, K Coudert, LH Dana, V Devi, VM Flaud, JM Gamache, RR Goldman, A Hartmann, JM Jucks, KW Maki, AG Mandin, JY Massie, ST Orphal, J Perrin, A Rinsland, CP Smith, MAH Tennyson, J Tolchenov, RN Toth, RA Vander Auwera, J Varanasi, P Wagner, G AF Rothman, LS Jacquemart, D Barbe, A Benner, DC Birk, M Brown, LR Carleer, MR Chackerian, C Chance, K Coudert, LH Dana, V Devi, VM Flaud, JM Gamache, RR Goldman, A Hartmann, JM Jucks, KW Maki, AG Mandin, JY Massie, ST Orphal, J Perrin, A Rinsland, CP Smith, MAH Tennyson, J Tolchenov, RN Toth, RA Vander Auwera, J Varanasi, P Wagner, G TI The HITRAN 2004 molecular spectroscopic database SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article; Proceedings Paper CT 8th Biennial HITRAN Database Conference CY JUN 16-18, 2004 CL Harvard Smithsonian Ctr Astrophys, Cambridge, MA HO Harvard Smithsonian Ctr Astrophys DE HITRAN; spectroscopic database; molecular spectroscopy; molecular absorption; line parameters; absorption cross-sections; aerosols ID SELF-BROADENING COEFFICIENTS; ABSOLUTE LINE-INTENSITIES; FOURIER-TRANSFORM SPECTROSCOPY; ABSORPTION CROSS-SECTIONS; DIODE-LASER SPECTROSCOPY; FAR-INFRARED SPECTRUM; MULTISPECTRUM FITTING PROCEDURE; PRESSURE-SHIFT COEFFICIENTS; EFFECTIVE DIPOLE-MOMENT; MU-M REGION AB This paper describes the status of the 2004 edition of the HITRAN molecular spectroscopic database. The HITRAN compilation consists of several components that serve as input for radiative transfer calculation codes: individual line parameters for the microwave through visible spectra of molecules in the gas phase; absorption cross-sections for molecules having dense spectral features, i.e., spectra in which the individual lines are unresolvable; individual line parameters and absorption cross-sections for bands in the ultra-violet; refractive indices of aerosols; tables and files of general properties associated with the database; and database management software. The line-by-line portion of the database contains spectroscopic parameters for 39 molecules including many of their isotopologues. The format of the section of the database on individual line parameters of HITRAN has undergone the most extensive enhancement in almost two decades. It now lists the Einstein A-coefficients, statistical weights of the upper and lower levels of the transitions, a better system for the representation of quantum identifications, and enhanced referencing and uncertainty codes. In addition, there is a provision for making corrections to the broadening of line transitions due to line mixing. (C) 2005 Elsevier Ltd. All rights reserved. C1 Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, Cambridge, MA 02138 USA. Univ Reims, Grp Spectrometrie Mol & Atmospher, F-51062 Reims, France. Coll William & Mary, Dept Phys, Williamsburg, VA 23187 USA. DLR, Remote Sensing Technol Inst, Wessling, Germany. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Free Univ Brussels, Serv Chim Quant & Photophys, B-1050 Brussels, Belgium. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Univ Paris 11, Photophys Mol Lab, F-91405 Orsay, France. Univ Paris 06, Lab Phys Mol & Applicat, F-75252 Paris, France. Univ Mass Lowell, Dept Environm Earth & Atmospher Sci, Lowell, MA 01854 USA. Univ Denver, Dept Phys, Denver, CO 80208 USA. Harvard Smithsonian Ctr Astrophys, Opt & Infrared Astron Div, Cambridge, MA 02138 USA. Natl Ctr Atmospher Res, Boulder, CO 80307 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. UCL, Dept Phys & Astron, London WC1E 6BT, England. SUNY Stony Brook, Stony Brook, NY 11794 USA. RP Rothman, LS (reprint author), Harvard Smithsonian Ctr Astrophys, Atom & Mol Phys Div, 60 Garden St, Cambridge, MA 02138 USA. EM lrothman@cfa.harvard.edu RI Tennyson, Jonathan/I-2222-2012; Orphal, Johannes/A-8667-2012; OI Tennyson, Jonathan/0000-0002-4994-5238; Orphal, Johannes/0000-0002-1943-4496; Rothman, Laurence/0000-0002-3837-4847; Chance, Kelly/0000-0002-7339-7577 NR 210 TC 2058 Z9 2154 U1 16 U2 155 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD DEC 1 PY 2005 VL 96 IS 2 BP 139 EP 204 DI 10.1016/j.jqsrt.2004.10.008 PG 66 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 956MG UT WOS:000231303400002 ER PT J AU Goldman, A Barbe, A Tyuterev, VG De Backer-Barilly, MR Hannigan, JW Coffey, MT Rinsland, CP Blatherwick, RD AF Goldman, A Barbe, A Tyuterev, VG De Backer-Barilly, MR Hannigan, JW Coffey, MT Rinsland, CP Blatherwick, RD TI Identification of enhanced absorption by O-16(3) lines around 5 mu m in high-resolution FTIR solar spectra SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article; Proceedings Paper CT 8th Biennial HITRAN Database Conference CY JUN 16-18, 2004 CL Harvard Smithsonian Ctr Astrophys, Cambridge, MA HO Harvard Smithsonian Ctr Astrophys DE atmospheric ozone; infrared Fourier transform spectroscopy; solar spectra ID BALLOON-BORNE; OZONE; REGION; HITRAN AB A set of previously unpredicted O-16(3) strong absorption lines in the 5 mu m region are identified for the first time in balloon-borne high-resolution (0.003 cm(-1)) solar spectra. These spectral features are consistent with recent ozone laboratory spectra, and are interpreted by accidental resonance effects. Some of the lines are also observed in high-resolution ground-based spectra. (C) 2005 Elsevier Ltd. All rights reserved. C1 Univ Denver, Dept Phys, Denver, CO 80208 USA. UFR Sci, CNRS, UMR 6089, Grp Spectrometrie Mol & Atmospher, F-51687 Reims, France. Natl Ctr Atmospher Res, Div Atmospher Chem, Boulder, CO 80303 USA. NASA, Langley Res Ctr, Hampton, VA 23681 USA. RP Goldman, A (reprint author), Univ Denver, Dept Phys, Denver, CO 80208 USA. EM goldman@acd.ucar.edu NR 14 TC 3 Z9 4 U1 0 U2 1 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD DEC 1 PY 2005 VL 96 IS 2 BP 241 EP 250 DI 10.1016/j.jqsrt.2004.10.009 PG 10 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 956MG UT WOS:000231303400004 ER PT J AU Brown, LR AF Brown, LR TI Empirical line parameters of methane from 1.1 to 2.1 mu m SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article; Proceedings Paper CT 8th Biennial HITRAN Database Conference CY JUN 16-18, 2004 CL Harvard Smithsonian Ctr Astrophys, Cambridge, MA HO Harvard Smithsonian Ctr Astrophys DE methane; positions; intensities; near-infrared ID DOUBLE-RESONANCE OBSERVATION; BROADENING COEFFICIENTS; M REGION; BAND; STRENGTHS; CM(-1); SPECTROSCOPY; SPECTRA; INTENSITIES; (CH4)-C-12 AB To provide line parameters for the near-infrared methane spectrum, 35,306 line positions and intensities at room temperature were retrieved between 6180 and 9200 cm(-1), along with 4936 lines between 4800 and 5 500 cm(-1). For this, laboratory absorption spectra were recorded at 0.010-0.022 cm(-1) resolution using the McMath-Pierce Fourier Transform Spectrometer located on Kitt Peak in Arizona. Positions were calibrated using CO transitions at 2.3 and 1.6 mu m and H2O lines at 1.9 and 1.3 mu m. The minimum line intensity included was 3.7 x 10(-26) cm(-1)/(molecule cm(-2)), and the combined sum of the intensities in these two intervals was 7.085 x 10(-20) cm(-1)/(molecule cm(-2)) at 296 (+/- 4)K. Quantum assignments from the literature were matched for 1% of the features, and a new methane database was compiled for the near-infrared. (C) 2005 Elsevier Ltd. All rights reserved. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Brown, LR (reprint author), CALTECH, Jet Prop Lab, Mail Stop 183-601,4800 Oak Grove Dr, Pasadena, CA 91109 USA. EM Linda.Brown@jpl.nasa.gov NR 43 TC 57 Z9 57 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD DEC 1 PY 2005 VL 96 IS 2 BP 251 EP 270 DI 10.1016/j.jqsrt.2004.12.037 PG 20 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 956MG UT WOS:000231303400005 ER PT J AU Rinsland, CP Sharpe, SW Sams, RL AF Rinsland, CP Sharpe, SW Sams, RL TI Temperature-dependent infrared absorption cross sections of methyl cyanide (acetonitrile) SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article; Proceedings Paper CT 8th Biennial HITRAN Database Conference CY JUN 16-18, 2004 CL Harvard Smithsonian Ctr Astrophys, Cambridge, MA HO Harvard Smithsonian Ctr Astrophys DE absorption cross section; infrared; methyl cyanide acetonitrile; laboratory spectroscopy; transmission and scattering of radiation; pollution ID SPECTRUM; ATMOSPHERE; CH3CN; CM(-1); TITAN; BANDS; HC3N AB Pressure broadened (1 atm. N-2) absorption cross sections and integrated band intensities have been derived from laboratory spectra of CH3CN, recorded at 276, 298, and 323 K, covering 600-6500 cm(-1). The spectra were recorded at a resolution of 0.112 cm(-1) using a commercial Fourier transform spectrometer and a custom flowing sample delivery system. We report integrated absorption cross sections for intervals corresponding to the most prominent bands, compare the results with previously reported values, and discuss error sources, which are estimated as similar to 7% with systematic error the largest error source. (C) 2005 Elsevier Ltd. All rights reserved. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. Pacific NW Natl Lab, Richland, WA 99352 USA. RP Rinsland, CP (reprint author), NASA, Langley Res Ctr, 21 Langley Blvd,Mail Stop 401A, Hampton, VA 23681 USA. EM c.p.rinsland@larc.nasa.gov NR 32 TC 14 Z9 14 U1 0 U2 5 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD DEC 1 PY 2005 VL 96 IS 2 BP 271 EP 280 DI 10.1016/j.jqsrt.2005.03.004 PG 10 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 956MG UT WOS:000231303400006 ER PT J AU Rinsland, CP Paton-Walsh, C Jones, NB Griffith, DWT Goldman, A Wood, SW Chiou, L Meier, A AF Rinsland, CP Paton-Walsh, C Jones, NB Griffith, DWT Goldman, A Wood, SW Chiou, L Meier, A TI High spectral resolution solar absorption measurements of ethylene (C2H4) in a forest fire smoke plume using HITRAN parameters: Tropospheric vertical profile retrieval SO JOURNAL OF QUANTITATIVE SPECTROSCOPY & RADIATIVE TRANSFER LA English DT Article; Proceedings Paper CT 8th Biennial HITRAN Database Conference CY JUN 16-18, 2004 CL Harvard Smithsonian Ctr Astrophys, Cambridge, MA HO Harvard Smithsonian Ctr Astrophys DE remote sensing; fire spectra ID TRANSFORM INFRARED-SPECTROSCOPY; LABORATORY BIOMASS FIRES; TRACE GAS EMISSIONS; INTENSITIES; HCN; CO AB The tropospheric mixing ratio profile of ethylene (C2H4) has been retrieved from a high spectral resolution ground-based infrared solar absorption spectrum. The spectrum was recorded during intense fires in New South Wales, Australia on January 1, 2002, and was analyzed with the C2H4 spectral parameters added to the 2000 HITRAN compilation. Absorption by C2H4 in the smoke-affected spectrum extends over a broad spectral range in a region with observable rotational fine structure. The fine structure occurs in addition to the 949.5 cm(-1) v(7) band Q branch that is traditionally used to quantify C2H4 amounts from infrared atmospheric measurements assuming room temperature laboratory absorption coefficients. The measured spectrum is fitted to near the noise level with a retrieved vertical column of (3.8 +/- 0.2) x 10(17) molecules per square centimeter. The retrieved vertical C2H4 profile increases with altitude near the surface reaching a maximum of 37 parts per billion (10(-9)) near 1 km, decreasing above. (C) 2005 Elsevier Ltd. All rights reserved. C1 NASA, Langley Res Ctr, Hampton, VA 23681 USA. Univ Wollongong, Dept Chem, Wollongong, NSW 2500, Australia. Univ Denver, Dept Phys, Denver, CO 80208 USA. Natl Inst Water & Atmospher Res, Omakau, Cent Otago, New Zealand. Syst & Appl Sci Corp, Hampton, VA USA. Apollo Life Sci Pty Ltd, Sydney, NSW 2015, Australia. RP Rinsland, CP (reprint author), NASA, Langley Res Ctr, Mail Stop 401A, Hampton, VA 23681 USA. EM Curtis.P.Rinsland@nasa.gov RI Paton-Walsh, Clare/B-2774-2009; Jones, Nicholas/G-5575-2011 OI Paton-Walsh, Clare/0000-0003-1156-4138; Jones, Nicholas/0000-0002-0111-2368 NR 24 TC 22 Z9 23 U1 1 U2 4 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0022-4073 J9 J QUANT SPECTROSC RA JI J. Quant. Spectrosc. Radiat. Transf. PD DEC 1 PY 2005 VL 96 IS 2 BP 301 EP 309 DI 10.1016/j.jqsrt.2005.03.003 PG 9 WC Optics; Spectroscopy SC Optics; Spectroscopy GA 956MG UT WOS:000231303400009 ER PT J AU Howard, A Seraji, H Werger, B AF Howard, A Seraji, H Werger, B TI Global and regional path planners for integrated planning and navigation SO JOURNAL OF ROBOTIC SYSTEMS LA English DT Article ID TERRAIN AB This paper presents a hierarchical strategy for field mobile robots that incorporates path planning at different ranges. At the top layer is a global path planner that utilizes gross terrain characteristics, such as hills and valleys, to determine globally safe paths through the rough terrain. This information is then passed via waypoints to a regional layer that plans appropriate navigation paths using regional terrain characteristics. The global and regional path planners share the same map information, but at different ranges. The motion recommendations from the regional layer are then combined with those of the reactive navigation layer to provide reactive control for the mobile robot. Details of the global and regional path planners are discussed, and simulation and experimental results are presented. (C) 2005 Wiley Periodicals, Inc. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Georgia Inst Technol, Atlanta, GA 30332 USA. RP CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 23 TC 10 Z9 10 U1 0 U2 0 PU JOHN WILEY & SONS INC PI HOBOKEN PA 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0741-2223 J9 J ROBOTIC SYST JI J. Robot. Syst. PD DEC PY 2005 VL 22 IS 12 BP 767 EP 778 DI 10.1002/rob.20098 PG 12 WC Robotics SC Robotics GA 998WN UT WOS:000234350700005 ER PT J AU Seraji, H AF Seraji, H TI SmartNav: A rule-free fuzzy approach to rover navigation SO JOURNAL OF ROBOTIC SYSTEMS LA English DT Article ID TERRAIN-BASED NAVIGATION; SYSTEMS; LOGIC AB This paper introduces the basic concepts of the SmartNav rule-free fuzzy approach to safe rover navigation through hazardous natural terrain. This novel "rule-free" approach reduces the complexity in rover navigation where many alternative paths must be evaluated and compared. The SmartNav rover navigation architecture integrates goal attainment with both local and regional hazard avoidance. Goal and safety preference factors differentiate between preferred and unpreferred terrain sectors. The goal-preference factor is used to make sector evaluation based on the sector orientation relative to the designated goal position. The safety-preference factors are used to make sector evaluations on the basis of the sector local and regional hazards. These sector evaluations are blended to find the effective preference factor for each sector. The preference factors of all sectors are then compared to choose the heading command for the rover. The rover speed command is also computed based on the goal distance and safety-preference factor of the chosen sector. The above navigation steps are continuously repeated throughout the rover motion. Numerical examples are presented to illustrate the basic concepts introduced in this paper, and tests on a commercial rover are planned. (C) 2005 Wiley Periodicals, Inc. C1 CALTECH, Jet Prop Lab, NASA, Pasadena, CA 91109 USA. RP Seraji, H (reprint author), CALTECH, Jet Prop Lab, NASA, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 18 TC 2 Z9 2 U1 0 U2 0 PU JOHN WILEY & SONS INC PI HOBOKEN PA 111 RIVER ST, HOBOKEN, NJ 07030 USA SN 0741-2223 J9 J ROBOTIC SYST JI J. Robot. Syst. PD DEC PY 2005 VL 22 IS 12 BP 795 EP 808 DI 10.1002/rob.20100 PG 14 WC Robotics SC Robotics GA 998WN UT WOS:000234350700007 ER PT J AU Strangman, G Thompson, JH Strauss, MM Marshburn, TH Sutton, JP AF Strangman, G Thompson, JH Strauss, MM Marshburn, TH Sutton, JP TI Functional brain imaging of a complex navigation task following one night of total sleep deprivation: a preliminary study SO JOURNAL OF SLEEP RESEARCH LA English DT Article DE flight docking task; functional magnetic resonance imaging; hemodynamics; spacedock; total sleep deprivation ID ATTENTION; PERFORMANCE; HUMANS; MRI AB Several neuroimaging studies have demonstrated compensatory cerebral responses consequent to sleep deprivation (SD), but all have focused on simple tasks with limited behavioral response options. We assessed the cerebral effects associated with SD during the performance of a complex, open-ended, dual-joystick, 3D navigation task (simulated orbital docking) in a cross-over protocol, with counterbalanced orders of normal sleep (NS) and a single night of total SD (similar to 27 h). Behavioral performance on multiple measures was comparable in the two sleep conditions. Functional magnetic resonance imaging revealed multiple compensatory SD > NS cerebral responses, including the posterior superior temporal sulcus [Brodmann area (BA) 39/22/37], prefrontal cortex (BA 9), lateral temporal cortex (BA 22/21), and right substantia nigra. Right posterior cingulate cortex (BA 31) exhibited NS > SD activity. Our findings extend the compensatory cerebral response hypothesis to complex, open-ended tasks. C1 Harvard Univ, Sch Med, Massachusetts Gen Hosp, Dept Psychiat,Neural Syst Grp, Charlestown, MA 02129 USA. Harvard Univ, Sch Med, Massachusetts Gen Hosp, Athinoula A Martinos Ctr, Charlestown, MA USA. NASA, Lyndon B Johnson Space Ctr, Houston, TX 77058 USA. Natl Space Biomed Res Inst, Houston, TX USA. RP Strangman, G (reprint author), Harvard Univ, Sch Med, Massachusetts Gen Hosp, Dept Psychiat,Neural Syst Grp, 149 13th St Psychiat Rm 2651, Charlestown, MA 02129 USA. EM strang@nmr.mgh.harvard.edu RI Sanguansri, Luz/B-6630-2011 OI Sanguansri, Luz/0000-0003-1908-7604 FU NCRR NIH HHS [P41-RR014075]; NINDS NIH HHS [K25-NS046554] NR 22 TC 15 Z9 15 U1 0 U2 2 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0962-1105 J9 J SLEEP RES JI J. Sleep Res. PD DEC PY 2005 VL 14 IS 4 BP 369 EP 375 DI 10.1111/j.1365-2869.2005.00488.x PG 7 WC Clinical Neurology; Neurosciences SC Neurosciences & Neurology GA 990AI UT WOS:000233715200005 PM 16364137 ER PT J AU Lee, KN Eldridge, JI Robinson, RC AF Lee, KN Eldridge, JI Robinson, RC TI Residual stresses and their effects on the durability of environmental barrier coatings for SiC ceramics SO JOURNAL OF THE AMERICAN CERAMIC SOCIETY LA English DT Article ID SIO2 SCALE VOLATILITY; RECESSION; MULLITE AB Qualitative residual stresses in current environmental barrier coatings (EBCs) were inferred from the curvature of EBC-coated SiC wafers, and the effects of EBC stresses on the durability of EBC-coated SiC were evaluated. The magnitude of substrate curvature correlated fairly well with the EBC-SiC coefficient of thermal expansion (CTE) mismatch, EBC modulus, and thermally induced physical changes in EBC. BSAS (1-xBaO.xSrO.Al2O3.2SiO(2), 0 <= x <= 1) components in the current EBCs, i.e., Si/mullite or mullite+BSAS/BSAS or yttria-stabilized zirconia (YSZ: ZrO2-8 wt% Y2O3), were the most beneficial for reducing the EBC stress in as-sprayed as well as in post-exposure EBCs. The reduced stress was attributed to the low modulus of BSAS. The addition of a YSZ top coat significantly increased the substrate curvature because of its high CTE and sintering in thermal exposures. There were clear correlations between the wafer curvature and the EBC durability. The Si/mullite+20 wt% BSAS/BSAS EBC maintained excellent adherence, protecting the SiC substrate from oxidation, while the Si/mullite+20 wt% BSAS/YSZ EBC suffered delamination, leading to severe oxidation of the SiC substrate, after a 100 h -1300 degrees C exposure in a high-pressure burner rig. C1 NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. RP Lee, KN (reprint author), NASA, Glenn Res Ctr, Cleveland, OH 44135 USA. EM kang.lee@grc.nasa.gov NR 23 TC 28 Z9 34 U1 6 U2 48 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0002-7820 J9 J AM CERAM SOC JI J. Am. Ceram. Soc. PD DEC PY 2005 VL 88 IS 12 BP 3483 EP 3488 DI 10.1111/j.1551-2916.2005.00640.x PG 6 WC Materials Science, Ceramics SC Materials Science GA 988TS UT WOS:000233624400031 ER PT J AU Zeng, XP Tao, WK Simpson, J AF Zeng, XP Tao, WK Simpson, J TI An equation for moist entropy in a precipitating and icy atmosphere SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Article ID THERMODYNAMIC FOUNDATION; CUMULUS CLOUDS; MODEL; PARAMETERIZATION; SUPERSATURATION; MICROPHYSICS; EQUILIBRIUM; CONVECTION; DYNAMICS AB This paper addresses an equation for moist entropy in the framework of cloud-resolving models. After rewriting the energy equation with moist entropy in the place of temperature, an equation for moist entropy is obtained. The equation expresses the internal and external sources of moist entropy explicitly, providing a basis for the use of moist entropy as a prognostic variable in long-term cloud-resolving modeling. In addition, a precise formula for the surface flux of moist entropy from the underlying surface into the air above is derived. The equation for moist entropy is used to express the Neelin-Held model for the diagnosis of large-scale vertical velocity. After applying the model to a tropical oceanic atmosphere with mean annual soundings, the paper shows the sensitivity of large-scale vertical circulations to the radiative cooling rate and the surface flux of moist entropy, which demonstrates the necessity for a precise equation for moist entropy in the analysis and modeling of large-scale tropical circulations. C1 NASA, Goddard Space Flight Ctr, Atmospheres Lab, Greenbelt, MD 20771 USA. Univ Maryland Baltimore Cty, Goddard Earth Sci & Technol Ctr, Baltimore, MD 21228 USA. RP Zeng, XP (reprint author), NASA, Goddard Space Flight Ctr, Atmospheres Lab, Mail Code 613-1,Rm A417,Bldg 33, Greenbelt, MD 20771 USA. EM zeng@agnes.gsfc.nasa.gov NR 29 TC 5 Z9 5 U1 0 U2 3 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0022-4928 J9 J ATMOS SCI JI J. Atmos. Sci. PD DEC PY 2005 VL 62 IS 12 BP 4293 EP 4309 DI 10.1175/JAS3570.1 PG 17 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 999VV UT WOS:000234419800010 ER PT J AU Garcia, RR Lieberman, R Russell, JM Mlynczak, MG AF Garcia, RR Lieberman, R Russell, JM Mlynczak, MG TI Large-scale waves in the mesosphere and lower thermosphere observed by SABER SO JOURNAL OF THE ATMOSPHERIC SCIENCES LA English DT Article ID MODE ROSSBY WAVES; ASYNOPTIC SATELLITE-OBSERVATIONS; 2-DAY WAVE; SEMIANNUAL OSCILLATION; MIDDLE ATMOSPHERE; 4-DAY WAVE; TRANSIENT-RESPONSE; EQUATORIAL WAVES; SAMPLING THEORY; FIELD BEHAVIOR AB Observations made by the Sounding of the Atmosphere using Broadband Emission Radiometry (SABER) instrument on board NASA's Thermosphere-Ionosphere-Mesosphere Energetics and Dynamics (TIMED) satellite have been processed using Salby's fast Fourier synoptic mapping (FFSM) algorithm. The mapped data provide a first synoptic look at the mean structure and traveling waves of the mesosphere and lower thermosphere (MLT) since the launch of the TIMED satellite in December 2001. The results show the presence of various wave modes in the MLT, which reach largest amplitude above the mesopause and include Kelvin and Rossby-gravity waves, eastward-propagating diurnal oscillations ("non-sunsynchronous tides"), and a set of quasi-normal modes associated with the so-called 2-day wave. The latter exhibits marked seasonal variability, attaining large amplitudes during the solstices and all but disappearing at the equinoxes. SABER data also show a strong quasi-stationary Rossby wave signal throughout the middle atmosphere of the winter hemisphere; the signal extends into the Tropics and even into the summer hemisphere in the MLT, suggesting ducting by westerly background zonal winds. At certain times of the year, the 5-day Rossby normal mode and the 4-day wave associated with instability of the polar night jet are also prominent in SABER data. C1 Natl Ctr Atmospher Res, Boulder, CO 80307 USA. Colorado Res Associates, Boulder, CO USA. Hampton Univ, Hampton, VA 23668 USA. NASA, Langley Res Ctr, Hampton, VA 23665 USA. RP Garcia, RR (reprint author), Natl Ctr Atmospher Res, 1850 Table Mesa Dr, Boulder, CO 80307 USA. EM rgarcia@ucar.edu RI Mlynczak, Martin/K-3396-2012 NR 40 TC 71 Z9 73 U1 0 U2 4 PU AMER METEOROLOGICAL SOC PI BOSTON PA 45 BEACON ST, BOSTON, MA 02108-3693 USA SN 0022-4928 J9 J ATMOS SCI JI J. Atmos. Sci. PD DEC PY 2005 VL 62 IS 12 BP 4384 EP 4399 DI 10.1175/JAS3612.1 PG 16 WC Meteorology & Atmospheric Sciences SC Meteorology & Atmospheric Sciences GA 999VV UT WOS:000234419800016 ER PT J AU Lehnert, H Watling, L Stone, R AF Lehnert, H Watling, L Stone, R TI Cladorhiza corona sp nov (Porifera : Demospongiae : Cladorhizidae) from the Aleutian Islands (Alaska) SO JOURNAL OF THE MARINE BIOLOGICAL ASSOCIATION OF THE UNITED KINGDOM LA English DT Article AB A new species of Cladorhizidac, front the Aleutian Islands is described and compared with all known species of Cladorhizza worldwide. Cladorhiza corona sp. now has a unique growth form with two planes of differently shaped appendages. Appendages are Inserted directly at the stalk; a spherical or conical body at the stalk is lacking. It is the only species reported where different spicule types occur in three morphologically different areas of the sponge. The spiculation of the basal plate is characterized by the occurrence of short, thick anisoxcas and the lack of anisochelae. Anisochelac arc found in the stalk and the basal appendages only. Flattened sigmancistras and (sub-)tylostyles are restricted to the crown. The arrangement of spicules is different in the basal plate, the stalk with the basal appendages, and in the distal append ages. The dimensions and combination of spicule types separate C. corona sp. nov. from all known members of the genus. C1 Univ Maine, Darling Marine Ctr, Walpole, ME 04573 USA. Natl Marine Fisheries Serv, Auke Bay Lab, Juneau, AK 99801 USA. RP Watling, L (reprint author), Univ Maine, Darling Marine Ctr, Walpole, ME 04573 USA. EM watling@maine.edu NR 12 TC 18 Z9 22 U1 1 U2 3 PU CAMBRIDGE UNIV PRESS PI NEW YORK PA 40 WEST 20TH ST, NEW YORK, NY 10011-4211 USA SN 0025-3154 J9 J MAR BIOL ASSOC UK JI J. Mar. Biol. Assoc. U.K. PD DEC PY 2005 VL 85 IS 6 BP 1359 EP 1366 DI 10.1017/S0025315405012531 PG 8 WC Marine & Freshwater Biology SC Marine & Freshwater Biology GA 994HF UT WOS:000234021100006 ER PT J AU Milman, MH AF Milman, MH TI Accurately computing the optical pathlength difference for a Michelson interferometer with minimal knowledge of the source spectrum SO JOURNAL OF THE OPTICAL SOCIETY OF AMERICA A-OPTICS IMAGE SCIENCE AND VISION LA English DT Article ID WHITE-LIGHT INTERFEROMETRY; STELLAR INTERFEROMETER; DELAY; DISPERSION; ALGORITHM; TRACKING; FRINGE AB Astrometric measurements using stellar interferometry rely on precise measurement of the central white light fringe to accurately obtain the optical pathlength difference of incoming starlight to the two arms of the interferometer. One standard approach to stellar interferometry uses a channeled spectrum to determine phases at a number of different wavelengths that are then converted to the pathlength delay. When throughput is low these channels are broadened to improve the signal-to-noise ratio. Ultimately the ability to use monochromatic models and algorithms in each of the channels to extract phase becomes problematic and knowledge of the spectrum must be incorporated to achieve the accuracies required of the astrometric measurements. To accomplish this an optimization problem is posed to estimate simultaneously the pathlength delay and spectrum of the source. Moreover, the nature of the parameterization of the spectrum that is introduced circumvents the need to solve directly for these parameters so that the optimization problem reduces to a scalar problem in just the pathlength delay variable. A number of examples are given to show the robustness of the approach. (c) 2005 Optical Society of America. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Milman, MH (reprint author), CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 32 TC 4 Z9 4 U1 1 U2 3 PU OPTICAL SOC AMER PI WASHINGTON PA 2010 MASSACHUSETTS AVE NW, WASHINGTON, DC 20036 USA SN 1084-7529 J9 J OPT SOC AM A JI J. Opt. Soc. Am. A-Opt. Image Sci. Vis. PD DEC PY 2005 VL 22 IS 12 BP 2774 EP 2785 DI 10.1364/JOSAA.22.002774 PG 12 WC Optics SC Optics GA 994GZ UT WOS:000234020500022 PM 16396039 ER PT J AU Rom, L Cruickshank, W Burnett, A Cleveland, J Coble, P Kaplan, M Schoedinger, S Wallace, B AF Rom, L Cruickshank, W Burnett, A Cleveland, J Coble, P Kaplan, M Schoedinger, S Wallace, B TI Improving ocean education by implementmg the US Ocean Action Plan's directives SO MARINE TECHNOLOGY SOCIETY JOURNAL LA English DT Editorial Material C1 Natl Sci Fdn, Joint Task Force Educ, Arlington, VA 22230 USA. US EPA, Washington, DC 20460 USA. Off Naval Res, Washington, DC USA. NASA, Washington, DC 20546 USA. NOAA, Washington, DC 20233 USA. RP Rom, L (reprint author), Natl Sci Fdn, Joint Task Force Educ, 4201 Wilson Blvd, Arlington, VA 22230 USA. EM elrom@nsf.gov NR 7 TC 0 Z9 0 U1 0 U2 0 PU MARINE TECHNOLOGY SOC INC PI COLUMBIA PA 5565 STERRETT PLACE, STE 108, COLUMBIA, MD 21044 USA SN 0025-3324 J9 MAR TECHNOL SOC J JI Mar. Technol. Soc. J. PD WIN PY 2005 VL 39 IS 4 BP 5 EP 7 PG 3 WC Engineering, Ocean; Oceanography SC Engineering; Oceanography GA 027ZA UT WOS:000236453700002 ER PT J AU Keener-Chavis, P Coble, PG AF Keener-Chavis, P Coble, PG TI Exploration and discovery: Essential elements in earth and space science literacy SO MARINE TECHNOLOGY SOCIETY JOURNAL LA English DT Editorial Material C1 NOAA, Off Ocean Explorat, Educ Programs, Washington, DC USA. NASA, Sci Miss Directorate, Earth Sun Syst Div, Washington, DC 20546 USA. RP Keener-Chavis, P (reprint author), NOAA, Off Ocean Explorat, Educ Programs, Washington, DC USA. EM Paula.Keener-Chavis@noaa.gov NR 7 TC 0 Z9 0 U1 0 U2 1 PU MARINE TECHNOLOGY SOC INC PI COLUMBIA PA 5565 STERRETT PLACE, STE 108, COLUMBIA, MD 21044 USA SN 0025-3324 J9 MAR TECHNOL SOC J JI Mar. Technol. Soc. J. PD WIN PY 2005 VL 39 IS 4 BP 12 EP 14 PG 3 WC Engineering, Ocean; Oceanography SC Engineering; Oceanography GA 027ZA UT WOS:000236453700004 ER PT J AU Meeson, BW AF Meeson, BW TI Using ocean observing systems to promote lifelong ocean education SO MARINE TECHNOLOGY SOCIETY JOURNAL LA English DT Article AB The coming ocean observing system provides an unprecedented opportunity to change both the public perception of our ocean, and to inspire, captivate and motivate our children, our young adults and our peers to pursue careers allied with the ocean and to become stewards of our planet's ocean. Within this context educators participating in the Ocean Research Interactive Observatory Networks Workshop (January 2004) and in the Integrated Ocean Observing System-Coastal Ocean Observing System and Education Workshop (March 2004) collectively sought to articulate recommendations for education allied with ocean observing systems (global, coastal, in situ, and remote sensing). At these workshops an education network was initiated and workshop recommendations called for creation of a collaborative framework to support and develop the network. This collaborative framework is to be established from existing education networks, be nationally coordinated through a coordinating center and embedded in a larger geography and Earth and space system science education collaborative. Recommendations address several other topics including identification of thematic areas and classes of education activities, availability of data and learning materials in forms that are useful and usable by educators, creating new learning materials where gaps exist, and ensuring that all citizens, especially those from underserved and underrepresented populations are engaged in ocean careers. Efforts are underway in several of these areas including expansion of the education network and identification of education, training and workforce supply and demand issues. C1 NASA, Washington, DC USA. EM b.meeson@ocean.us NR 13 TC 1 Z9 1 U1 1 U2 2 PU MARINE TECHNOLOGY SOC INC PI COLUMBIA PA 5565 STERRETT PLACE, STE 108, COLUMBIA, MD 21044 USA SN 0025-3324 J9 MAR TECHNOL SOC J JI Mar. Technol. Soc. J. PD WIN PY 2005 VL 39 IS 4 BP 41 EP 47 PG 7 WC Engineering, Ocean; Oceanography SC Engineering; Oceanography GA 027ZA UT WOS:000236453700008 ER PT J AU Tweedie, MS Stanitski, DM Snyder, HD Hammond, JN AF Tweedie, MS Stanitski, DM Snyder, HD Hammond, JN TI Follow the world's ocean currents with the Ocean Surface Currents Web site and the Adopt a Drifter Program SO MARINE TECHNOLOGY SOCIETY JOURNAL LA English DT Article AB The ocean surface has provided the interface for commerce, adventure and exploration for millennia. Studies of ocean surface currents play a vital role in our present day understanding of the dynamics at this ocean-atmosphere interface. Using technology to bridge vast distances, students can now reach the oceans and experience real-life challenges that rival those of the space program. In this paper, we detail two efforts using different approaches to engage teachers and their students in the study of ocean surface currents. The NASA-sponsored Ocean Surface Currents Web site (www.oceanmotion.org) provides a comprehensive review of the surface circulation of Earth's ocean and classroom investigations appropriate for various disciplines at the high school level. The site highlights use of data derived from the online satellite data to understand patterns of ocean surface currents and how they relate to issues of exploration, commerce, marine life, weather/climate, natural hazards and national security. Classroom investigations help high school students practice skills matched to national standards, and keyed to topics covered in the traditional high school curriculum and to the stages of the 5 E's teaching and learning model. The NOAA-sponsored Adopt a Drifter Program (ADP) provides an educational opportunity for K-16 teachers to infuse ocean observing system data into their curriculum. The ADP promotes one-on-one partnerships between schools from the United States and international schools where students from both schools mutually adopt a drifting buoy to be deployed from a ship at sea. An educational sticker from each school is adhered to the drifter before deployment and teachers and their students access drifter location, sea surface temperature and/or sea surface pressure data from the drifter online at http://osmc.noaa.gov/ OSMC/adopt, a_drifter.html. These resources better equip teachers with the tools necessary to ignite the interest of students and explain complex relationships between dynamic atmosphere and ocean systems. C1 NASA, Washington, DC 20546 USA. Shippensburg Univ, Shippensburg, PA 17257 USA. Gallaudet Univ, Washington, DC 20002 USA. NOAA, Washington, DC USA. RP Tweedie, MS (reprint author), NASA, Washington, DC 20546 USA. EM diane.stanitski@noaa.gov NR 7 TC 0 Z9 0 U1 0 U2 0 PU MARINE TECHNOLOGY SOC INC PI COLUMBIA PA 5565 STERRETT PLACE, STE 108, COLUMBIA, MD 21044 USA SN 0025-3324 J9 MAR TECHNOL SOC J JI Mar. Technol. Soc. J. PD WIN PY 2005 VL 39 IS 4 BP 83 EP 89 PG 7 WC Engineering, Ocean; Oceanography SC Engineering; Oceanography GA 027ZA UT WOS:000236453700014 ER PT J AU Lee, P Osinski, GR AF Lee, P Osinski, GR TI The Haughton-Mars Project: Overview of science investigations at the Haughton impact structure and surrounding terrains, and relevance to planetary studies SO METEORITICS & PLANETARY SCIENCE LA English DT Editorial Material ID ARCTIC CANADA; CRATER C1 SETI Inst, Mars Inst, Moffett Field, CA 94035 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Canadian Space Agcy, St Hubert, PQ J3Y 8Y9, Canada. RP Lee, P (reprint author), SETI Inst, Mars Inst, MS 245-3 Moffett Field, Moffett Field, CA 94035 USA. NR 27 TC 16 Z9 18 U1 0 U2 4 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD DEC PY 2005 VL 40 IS 12 BP 1755 EP 1758 PG 4 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 011MS UT WOS:000235273000001 ER PT J AU Osinski, GR Lee, P Spray, JG Parnell, J Lim, DSS Bunch, TE Cockell, CS Glass, B AF Osinski, GR Lee, P Spray, JG Parnell, J Lim, DSS Bunch, TE Cockell, CS Glass, B TI Geological overview and cratering model for the Haughton impact structure, Devon Island, Canadian High Arctic SO METEORITICS & PLANETARY SCIENCE LA English DT Review ID SHOCK-WAVE METAMORPHISM; ISOTOPE SYSTEMATICS; TERRESTRIAL IMPACT; U-PB; ROCKS; ASTROBLEME; CHICXULUB; GERMANY; ORIGIN; ATEM AB The Haughton impact structure has been the focus of systematic, multi-disciplinary field and laboratory research activities over the past several years. Regional geological mapping has refined the sedimentary target stratigraphy and constrained the thickness of the sedimentary sequence at the time of impact to similar to 1880 m. New Ar-40-Ar-39 dates place the impact event at similar to 39 Ma, in the late Eocene. Haughton has an apparent crater diameter of similar to 23 km, with an estimated run (final crater) diameter of similar to 16 km. The structure lacks a central topographic peak or peak ring, which is unusual for craters of this size. Geological mapping and sampling reveals that a series of different impactites are present at Haughton. The volumetrically dominant crater-fill impact melt breccias contain a calcite-anhydrite-silicate glass groundmass, all of which have been shown to represent impact-generated melt phases. These impactites are, therefore, stratigraphically and genetically equivalent to coherent impact melt rocks present in craters developed in crystalline targets. The crater-fill impactites provided a heat source that drove a post-impact hydrothermal system. During this time. Haughton would have represented a transient, warm, wet microbial oasis. A subsequent episode of erosion, during which time substantial amounts of impactites were removed, was followed by the deposition of intra-crater lacustrine sediments of the Haughton Formation during the Miocene. Present-day intra-crater lakes and ponds preserve a detailed paleoenvironmental record dating back to the last glaciation in the High Arctic. Modern modification of the landscape is dominated by seasonal regional glacial and niveal melting, and local periglacial processes. The impact processing of target materials improved the opportunities for colonization and has provided several present-day habitats suitable for microbial life that otherwise do not exist in the surrounding terrain. C1 Canadian Space Agcy, St Hubert, PQ J3Y 8Y9, Canada. Univ New Brunswick, Dept Geol, Planetary & Space Sci Ctr, Fredericton, NB E3B 5A3, Canada. SETI Inst, Mars Inst, Moffett Field, CA 94035 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Univ Aberdeen, Dept Geol & Petr Geol, Geofluids Res Grp, Aberdeen AB24 3UE, Scotland. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. No Arizona Univ, Bilby Res Ctr, Dept Geol, Flagstaff, AZ 86011 USA. Open Univ, Planetary & Space Sci Res Inst, Milton Keynes MK7 6AA, Bucks, England. RP Osinski, GR (reprint author), Canadian Space Agcy, St Hubert, PQ J3Y 8Y9, Canada. EM gordon.osinski@space.gc.ca RI Spray, John/J-7504-2013 NR 99 TC 41 Z9 41 U1 2 U2 10 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD DEC PY 2005 VL 40 IS 12 BP 1759 EP 1776 PG 18 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 011MS UT WOS:000235273000002 ER PT J AU Sherlock, SC Kelley, SP Parnell, J Green, P Lee, P Osinsk, GR Cockell, CS AF Sherlock, SC Kelley, SP Parnell, J Green, P Lee, P Osinsk, GR Cockell, CS TI Re-evaluating the age of the Haughton impact event SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID DEVON-ISLAND; HYDROTHERMAL SYSTEM; ARCTIC CANADA; SUDBURY STRUCTURE; FLUID INCLUSION; RIES CRATER; DRILL CORE; AR-40/AR-39; AR-40-AR-39; ROCKS AB We have re-evaluated the published age information for the Haughton impact structure, which was believed to have formed similar to 23 Ma ago during the Miocene age, and report new Ar/Ar laser probe data from shocked basement clasts. This reveals all Eocene age, which is at odds with the published Miocene stratigraphic, apatite fission track and Ar/Ar data; we discuss our new data within this context. We have found that the age of the Haughton impact structure is similar to 39 Ma, which has implications for both crater recolonization models and post-impact hydrothermal activity. Future work on the relationship between flora and fauna within the crater, and others at high latitude, may resolve this paradox. C1 Open Univ, Dept Earth Sci, CEPSAR, Milton Keynes MK7 6AA, Bucks, England. Univ Aberdeen, Kings Coll, Coll Phys Sci, Dept Geol & Petr Geol, Aberdeen AB24 3UE, Scotland. Geotrack Int, Brunswick W, Vic 3055, Australia. SETI Inst, Mars Inst, Moffett Field, CA 94035 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Canadian Space Agcy, St Hubert, PQ J3Y 8Y9, Canada. Open Univ, Planetary & Space Sci Res Inst, CEPSAR, Milton Keynes MK7 6AA, Bucks, England. RP Sherlock, SC (reprint author), Open Univ, Dept Earth Sci, CEPSAR, Walton Hall, Milton Keynes MK7 6AA, Bucks, England. EM s.sherlock@open.ac.uk RI Kelley, Simon/C-5489-2012 OI Kelley, Simon/0000-0002-1756-0480 NR 61 TC 25 Z9 25 U1 0 U2 4 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD DEC PY 2005 VL 40 IS 12 BP 1777 EP 1787 PG 11 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 011MS UT WOS:000235273000003 ER PT J AU Osinski, GR Spray, JG Lee, P AF Osinski, GR Spray, JG Lee, P TI Impactites of the Haughton impact structure, Devon Island, Canadian High Arctic SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID MELT ROCKS; SHOCK METAMORPHISM; CARBON-DIOXIDE; SILICATE MELTS; CRATER; CHICXULUB; YAXCOPOIL-1; MEXICO; RIES; GERMANY AB Contrary to the previous interpretation of a single allochthonous impactite lithology, combined field, optical, and analytical scanning electron microscopy (SEM) studies have revealed the presence of a series of impactites at the Haughton impact structure. In the crater interior. there is a consistent upward sequence from parautochthonous target rocks overlain by parautochthonous lithic (monomict) breccias, through allochthonous lithic (polymict) breccia, into pale grey allochthonous impact melt breccias. The groundmass of the pale grey impact melt breccias consists of microcrystalline calcite, silicate impact melt glass, and anhydrite. Analytical data and microtextures indicate that these phases represent a series of impact-generated melts that were molten at the time of, and following, deposition. Impact melt glass clasts are present in approximately half of the samples studied. Consideration of the groundmass phases and impact glass clasts reveal that impactites of the crater interior contain shock-melted sedimentary material from depths of > 920 to < 1880 in in the pre-impact target sequence. Two principal impactites have been recognized in the near-surface crater rim region of Haughton. Pale yellow-brown allochthonous impact melt breccias and megablocks are overlain by pale grey allochthonous impact melt breccias. The former are derived from depths of > 200 to < 760 m and are interpreted as remnants of the continuous ejecta blanket. The pale grey impact melt breccias, although similar to the impact melt breccias of the crater interior, are more carbonate-rich and do not appear to have incorporated clasts from the crystalline basement. Thus, the spatial distribution of the crater-fill impactites at Haughton, the stratigraphic Succession from target rocks to allochthonous impactites, the recognition of large volumes of impact melt breccias, and their probable original volume are all analogous to characteristics of coherent impact melt layers in comparatively sized structures formed in crystalline targets. C1 Univ New Brunswick, Dept Geol, Planetary & Space Sci Ctr, Fredericton, NB E3B 5A3, Canada. SETI Inst, Mars Inst, Moffett Field, CA 94035 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Canadian Space Agcy, St Hubert, PQ J3Y 8Y9, Canada. RP Osinski, GR (reprint author), Univ New Brunswick, Dept Geol, Planetary & Space Sci Ctr, 2 Bailey Dr, Fredericton, NB E3B 5A3, Canada. EM osinski@lycos.corn RI Spray, John/J-7504-2013 NR 63 TC 25 Z9 25 U1 1 U2 4 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD DEC PY 2005 VL 40 IS 12 BP 1789 EP 1812 PG 24 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 011MS UT WOS:000235273000004 ER PT J AU Tornabene, LL Moersch, JE Osinski, GR Lee, P Wright, SP AF Tornabene, LL Moersch, JE Osinski, GR Lee, P Wright, SP TI Spaceborne visible and thermal infrared lithologic mapping of impact-exposed subsurface lithologies at the Haughton impact structure, Devon Island, Canadian High Arctic: Applications to Mars SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID REFLECTION RADIOMETER ASTER; EMISSION SPECTROMETER EXPERIMENT; MULTISPECTRAL DATA; MARTIAN SURFACE; IMAGING-SYSTEM; MGS-TES; CRATER; SPECTRA; MISSION; SPECTROSCOPY AB This study serves as a proof-of-concept for the technique of using visible-near infrared (VNIR), short-wavelength infrared (SWIR), and thermal infrared (TIR) spectroscopic observations to map impact-exposed subsurface lithologies and stratigraphy on Earth or Mars. The topmost layer, three subsurface layers and undisturbed outcrops of the target sequence exposed just 10 km to the northeast of the 23 km diameter Haughton impact Structure (Devon Island,. Nunavut, Canada) were mapped as distinct spectral units using Landsat 7 ETM+ (VNIR/SWIR) and ASTER (VNIR/SWIR/TIR) multispectral images. Spectral mapping was accomplished by using standard image contrast-stretching algorithms. Both spectral matching and deconvolution algorithms were applied to image-derived ASTER TIR emissivity spectra using spectra from a library of laboratory-measured spectra of minerals (Arizona State University) and whole-rocks (Ward's). These identifications were made without the use of a priori knowledge from the field (i.e., a "blind" analysis). The results from this analysis suggest a sequence of dolomitic rock (in the crater rim), limestone (wall), gypsum-rich carbonate (floor), and limestone again (central Uplift). These matched compositions agree with the lithologic units and the pre-impact stratigraphic sequence as mapped during recent field studies of the Haughton impact structure by Osinski et al. (2005a). Further conformation of the identity of image-derived spectra was confirmed by matching these spectra with laboratory-measured spectra of samples collected from Haughton. The results from the "blind" remote sensing methods used here suggest that these techniques can also be used to understand subsurface lithologies on Mars, where ground truth knowledge may not be generally available. C1 Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. Canadian Space Agcy, John H Chaoman Space Ctr, Longueuil, PQ J3Y 8Y9, Canada. SETI Inst, Mars Inst, Moffett Field, CA 94035 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Arizona State Univ, Dept Geol Sci, Tempe, AZ 85287 USA. RP Tornabene, LL (reprint author), Univ Tennessee, Dept Earth & Planetary Sci, Knoxville, TN 37996 USA. EM ltornabe@utk.edu RI Moersch, Jeffrey/F-7189-2010 NR 76 TC 3 Z9 3 U1 0 U2 8 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD DEC PY 2005 VL 40 IS 12 BP 1835 EP 1858 PG 24 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 011MS UT WOS:000235273000006 ER PT J AU Osinski, GR Lee, P Parnell, J Spray, JG Baron, MT AF Osinski, GR Lee, P Parnell, J Spray, JG Baron, MT TI A case study of impact-induced hydrothermal activity: The Haughton impact structure, Devon Island, Canadian high arctic SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID REACTIONS FORMING PYRITE; RIES CRATER; FLUID INCLUSION; DRILL CORE; MARCASITE; GERMANY; SYSTEM; MARS; MELT; MEXICO AB The well-preserved state and excellent exposure at the 39 Ma Haughton impact structure, 23 km in diameter, allows a clearer picture to be made of the nature and distribution of hydrothermal deposits within mid-size complex impact craters. A moderate- to low-temperature hydrothermal system was generated at Haughton by the interaction of groundwaters with the hot impact melt breccias that filled the interior of the crater. Four distinct settings and styles of hydrothermal mineralization are recognized at Haughton: a) Wigs and veins within the impact melt breccias, with an increase in intensity of alteration towards the base; b) cementation of brecciated lithologies in the interior of the central uplift; c) intense veining around the heavily faulted and fractured outer margin of the central uplift; and d) hydrothermal pipe structures or gossans and mineralization along fault surfaces around the faulted crater rim. Each setting is associated with a different suite of hydrothermal minerals that were deposited at different stages in the development of the hydrothermal system. Minor, early quartz precipitation in the impact melt breccias was followed by the deposition of calcite and marcasite within cavities and fractures, plus minor celestite, barite, and fluorite. This occurred at temperatures of at least 200 degrees C and down to similar to 100-120 degrees C. Hydrothermal circulation through the faulted crater rim with the deposition of calcite, quartz, marcasite, and pyrite, occurred at similar temperatures. Quartz mineralization within breccias of the interior of the central uplift occurred in two distinct episodes (similar to 250 down to similar to 90 degrees C, and < 60 degrees C). With continued cooling (< 90 degrees C), calcite and quartz were precipitated in vugs and veins within the impact melt breccias. Calcite veining around the outer margin of the central uplift occurred at temperatures of similar to 150 degrees C down to < 60 degrees C. Mobilization of hydrocarbons from the country rocks occurred during formation of the higher temperature calcite veins (> 80 degrees C). Appreciation of the structural features of impact craters has proven to be key to understanding the distribution of hydrothermal deposits at Haughton. C1 Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA. NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. Univ Aberdeen, Dept Geol & Petr Geol, Geofluids Res Grp, Aberdeen AB24 3UE, Scotland. Univ New Brunswick, Dept Geol, Planetary & Space Sci Ctr, Fredericton, NB E3B 5A3, Canada. Canadian Space Agcy, St Hubert, PQ J3Y 8Y9, Canada. RP Osinski, GR (reprint author), Univ Arizona, Lunar & Planetary Lab, 1629 E Univ Blvd, Tucson, AZ 85721 USA. EM osinski@lycos.com RI Spray, John/J-7504-2013 NR 63 TC 48 Z9 48 U1 0 U2 12 PU WILEY-BLACKWELL PI HOBOKEN PA 111 RIVER ST, HOBOKEN 07030-5774, NJ USA SN 1086-9379 EI 1945-5100 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD DEC PY 2005 VL 40 IS 12 BP 1859 EP 1877 PG 19 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 011MS UT WOS:000235273000007 ER PT J AU Parnell, J Lee, P Osinski, GR Cockell, CS AF Parnell, J Lee, P Osinski, GR Cockell, CS TI Application of organic geochemistry to detect signatures of organic matter in the Haughton impact structure SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID DEVON ISLAND; HYDROTHERMAL ACTIVITY; TARGET ROCKS; CANADA; SWEDEN; CRATER; FOSSILS; NORWAY; LIFE; OILS AB Organic geochemistry applied to samples of bedrock and surface sediment from the Haughton impact structure detects a range of signatures representing the impact event and the transfer of organic matter from the crater bedrock to its erosion products. The bedrock dolomite contains hydrocarbon-bearing fluid inclusions which were incorporated before the impact event. Comparison of biomarker data from the hydrocarbons in samples inside and Outside of the crater show the thermal signature of an impact. The occurrence of hydrocarbon inclusions in hydrothermal mineral samples shows that organic matter was mobilized and migrated in the immediate aftermath of the impact. The hydrocarbon signature was then transferred from bedrock to the crater-fill lacustrine deposits and present-day sediments in the crater, including wind-blown detritus in snow/ice. Separate signatures are detected from modern microbial life in crater rock and sediment samples. Signatures in Haughton crater samples are readily detectable because they include hydrocarbons generated by the burial of organic matter. This type of organic matter is not expected in crater samples oil other planets, but the Haughton data show that, using very high resolution detection of organic Compounds,. any signature of primitive life in the crater rocks Could be transferred to surface detritus and so extend the sampling medium. C1 Univ Aberdeen, Dept Geol & Petr Geol, Aberdeen AB24 3UE, Scotland. NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. Univ Arizona, Dept Planetary Sci, Lunar & Planetary Lab, Tucson, AZ 85721 USA. British Antarctic Survey, Cambridge CB3 0ET, England. RP Parnell, J (reprint author), Univ Aberdeen, Dept Geol & Petr Geol, Aberdeen AB24 3UE, Scotland. EM j.parnell@abdn.ac.uk NR 32 TC 2 Z9 2 U1 0 U2 2 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD DEC PY 2005 VL 40 IS 12 BP 1879 EP 1885 PG 7 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 011MS UT WOS:000235273000008 ER PT J AU Osinski, GR Lee, P AF Osinski, GR Lee, P TI Intra-crater sedimentary deposits at the Haughton impact structure, Devon Island, Canadian High Arctic SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID SOUTHERN GERMANY; MARS; ASTROBLEME; BIOHERMS; MIOCENE; LAKES; FILL AB Detailed field mapping has revealed the presence of a series of intra-crater sedimentary deposits within the interior of the Haughton impact structure, Devon Island, Canadian High Arctic. Coarse-grained, well-sorted, pate gray lithic sandstones (reworked impact melt breccias) unconformably overlie pristine impact melt breccias and attest to an episode of erosion,. during which time significant quantities of impact melt breccias were removed. The reworked impact melt breccias are, in turn, unconformably overlain by paleolacustrine sediments of the Miocene Haughton Formation. Sediments of the Haughton Formation were clearly derived from pre-impact lower Paleozoic target rocks of the Allen Bay Formation, which form the crater rim in the northern, western, and southern regions of the Haughton structure. Collectively, these field relationships indicate that the Haughton Formation was deposited up to several million years after the formation of the Haughton crater and that they do not, therefore, represent an immediate, post-impact crater lake deposit. This is consistent with new isotopic dating of impactites from Haughton that indicate an Eocene age for the impact event (Sherlock et al. 2005). In addition, isolated deposits of post-Miocene intra-crater glacigenic and fluvioglacial sediments were found lying unconformably over remnants of the Haughton Formation, impact melt breccias, and other pre-impact target rock formations. These deposits provide clear evidence for glaciation at the Haughton crater. The wealth and complexity of geological and climatological information preserved as intra-crater deposits at Haughton suggests that craters on Mars with intra-crater sedimentary records might present us with similar opportunities, but also possibly significant challenges. C1 Mars Inst, Vancouver, BC V6B 1B5, Canada. SETI Inst, Mars Inst, Moffett Field, CA 94035 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. RP Osinski, GR (reprint author), Mars Inst, 980 Seymour St,Suite 1306, Vancouver, BC V6B 1B5, Canada. EM osinski@lycos.com NR 37 TC 10 Z9 10 U1 0 U2 3 PU METEORITICAL SOC PI FAYETTEVILLE PA DEPT CHEMISTRY/BIOCHEMISTRY, UNIV ARKANSAS, FAYETTEVILLE, AR 72701 USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD DEC PY 2005 VL 40 IS 12 BP 1887 EP 1899 PG 13 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 011MS UT WOS:000235273000009 ER PT J AU Cockell, CS Lee, P Broady, P Lim, DSS Osinski, GR Parnell, J Koeberl, C Pesonen, L Salminen, J AF Cockell, CS Lee, P Broady, P Lim, DSS Osinski, GR Parnell, J Koeberl, C Pesonen, L Salminen, J TI Effects of asteroid and comet impacts on habitats for lithophytic organisms - A synthesis SO METEORITICS & PLANETARY SCIENCE LA English DT Article ID DEVON ISLAND; POLAR DESERT; HAUGHTON FORMATION; MICROBIAL ACTIVITY; ARCTIC CANADA; CRATER; SHOCK; MICROORGANISMS; ALGAE; ROCKS AB Asteroid and cornet impacts can have a profound influence on the habitats available for lithophytic microorganisms. Using evidence from the Haughton impact structure, Nunavut, Canadian High Arctic, we describe the role of impacts in influencing, the nature of the lithophytic ecological niche. Impact-induced increases in rock porosity and fracturing can result in the formation of cryptoendolithic habitats. In some cases and depending upon the target material, an increase in rock translucence can yield new habitats for photosynthetic cryptoendoliths. Chasmoendolithic habitats are associated with cracks and cavities connected to the surface of the rock and are commonly increased in abundance as a result of impact bulking. Chasmoendolithic habitats require less specific geological conditions than are required for cryptoendolithic habitats, and their formation is likely to be common to most impact events. Impact events are unlikely to have all influence on epilithic and hypolithic habitats except in rare cases, where, for example, the formation of impact glasses might yield new hypolithic habitats. We present a synthetic understanding of the influence of asteroid and comet impacts on the availability and characteristics of rocky habitats for microorganisms. C1 Open Univ, Planetary & Space Sci Res Inst, Milton Keynes MK7 6AA, Bucks, England. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Univ Canterbury, Sch Biol Sci, Christchurch 1, New Zealand. Canadian Space Agcy, St Hubert, PQ J3Y 8Y9, Canada. Univ Aberdeen, Dept Geol, Aberdeen AB24 3UE, Scotland. Univ Vienna, Dept Geol Sci, A-1090 Vienna, Austria. Univ Helsinki, Dept Phys Sci, Div Geophys, FIN-00014 Helsinki, Finland. RP Cockell, CS (reprint author), Open Univ, Planetary & Space Sci Res Inst, Milton Keynes MK7 6AA, Bucks, England. EM c.s.cockell@open.ac.uk OI Salminen, Johanna/0000-0001-5347-1920 NR 91 TC 29 Z9 29 U1 3 U2 8 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 1086-9379 J9 METEORIT PLANET SCI JI Meteorit. Planet. Sci. PD DEC PY 2005 VL 40 IS 12 BP 1901 EP 1914 PG 14 WC Geochemistry & Geophysics SC Geochemistry & Geophysics GA 011MS UT WOS:000235273000010 ER PT J AU Chen, Y Wang, Q Kayali, S AF Chen, Y Wang, Q Kayali, S TI A statistical approach to characterizing the reliability of systems utilizing HBT devices SO MICROELECTRONICS RELIABILITY LA English DT Article; Proceedings Paper CT Workshop on Reliability of Compound Semiconductors (ROCS) CY OCT 24, 2004 CL Monterey, CA SP JEDEC JC 14 7, IEEE Electron Devices Soc ID THERMAL-RESISTANCE; JUNCTION TEMPERATURE AB This paper describes a statistical approach to simulating the reliability of systems with HBT devices. Compared to the conventional worst-case method, the described approach utilizes statistical reliability information of the HBT individual devices, along with analysis on the critical paths of the system, to provide more accurate and more comprehensive reliability evaluation of the systems utilizing HBT devices. (c) 2005 Elsevier Ltd. All rights reserved. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Calif State Univ Los Angeles, Dept Elect & Comp Engn, Chico, CA 95926 USA. RP CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. EM yuan.chen@jpl.nasa.gov NR 16 TC 1 Z9 1 U1 0 U2 2 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0026-2714 J9 MICROELECTRON RELIAB JI Microelectron. Reliab. PD DEC PY 2005 VL 45 IS 12 BP 1869 EP 1874 DI 10.1016/j.microrel.2005.01.014 PG 6 WC Engineering, Electrical & Electronic; Nanoscience & Nanotechnology; Physics, Applied SC Engineering; Science & Technology - Other Topics; Physics GA 989ZH UT WOS:000233712400008 ER PT J AU Fortney, JJ AF Fortney, JJ TI The effect of condensates on the characterization of transiting planet atmospheres with transmission spectroscopy SO MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY LA English DT Article DE radiative transfer; planetary systems ID EXTRASOLAR GIANT PLANETS; HD 209458B; DWARF ATMOSPHERES; JUPITER; CLOUDS; AEROSOLS; SPECTRA; MODELS; TEMPERATURES; CARBON AB Through a simple physical argument we show that the slant optical depth through the atmosphere of a 'hot Jupiter' planet is similar to 35-90 times greater than the normal optical depth. This not unexpected result has direct consequences for the method of transmission spectroscopy for characterizing the atmospheres of transiting giant planets. The atmospheres of these planets likely contain minor condensates and hazes, which at normal viewing geometry have negligible optical depth, but at slant viewing geometry have appreciable optical depth that can obscure absorption features of gaseous atmospheric species. We identify several possible condensates. We predict that this is a general masking mechanism for all planets, not just for HD 209458b, and will lead to weaker than expected or undetected absorption features. Constraints on an atmosphere from transmission spectroscopy are not the same as constraints on an atmosphere at normal viewing geometry. C1 NASA, Ames Res Ctr, Space Sci & Astrobiol Div, Moffett Field, CA 94035 USA. RP Fortney, JJ (reprint author), NASA, Ames Res Ctr, Space Sci & Astrobiol Div, MS 245-3, Moffett Field, CA 94035 USA. EM jfortney@arc.nasa.gov OI Fortney, Jonathan/0000-0002-9843-4354 NR 39 TC 80 Z9 80 U1 1 U2 5 PU WILEY-BLACKWELL PI MALDEN PA COMMERCE PLACE, 350 MAIN ST, MALDEN 02148, MA USA SN 0035-8711 J9 MON NOT R ASTRON SOC JI Mon. Not. Roy. Astron. Soc. PD DEC 1 PY 2005 VL 364 IS 2 BP 649 EP 653 DI 10.1111/j.1365-2966.2005.09587.x PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 984LZ UT WOS:000233307700024 ER PT J AU Lee, C Bae, SY Mobasser, S Manohara, H AF Lee, C Bae, SY Mobasser, S Manohara, H TI A novel silicon nanotips antireflection surface for the micro sun sensor SO NANO LETTERS LA English DT Article AB We have developed a new technique to fabricate an antireflection surface using silicon nanotips for use on a micro Sun sensor for Mars rovers. We have achieved randomly distributed nanotips of radii spanning from 20 to 100 nm and aspect ratio of similar to 200 using a two-step dry etching process. The 30 degrees specular reflectance at the target wavelength of 1 mu m is only about 0.09%, nearly 3 orders of magnitude lower than that of bare silicon, and the hemispherical reflectance is similar to 8%. When the density and aspect ratio of these nanotips are changed, a change in reflectance is demonstrated. When surfaces are covered with these nano-tips, the critical problem of ghost images that are caused by multiple internal reflections in a micro Sun sensor was solved. C1 CALTECH, Pasadena, CA 91125 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Lee, C (reprint author), CALTECH, 1200 Calif Blvd, Pasadena, CA 91125 USA. EM Choonsup.Lee@jpl.nasa.gov; Harish.Manohara@jpl.nasa.gov NR 9 TC 126 Z9 127 U1 0 U2 23 PU AMER CHEMICAL SOC PI WASHINGTON PA 1155 16TH ST, NW, WASHINGTON, DC 20036 USA SN 1530-6984 J9 NANO LETT JI Nano Lett. PD DEC PY 2005 VL 5 IS 12 BP 2438 EP 2442 DI 10.1021/nl0517161 PG 5 WC Chemistry, Multidisciplinary; Chemistry, Physical; Nanoscience & Nanotechnology; Materials Science, Multidisciplinary; Physics, Applied; Physics, Condensed Matter SC Chemistry; Science & Technology - Other Topics; Materials Science; Physics GA 998YY UT WOS:000234357000019 PM 16351193 ER PT J AU Le Novere, N Finney, A Hucka, M Bhalla, US Campagne, F Collado-Vides, J Crampin, EJ Halstead, M Klipp, E Mendes, P Nielsen, P Sauro, H Shapiro, B Snoep, JL Spence, HD Wanner, BL AF Le Novere, N Finney, A Hucka, M Bhalla, US Campagne, F Collado-Vides, J Crampin, EJ Halstead, M Klipp, E Mendes, P Nielsen, P Sauro, H Shapiro, B Snoep, JL Spence, HD Wanner, BL TI Minimum information requested in the annotation of biochemical models (MIRIAM) SO NATURE BIOTECHNOLOGY LA English DT Article ID BIOLOGY MARKUP LANGUAGE; SYSTEMS BIOLOGY; PROTEIN KNOWLEDGEBASE; ESCHERICHIA-COLI; ENZYME DATABASE; RESOURCE; GENOME; REPRESENTATION; STANDARDS; NETWORKS AB Most of the published quantitative models in biology are lost for the community because they are either not made available or they are insufficiently characterized to allow them to be reused. The lack of a standard description format, lack of stringent reviewing and authors' carelessness are the main causes for incomplete model descriptions. With today's increased interest in detailed biochemical models, it is necessary to define a minimum quality standard for the encoding of those models. We propose a set of rules for curating quantitative models of biological systems. These rules define procedures for encoding and annotating models represented in machine-readable form. We believe their application will enable users to (i) have confidence that curated models are an accurate reflection of their associated reference descriptions, (ii) search collections of curated models with precision, (iii) quickly identify the biological phenomena that a given curated model or model constituent represents and (iv) facilitate model reuse and composition into large subcellular models. C1 European Bioinformat Inst, Hinxton CB10 1SD, England. Physiom PLC, Magdalen Ctr, Oxford OX4 4GA, England. CALTECH, Pasadena, CA 91125 USA. UAS, TIFR, Natl Ctr Biol Sci, Bangalore 560065, Karnataka, India. Cornell Univ, Weill Med Coll, Inst Computat Biomed, New York, NY 10021 USA. Univ Nacl Autonoma Mexico, Ctr Genom Sci, Cuernavaca 62100, Morelos, Mexico. Univ Auckland, Bioengn Inst, Auckland 1, New Zealand. Univ Auckland, Dept Engn Sci, Auckland 1, New Zealand. Max Planck Inst Mol Genet, BCB, D-14195 Berlin, Germany. Virginia Tech, Virginia Bioinformat Inst, Blacksburg, VA 24061 USA. Keck Grad Inst, Claremont, CA 91711 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. Univ Stellenbosch, Dept Biochem, Triple J Grp Mol Cell Physiol, ZA-7602 Matieland, South Africa. GlaxoSmithKline Res & Dev Ltd, Dept Sci Comp & Mathemat Modeling, Med Res Ctr, Stevenage SG1 2NY, Herts, England. Purdue Univ, Dept Biol Sci, W Lafayette, IN 47907 USA. RP Le Novere, N (reprint author), European Bioinformat Inst, Hinxton CB10 1SD, England. EM lenov@ebi.ac.uk RI Campagne, Fabien/F-5158-2010; Le Novere, Nicolas/F-9973-2010; Hucka, Michael/B-1896-2012; Nielsen, Poul/A-5814-2009; OI Le Novere, Nicolas/0000-0002-6309-7327; Nielsen, Poul/0000-0002-4704-0179; Sauro, Herbert/0000-0002-3659-6817; Snoep, Jacky/0000-0002-0405-8854; Campagne, Fabien/0000-0001-6237-3564; Mendes, Pedro/0000-0001-6507-9168 NR 44 TC 257 Z9 260 U1 2 U2 8 PU NATURE PUBLISHING GROUP PI NEW YORK PA 345 PARK AVENUE SOUTH, NEW YORK, NY 10010-1707 USA SN 1087-0156 J9 NAT BIOTECHNOL JI Nat. Biotechnol. PD DEC PY 2005 VL 23 IS 12 BP 1509 EP 1515 DI 10.1038/nbt1156 PG 7 WC Biotechnology & Applied Microbiology SC Biotechnology & Applied Microbiology GA 992ED UT WOS:000233866300027 PM 16333295 ER PT J AU Ehrenreich, T Miller, K Gee, P Kessel, Q Pollack, E Smith, WW Djuric, N Lozano, J Smith, SJ Chutjian, A AF Ehrenreich, T Miller, K Gee, P Kessel, Q Pollack, E Smith, WW Djuric, N Lozano, J Smith, SJ Chutjian, A TI Photon emission resulting from collisions of O5+ with CO SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION B-BEAM INTERACTIONS WITH MATERIALS AND ATOMS LA English DT Article; Proceedings Paper CT 18th International Conference on Application of Accelerators in Research and Industry (CAARI) CY OCT 10-15, 2004 CL Ft Worth, TX SP US DOE, Natl Sci Fdn, Int Atom Energy Agcy, Natl Canc Inst, Sadia Natl Lab, Oak Ridge Natl Lab, Oak Ridge Associated Univ, Los Alamos Natl Lab, Synergy Vaccum, Ft Worth Convent & Vistors Bureau, Elsevier B V, Univ N Texas DE electron capture; solar wind; comets AB As part of an investigation of the interactions between solar-wind ions and cometary gases, UV/X-ray and optical measurements of the photons resulting from collisions of 051 with CO have been made. Although O5+ is not a major solar-wind ion, its interaction with CO yields information applicable to other solar-wind ion interactions. The data show general agreement with the "over-the-barrier" model prediction that electrons are likely to be captured into the n = 4 levels of the resulting O4+ ion. Not only are the UV/X-ray lines measured in the 10-20 nm range with the UV/X-ray spectrometer consistent with this prediction, but the general lack of optical lines in the optical spectrometer range of 350-850 nm support the model for O5+-Co collisions. Only one optical line may be attributed to the decay of excited O4+ ions while most of the observed optical lines are attributable to atomic and molecular excitation of the CO target. (c) 2005 Elsevier B.V. All rights reserved. C1 Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. Univ Connecticut, Inst Mat Sci, Storrs, CT 06269 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Kessel, Q (reprint author), Univ Connecticut, Dept Phys, Storrs, CT 06269 USA. EM quentin.kessel@uconn.edu NR 4 TC 1 Z9 1 U1 1 U2 1 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-583X J9 NUCL INSTRUM METH B JI Nucl. Instrum. Methods Phys. Res. Sect. B-Beam Interact. Mater. Atoms PD DEC PY 2005 VL 241 IS 1-4 BP 125 EP 128 DI 10.1016/j.nimb.2005.07.075 PG 4 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Atomic, Molecular & Chemical; Physics, Nuclear SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 997PX UT WOS:000234260000030 ER PT J AU Akkurt, H Groves, JL Trombka, J Starr, R Evans, L Floyd, S Hoover, R Lim, L McClanahan, T James, R McCoy, T Schweitzer, J AF Akkurt, H Groves, JL Trombka, J Starr, R Evans, L Floyd, S Hoover, R Lim, L McClanahan, T James, R McCoy, T Schweitzer, J TI Pulsed neutron generator system for astrobiological and geochemical exploration of planetary bodies SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION B-BEAM INTERACTIONS WITH MATERIALS AND ATOMS LA English DT Article; Proceedings Paper CT 18th International Conference on Application of Accelerators in Research and Industry (CAARI) CY OCT 10-15, 2004 CL Ft Worth, TX SP US DOE, Natl Sci Fdn, Int Atom Energy Agcy, Natl Canc Inst, Sadia Natl Lab, Oak Ridge Natl Lab, Oak Ridge Associated Univ, Los Alamos Natl Lab, Synergy Vaccum, Ft Worth Convent & Vistors Bureau, Elsevier B V, Univ N Texas DE neutron generator; subsurface elemental composition; planetary surveys AB A pulsed neutron/gamma-ray detection system for use on rovers to survey the elemental concentrations of Martian and Lunar surface and subsurface materials is evaluated. A robotic survey system combining a pulsed neutron generator (PNG) and detectors (gamma ray and neutron) can measure the major constituents to a depth of about 30 cm. Scanning mode measurements can give the major elemental concentrations while the rover is moving; analyzing mode measurements can give a detailed elemental analysis of the adjacent material when the rover is stationary. A detailed map of the subsurface elemental concentrations will provide invaluable information relevant to some of the most fundamental astrobiological questions including the presence of water, biogenic activity, life habitability and deposition processes. (c) 2005 Elsevier B.V. All rights reserved. C1 Schlumberger Princeton Technol Ctr, Princeton Jct, NJ 07605 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Catholic Univ Amer, Washington, DC 20064 USA. Comp Sci Corp, Lanham, MD 20706 USA. Brookhaven Natl Lab, Upton, NY 11973 USA. Smithsonian Inst, Natl Museum Amer Hist, Washington, DC 20560 USA. Univ Connecticut, Storrs, CT 06269 USA. RP Groves, JL (reprint author), Schlumberger Princeton Technol Ctr, 20 Wallace Rd, Princeton Jct, NJ 07605 USA. EM groves@princeton.oilfield.slb.com RI McClanahan, Timothy/C-8164-2012; Lim, Lucy/C-9557-2012 OI Lim, Lucy/0000-0002-9696-9654 NR 7 TC 6 Z9 6 U1 0 U2 4 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-583X J9 NUCL INSTRUM METH B JI Nucl. Instrum. Methods Phys. Res. Sect. B-Beam Interact. Mater. Atoms PD DEC PY 2005 VL 241 IS 1-4 BP 232 EP 237 DI 10.1016/j.nimb.2005.07.029 PG 6 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Atomic, Molecular & Chemical; Physics, Nuclear SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 997PX UT WOS:000234260000052 ER PT J AU Schweitzer, JS Trombka, JI Floyd, S Selavka, C Zeosky, G Gahn, N McClanahan, T Burbine, T AF Schweitzer, JS Trombka, JI Floyd, S Selavka, C Zeosky, G Gahn, N McClanahan, T Burbine, T TI Portable generator-based XRF instrument for non-destructive analysis at crime scenes SO NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION B-BEAM INTERACTIONS WITH MATERIALS AND ATOMS LA English DT Article; Proceedings Paper CT 18th International Conference on Application of Accelerators in Research and Industry (CAARI) CY OCT 10-15, 2004 CL Ft Worth, TX SP US DOE, Natl Sci Fdn, Int Atom Energy Agcy, Natl Canc Inst, Sadia Natl Lab, Oak Ridge Natl Lab, Oak Ridge Associated Univ, Los Alamos Natl Lab, Synergy Vaccum, Ft Worth Convent & Vistors Bureau, Elsevier B V, Univ N Texas DE portable XRF instrument; gunshot residue; blood; semen; Schottky CdTe detector; X-ray generator AB Unattended and remote detection systems find applications in space exploration, telemedicine, teleforensics, homeland security and nuclear non-proliferation programs. The National Institute of Justice (NIJ) and the National Aeronautics and Space Administration's (NASA) Goddard Space Flight Center (GSFC) have teamed up to explore the use of NASA developed technologies to help criminal justice agencies and professionals investigate crimes. The objective of the program is to produce instruments and communication networks that have application within both NASA's space program and NIJ, together with state and local forensic laboratories. A general-purpose X-ray fluorescence system has been built for non-destructive analyses of trace and invisible material at crime scenes. This portable instrument is based on a generator that can operate to 60 kV and a Schottky CdTe detector. The instrument has been shown to be successful for the analysis of gunshot residue and a number of bodily fluids at crime scenes. (c) 2005 Elsevier B.V. All rights reserved. C1 Univ Connecticut, Dept Phys, Unit 3046, Storrs, CT 06269 USA. Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Massachusetts State Police Crime Lab, Sudbury, MA 01776 USA. Forens Invest Ctr, Crime Lab, Albany, NY 12226 USA. Milwaukee Cty Dist Attorneys Off, Milwaukee, WI 53233 USA. RP Schweitzer, JS (reprint author), Univ Connecticut, Dept Phys, Unit 3046, Storrs, CT 06269 USA. EM schweitz@phys.uconn.edu RI McClanahan, Timothy/C-8164-2012 NR 5 TC 18 Z9 18 U1 1 U2 12 PU ELSEVIER SCIENCE BV PI AMSTERDAM PA PO BOX 211, 1000 AE AMSTERDAM, NETHERLANDS SN 0168-583X J9 NUCL INSTRUM METH B JI Nucl. Instrum. Methods Phys. Res. Sect. B-Beam Interact. Mater. Atoms PD DEC PY 2005 VL 241 IS 1-4 BP 816 EP 819 DI 10.1016/j.nimb.2005.07.137 PG 4 WC Instruments & Instrumentation; Nuclear Science & Technology; Physics, Atomic, Molecular & Chemical; Physics, Nuclear SC Instruments & Instrumentation; Nuclear Science & Technology; Physics GA 997PX UT WOS:000234260000169 ER PT J AU Refaat, TF Abedin, MN Bhat, IB Xiao, YG AF Refaat, TF Abedin, MN Bhat, IB Xiao, YG TI Sb-based two-color photodetector fabrication and characterization SO OPTICAL ENGINEERING LA English DT Article DE infrared; two-color; detectors; epitaxy; spectral response AB Sb-based dual-band detectors were fabricated and characterized. The first band consists of an InGaAsSb pn junction for long wavelength detection, while the second band consists of a GaSb pn junction for shorter wavelength detection. Both bands were grown, lattice-matched to a GaSb substrate, using metal-organic vapor phase epitaxy. Three metal contacts were deposited to access the individual junctions. Spectral response measurements indicated either independent operation of both detectors simultaneously, or bias selective operation for one detector while serially accessing both devices. (c) 2005 Society of Photo-Optical Instrumentation Engineers. C1 NASA, Langley Res Ctr, Sci & Technol Corp, Hampton, VA 23681 USA. NASA, Langley Res Ctr, Pass Sensor Syst Branch, Hampton, VA 23681 USA. Rensselaer Polytech Inst, Dept Elect Comp & Syst Engn, Troy, NY 12180 USA. RP Refaat, TF (reprint author), NASA, Langley Res Ctr, Sci & Technol Corp, 5 Dryden St,MS 468, Hampton, VA 23681 USA. NR 6 TC 1 Z9 2 U1 0 U2 1 PU SPIE-INT SOCIETY OPTICAL ENGINEERING PI BELLINGHAM PA 1000 20TH ST, PO BOX 10, BELLINGHAM, WA 98225 USA SN 0091-3286 J9 OPT ENG JI Opt. Eng. PD DEC PY 2005 VL 44 IS 12 AR 120501 DI 10.1117/1.2147576 PG 3 WC Optics SC Optics GA 006LE UT WOS:000234898200002 ER PT J AU Weber, AL AF Weber, AL TI Growth of organic microspherules in sugar-ammonia reactions SO ORIGINS OF LIFE AND EVOLUTION OF BIOSPHERES LA English DT Article DE sugar chemistry; sugar-ammonia reaction; erythrose - maillard reaction; microspherule growth; prebiotic chemistry; prebiotic polymerization; origin of life ID MILD AQUEOUS CONDITIONS; EARLY EARTH; CHEMICAL EVOLUTION; MAILLARD REACTION; PRIMITIVE EARTH; AMINO-ACIDS; CARBON; ATMOSPHERE; WATER; FORMALDEHYDE AB Reaction of small sugars of less than four carbons with ammonia in water yielded organic microspherules generally less than ten microns in size. The time course of microspherule growth was examined for the D-erythrose-ammonia reaction that yielded microspherules attached to the glass walls of containers. Measurements were made of the elemental composition and infrared spectrum of the microspherule material. These viscose semi-solid microspherules are viewed as possible containers for prebiotic catalytic processes relevant to the origin of life. C1 NASA, Ames Res Ctr, SETI Inst, Moffett Field, CA 94035 USA. RP Weber, AL (reprint author), NASA, Ames Res Ctr, SETI Inst, Mail Stop 239-4, Moffett Field, CA 94035 USA. EM aweber@mailarc.nasa.gov NR 46 TC 13 Z9 16 U1 0 U2 5 PU SPRINGER PI DORDRECHT PA VAN GODEWIJCKSTRAAT 30, 3311 GZ DORDRECHT, NETHERLANDS SN 0169-6149 J9 ORIGINS LIFE EVOL B JI Orig. Life Evol. Biosph. PD DEC PY 2005 VL 35 IS 6 BP 523 EP 536 DI 10.1007/s11084-005-0234-1 PG 14 WC Biology SC Life Sciences & Biomedicine - Other Topics GA 018QB UT WOS:000235778800002 PM 16254690 ER PT J AU Cohen, HS Bloomberg, JJ Mulavara, AP AF Cohen, HS Bloomberg, JJ Mulavara, AP TI Obstacle avoidance in novel visual environments improved by variable practice training SO PERCEPTUAL AND MOTOR SKILLS LA English DT Article ID MOTOR SKILL; VARIABILITY; ADAPTATION; INTERFERENCE AB Motor performance on simple tasks improves after training in variable practice. We asked if locomotor skill during an obstacle-avoidance task in a novel sensorimotor environment improved through training in variable practice on other complex tasks. 40 normal adults practiced gross motor skills while wearing either sham lenses, one of several visual distortion lens (constant practice), or three different visual distortion lenses (variable practice). Posttests on obstacle avoidance with novel lenses showed significantly better scores with variable practice and one of the constant groups vs sham lenses. Constant and variable practice groups did not differ. Thus, performance in a novel environment improves after training on similar type novelty, even when practice and test conditions differ. Constant practice was effective only if the Subjects used the lens efficacious in training. Variable practice increases the likelihood of efficacious training when adaptive performance is required in a novel environment. C1 Baylor Coll Med, Bobby R Alford Dept Otolaryngol Head & Neck Surg, Houston, TX 77030 USA. NASA, Lyndon B Johnson Space Ctr, Neurosci Labs, Houston, TX 77058 USA. Baylor Coll Med, Natl Space Biomed Res Inst, Houston, TX 77030 USA. RP Cohen, HS (reprint author), Baylor Coll Med, Dept Otolaryngol, 1 Baylor Plaza, Houston, TX 77030 USA. EM hcohen@bcm.tmc.edu FU NIDCD NIH HHS [DC04167] NR 13 TC 14 Z9 14 U1 0 U2 0 PU PERCEPTUAL MOTOR SKILLS PI MISSOULA PA PO BOX 9229, MISSOULA, MT 59807 USA SN 0031-5125 J9 PERCEPT MOTOR SKILL JI Percept. Mot. Skills PD DEC PY 2005 VL 101 IS 3 BP 853 EP 861 DI 10.2466/pms.101.3.853-861 PG 9 WC Psychology, Experimental SC Psychology GA 006EL UT WOS:000234878200019 PM 16491689 ER PT J AU Duda, KA Abrams, M AF Duda, KA Abrams, M TI ASTER and USGS EROS disaster response: Emergency imaging after Hurricane Katrina SO PHOTOGRAMMETRIC ENGINEERING AND REMOTE SENSING LA English DT Article C1 USGS, Ctr Earth Resources Observat & Sci, Sci Applicat Int Corp, Sioux Falls, SD 57198 USA. CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP Duda, KA (reprint author), USGS, Ctr Earth Resources Observat & Sci, Sci Applicat Int Corp, Sioux Falls, SD 57198 USA. EM duda@usgs.gov; Michael.J.Abrams@jpl.nasa.gov NR 3 TC 4 Z9 4 U1 0 U2 3 PU AMER SOC PHOTOGRAMMETRY PI BETHESDA PA 5410 GROSVENOR LANE SUITE 210, BETHESDA, MD 20814-2160 USA SN 0099-1112 J9 PHOTOGRAMM ENG REM S JI Photogramm. Eng. Remote Sens. PD DEC PY 2005 VL 71 IS 12 BP 1346 EP 1350 PG 5 WC Geography, Physical; Geosciences, Multidisciplinary; Remote Sensing; Imaging Science & Photographic Technology SC Physical Geography; Geology; Remote Sensing; Imaging Science & Photographic Technology GA 994TU UT WOS:000234054900001 ER PT J AU Estep, L Carter, GA AF Estep, L Carter, GA TI Derivative analysis of AVIRIS data for crop stress detection SO PHOTOGRAMMETRIC ENGINEERING AND REMOTE SENSING LA English DT Article ID 2ND DERIVATIVES; CORN LEAVES; REFLECTANCE; VEGETATION; PLANTS; TRANSMITTANCE; NITROGEN; SPECTRA; INDEXES AB Low-altitude Airborne Visible/Infirared Imaging Spectrometer (AVIRIS) hyperspectral imagery of a cornfield in Nebraska was used to determine whether derivative analysis methods provided enhanced plant stress detection compared with narrow-band ratios. The field was divided into 20 plots representing four replicates each of five nitrogen (N) fertilization treatments that ranged from 0 to 200 kg Who in 50 kg/ha increments. The imagery yielded a 3 m ground pixel size for 224 spectral bands. Derivative analysis provided no advantage in stress detection compared with the performance of narrow-band ratio indices derived from the literature. This result was attributed to a high leaf area index at the time of the overflight (LAI of approximately 5 to 6) and the high signal-to-noise character of the narrow AVIRIS bands. C1 Lockheed Martin Space Operat Sci Syst & Applicat, Stennis Space Ctr, MS 39529 USA. Univ So Mississippi, Gulf Coast Geospatial Ctr, NASA, Earth Sci Applicat Directorate, Ocean Springs, MS 39564 USA. RP Estep, L (reprint author), Lockheed Martin Space Operat Sci Syst & Applicat, Bldg 1105, Stennis Space Ctr, MS 39529 USA. EM lestep@cox.net; Greg.Carter@usm.edu NR 26 TC 19 Z9 19 U1 0 U2 4 PU AMER SOC PHOTOGRAMMETRY PI BETHESDA PA 5410 GROSVENOR LANE SUITE 210, BETHESDA, MD 20814-2160 USA SN 0099-1112 J9 PHOTOGRAMM ENG REM S JI Photogramm. Eng. Remote Sens. PD DEC PY 2005 VL 71 IS 12 BP 1417 EP 1421 PG 5 WC Geography, Physical; Geosciences, Multidisciplinary; Remote Sensing; Imaging Science & Photographic Technology SC Physical Geography; Geology; Remote Sensing; Imaging Science & Photographic Technology GA 994TU UT WOS:000234054900008 ER PT J AU Smith, SJ Chutjian, A Lozano, JA AF Smith, SJ Chutjian, A Lozano, JA TI Measurement of metastable lifetimes for transitions in Fe9+, Fe10+, and Fe13+ SO PHYSICAL REVIEW A LA English DT Article ID SPECTRAL-LINE INTENSITIES; STELLAR CORONAL ABUNDANCES; GROUND-STATE CONFIGURATION; AL-LIKE IONS; FORBIDDEN LINES; ATOMIC DATA; ENERGY-LEVELS; LEVEL LIFETIMES; NPQ IONS; PROBABILITIES AB Radiative lifetimes are measured for metastable levels in the iron charge states Fe9+, Fe10+, and Fe13+. The ions are generated in a 14 GHz electron cyclotron resonance ion source and trapped in a Kingdon ion trap. The Fe levels and their measured lifetimes are (a) 73.0 +/- 0.8 ms for the 3s(2)3p(4)(P-3)3d F-4(7/2) level in Fe9+, (b) 9.91 +/- 0.5 ms for the 3s(2)3p(4) D-1(2) level in Fe10+, and (c) 17.0 +/- 0.2 ms for the 3s(2)3p P-2(3/2)o level in Fe13+. Comparisons are made to other measured results using a Kingdon trap, an ion storage, and an electron-beam ion trap (EBIT). C1 CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA. RP CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA. NR 48 TC 22 Z9 22 U1 0 U2 5 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2469-9926 EI 2469-9934 J9 PHYS REV A JI Phys. Rev. A PD DEC PY 2005 VL 72 IS 6 AR 062504 DI 10.1103/PhysRevA.72.062504 PG 6 WC Optics; Physics, Atomic, Molecular & Chemical SC Optics; Physics GA 998QU UT WOS:000234334900062 ER PT J AU Abbott, B Abbott, R Adhikari, R Ageev, A Agresti, J Ajith, P Allen, B Allen, J Amin, R Anderson, SB Anderson, WG Araya, M Armandula, H Ashley, M Asiri, F Aufmuth, P Aulbert, C Babak, S Balasubramanian, R Ballmer, S Barish, BC Barker, C Barker, D Barnes, M Barr, B Barton, MA Bayer, K Beausoleil, R Belczynski, K Bennett, R Berukoff, SJ Betzwieser, J Bhawal, B Bilenko, IA Billingsley, G Black, E Blackburn, K Blackburn, L Bland, B Bochner, B Bogue, L Bork, R Bose, S Brady, PR Braginsky, VB Brau, JE Brown, DA Bullington, A Bunkowski, A Buonanno, A Burgess, R Busby, D Butler, WE Byer, RL Cadonati, L Cagnoli, G Camp, JB Cannizzo, J Cannon, K Cantley, CA Cao, J Cardenas, L Carter, K Casey, MM Castiglione, J Chandler, A Chapsky, J Charlton, P Chatterji, S Chelkowski, S Chen, Y Chickarmane, V Chin, D Christensen, N Churches, D Cokelaer, T Colacino, C Coldwell, R Coles, M Cook, D Corbitt, T Coyne, D Creighton, JDE Creighton, TD Crooks, DRM Csatorday, P Cusack, BJ Cutler, C Dalrymple, J D'Ambrosio, E Danzmann, K Davies, G Daw, E DeBra, D Delker, T Dergachev, V Desai, S DeSalvo, R Dhurandhar, S Di Credico, A Diaz, M Ding, H Drever, RWP Dupuis, RJ Edlund, JA Ehrens, P Elliffe, EJ Etzel, T Evans, M Evans, T Fairhurst, S Fallnich, C Farnham, D Fejer, MM Findley, T Fine, M Finn, LS Franzen, KY Freise, A Frey, R Fritschel, P Frolov, VV Fyffe, M Ganezer, KS Garofoli, J Giaime, JA Gillespie, A Goda, K Goggin, L Gonzalez, G Gossler, S Grandclement, P Grant, A Gray, C Gretarsson, AM Grimmett, D Grote, H Grunewald, S Guenther, M Gustafson, E Gustafson, R Hamilton, WO Hammond, M Hanna, C Hanson, J Hardham, C Harms, J Harry, G Hartunian, A Heefner, J Hefetz, Y Heinzel, G Heng, IS Hennessy, M Hepler, N Heptonstall, A Heurs, M Hewitson, M Hild, S Hindman, N Hoang, P Hough, J Hrynevych, M Hua, W Ito, M Itoh, Y Ivanov, A Jennrich, O Johnson, B Johnson, WW Johnston, WR Jones, DI Jones, G Jones, L Jungwirth, D Kalogera, V Katsavounidis, E Kawabe, K Kells, W Kern, J Khan, A Killbourn, S Killow, CJ Kim, C King, C King, P Klimenko, S Koranda, S Kotter, K Kovalik, J Kozak, D Krishnan, B Landry, M Langdale, J Lantz, B Lawrence, R Lazzarini, A Lei, M Leonor, I Libbrecht, K Libson, A Lindquist, P Liu, S Logan, J Lormand, M Lubinski, M Luck, H Luna, M Lyons, TT Machenschalk, B MacInnis, M Mageswaran, M Mailand, K Majid, W Malec, M Mandic, V Mann, F Marin, A Marka, S Maros, E Mason, J Mason, K Matherny, O Matone, L Mavalvala, N McCarthy, R McClelland, DE McHugh, M McNabb, JWC Melissinos, A Mendell, G Mercer, RA Meshkov, S Messaritaki, E Messenger, C Mikhailov, E Mitra, S Mitrofanov, VP Mitselmakher, G Mittleman, R Miyakawa, O Mohanty, S Moreno, G Mossavi, K Mueller, G Mukherjee, S Murray, P Myers, E Myers, J Nagano, S Nash, T Nayak, R Newton, G Nocera, F Noel, JS Nutzman, P Olson, T O'Reilly, B Ottaway, DJ Ottewill, A Ouimette, D Overmier, H Owen, BJ Pan, Y Papa, MA Parameshwaraiah, V Parameswariah, C Pedraza, M Penn, S Pitkin, M Plissi, M Prix, R Quetschke, V Raab, F Radkins, H Rahkola, R Rakhmanov, M Rao, SR Rawlins, K Ray-Majumder, S Re, V Redding, D Regehr, MW Regimbau, T Reid, S Reilly, KT Reithmaier, K Reitze, DH Richman, S Riesen, R Riles, K Rivera, B Rizzi, A Robertson, DI Robertson, NA Robinson, C Robison, L Roddy, S Rodriguez, A Rollins, J Romano, JD Romie, J Rong, H Rose, D Rotthoff, E Rowan, S Rudiger, A Ruet, L Russell, P Ryan, K Salzman, I Sandberg, V Sanders, GH Sannibale, V Sarin, P Sathyaprakash, B Saulson, PR Savage, R Sazonov, A Schilling, R Schlaufman, K Schmidt, V Schnabel, R Schofield, R Schutz, BF Schwinberg, P Scott, SM Seader, SE Searle, AC Sears, B Seel, S Seifert, F Sellers, D Sengupta, AS Shapiro, CA Shawhan, P Shoemaker, DH Shu, QZ Sibley, A Siemens, X Sievers, L Sigg, D Sintes, AM Smith, JR Smith, M Smith, MR Sneddon, PH Spero, R Spjeld, O Stapfer, G Steussy, D Strain, KA Strom, D Stuver, A Summerscales, T Sumner, MC Sung, M Sutton, PJ Sylvestre, J Tanner, DB Tariq, H Tarallo, M Taylor, I Taylor, R Taylor, R Thorne, KA Thorne, KS Tibbits, M Tilav, S Tinto, M Tokmakov, KV Torres, C Torrie, C Traylor, G Tyler, W Ugolini, D Ungarelli, C Vallisneri, M van Putten, M Vass, S Vecchio, A Veitch, J Vorvick, C Vyachanin, SP Wallace, L Walther, H Ward, H Ward, R Ware, B Watts, K Webber, D Weidner, A Weiland, U Weinstein, A Weiss, R Welling, H Wen, L Wen, S Wette, K Whelan, JT Whitcomb, SE Whiting, BF Wiley, S Wilkinson, C Willems, PA Williams, PR Williams, R Willke, B Wilson, A Winjum, BJ Winkler, W Wise, S Wiseman, AG Woan, G Woods, D Wooley, R Worden, J Wu, W Yakushin, I Yamamoto, H Yoshida, S Zaleski, KD Zanolin, M Zawischa, I Zhang, L Zhu, R Zotov, N Zucker, M Zweizig, J Akutsu, T Akutsu, T Ando, M Arai, K Araya, A Asada, H Aso, Y Beyersdorf, P Fujiki, Y Fujimoto, MK Fujita, R Fukushima, M Futamase, T Hamuro, Y Haruyama, T Hayama, K Iguchi, H Iida, Y Ioka, K Ishizuka, H Kamikubota, N Kanda, N Kaneyama, T Karasawa, Y Kasahara, K Kasai, T Katsuki, M Kawamura, S Kawamura, M Kawazoe, F Kojima, Y Kokeyama, K Kondo, K Kozai, Y Kudoh, H Kuroda, K Kuwabara, T Matsuda, N Mio, N Miura, K Miyama, S Miyoki, S Mizusawa, H Moriwaki, S Musha, M Nagayama, Y Nakagawa, K Nakamura, T Nakano, H Nakao, K Nishi, Y Numata, K Ogawa, Y Ohashi, M Ohishi, N Okutomi, A Oohara, K Otsuka, S Saito, Y Sakata, S Sasaki, M Sato, N Sato, S Sato, Y Sato, K Sekido, A Seto, N Shibata, M Shinkai, H Shintomi, T Soida, K Somiya, K Suzuki, T Tagoshi, H Takahashi, H Takahashi, R Takamori, A Takemoto, S Takeno, K Tanaka, T Taniguchi, K Tanji, T Tatsumi, D Telada, S Tokunari, M Tomaru, T Tsubono, K Tsuda, N Tsunesada, Y Uchiyama, T Ueda, K Ueda, A Waseda, K Yamamoto, A Yamamoto, K Yamazaki, T Yanagi, Y Yokoyama, J Yoshida, T Zhu, ZH AF Abbott, B Abbott, R Adhikari, R Ageev, A Agresti, J Ajith, P Allen, B Allen, J Amin, R Anderson, SB Anderson, WG Araya, M Armandula, H Ashley, M Asiri, F Aufmuth, P Aulbert, C Babak, S Balasubramanian, R Ballmer, S Barish, BC Barker, C Barker, D Barnes, M Barr, B Barton, MA Bayer, K Beausoleil, R Belczynski, K Bennett, R Berukoff, SJ Betzwieser, J Bhawal, B Bilenko, IA Billingsley, G Black, E Blackburn, K Blackburn, L Bland, B Bochner, B Bogue, L Bork, R Bose, S Brady, PR Braginsky, VB Brau, JE Brown, DA Bullington, A Bunkowski, A Buonanno, A Burgess, R Busby, D Butler, WE Byer, RL Cadonati, L Cagnoli, G Camp, JB Cannizzo, J Cannon, K Cantley, CA Cao, J Cardenas, L Carter, K Casey, MM Castiglione, J Chandler, A Chapsky, J Charlton, P Chatterji, S Chelkowski, S Chen, Y Chickarmane, V Chin, D Christensen, N Churches, D Cokelaer, T Colacino, C Coldwell, R Coles, M Cook, D Corbitt, T Coyne, D Creighton, JDE Creighton, TD Crooks, DRM Csatorday, P Cusack, BJ Cutler, C Dalrymple, J D'Ambrosio, E Danzmann, K Davies, G Daw, E DeBra, D Delker, T Dergachev, V Desai, S DeSalvo, R Dhurandhar, S Di Credico, A Diaz, M Ding, H Drever, RWP Dupuis, RJ Edlund, JA Ehrens, P Elliffe, EJ Etzel, T Evans, M Evans, T Fairhurst, S Fallnich, C Farnham, D Fejer, MM Findley, T Fine, M Finn, LS Franzen, KY Freise, A Frey, R Fritschel, P Frolov, VV Fyffe, M Ganezer, KS Garofoli, J Giaime, JA Gillespie, A Goda, K Goggin, L Gonzalez, G Gossler, S Grandclement, P Grant, A Gray, C Gretarsson, AM Grimmett, D Grote, H Grunewald, S Guenther, M Gustafson, E Gustafson, R Hamilton, WO Hammond, M Hanna, C Hanson, J Hardham, C Harms, J Harry, G Hartunian, A Heefner, J Hefetz, Y Heinzel, G Heng, IS Hennessy, M Hepler, N Heptonstall, A Heurs, M Hewitson, M Hild, S Hindman, N Hoang, P Hough, J Hrynevych, M Hua, W Ito, M Itoh, Y Ivanov, A Jennrich, O Johnson, B Johnson, WW Johnston, WR Jones, DI Jones, G Jones, L Jungwirth, D Kalogera, V Katsavounidis, E Kawabe, K Kells, W Kern, J Khan, A Killbourn, S Killow, CJ Kim, C King, C King, P Klimenko, S Koranda, S Kotter, K Kovalik, J Kozak, D Krishnan, B Landry, M Langdale, J Lantz, B Lawrence, R Lazzarini, A Lei, M Leonor, I Libbrecht, K Libson, A Lindquist, P Liu, S Logan, J Lormand, M Lubinski, M Luck, H Luna, M Lyons, TT Machenschalk, B MacInnis, M Mageswaran, M Mailand, K Majid, W Malec, M Mandic, V Mann, F Marin, A Marka, S Maros, E Mason, J Mason, K Matherny, O Matone, L Mavalvala, N McCarthy, R McClelland, DE McHugh, M McNabb, JWC Melissinos, A Mendell, G Mercer, RA Meshkov, S Messaritaki, E Messenger, C Mikhailov, E Mitra, S Mitrofanov, VP Mitselmakher, G Mittleman, R Miyakawa, O Mohanty, S Moreno, G Mossavi, K Mueller, G Mukherjee, S Murray, P Myers, E Myers, J Nagano, S Nash, T Nayak, R Newton, G Nocera, F Noel, JS Nutzman, P Olson, T O'Reilly, B Ottaway, DJ Ottewill, A Ouimette, D Overmier, H Owen, BJ Pan, Y Papa, MA Parameshwaraiah, V Parameswariah, C Pedraza, M Penn, S Pitkin, M Plissi, M Prix, R Quetschke, V Raab, F Radkins, H Rahkola, R Rakhmanov, M Rao, SR Rawlins, K Ray-Majumder, S Re, V Redding, D Regehr, MW Regimbau, T Reid, S Reilly, KT Reithmaier, K Reitze, DH Richman, S Riesen, R Riles, K Rivera, B Rizzi, A Robertson, DI Robertson, NA Robinson, C Robison, L Roddy, S Rodriguez, A Rollins, J Romano, JD Romie, J Rong, H Rose, D Rotthoff, E Rowan, S Rudiger, A Ruet, L Russell, P Ryan, K Salzman, I Sandberg, V Sanders, GH Sannibale, V Sarin, P Sathyaprakash, B Saulson, PR Savage, R Sazonov, A Schilling, R Schlaufman, K Schmidt, V Schnabel, R Schofield, R Schutz, BF Schwinberg, P Scott, SM Seader, SE Searle, AC Sears, B Seel, S Seifert, F Sellers, D Sengupta, AS Shapiro, CA Shawhan, P Shoemaker, DH Shu, QZ Sibley, A Siemens, X Sievers, L Sigg, D Sintes, AM Smith, JR Smith, M Smith, MR Sneddon, PH Spero, R Spjeld, O Stapfer, G Steussy, D Strain, KA Strom, D Stuver, A Summerscales, T Sumner, MC Sung, M Sutton, PJ Sylvestre, J Tanner, DB Tariq, H Tarallo, M Taylor, I Taylor, R Taylor, R Thorne, KA Thorne, KS Tibbits, M Tilav, S Tinto, M Tokmakov, KV Torres, C Torrie, C Traylor, G Tyler, W Ugolini, D Ungarelli, C Vallisneri, M van Putten, M Vass, S Vecchio, A Veitch, J Vorvick, C Vyachanin, SP Wallace, L Walther, H Ward, H Ward, R Ware, B Watts, K Webber, D Weidner, A Weiland, U Weinstein, A Weiss, R Welling, H Wen, L Wen, S Wette, K Whelan, JT Whitcomb, SE Whiting, BF Wiley, S Wilkinson, C Willems, PA Williams, PR Williams, R Willke, B Wilson, A Winjum, BJ Winkler, W Wise, S Wiseman, AG Woan, G Woods, D Wooley, R Worden, J Wu, W Yakushin, I Yamamoto, H Yoshida, S Zaleski, KD Zanolin, M Zawischa, I Zhang, L Zhu, R Zotov, N Zucker, M Zweizig, J Akutsu, T Akutsu, T Ando, M Arai, K Araya, A Asada, H Aso, Y Beyersdorf, P Fujiki, Y Fujimoto, MK Fujita, R Fukushima, M Futamase, T Hamuro, Y Haruyama, T Hayama, K Iguchi, H Iida, Y Ioka, K Ishizuka, H Kamikubota, N Kanda, N Kaneyama, T Karasawa, Y Kasahara, K Kasai, T Katsuki, M Kawamura, S Kawamura, M Kawazoe, F Kojima, Y Kokeyama, K Kondo, K Kozai, Y Kudoh, H Kuroda, K Kuwabara, T Matsuda, N Mio, N Miura, K Miyama, S Miyoki, S Mizusawa, H Moriwaki, S Musha, M Nagayama, Y Nakagawa, K Nakamura, T Nakano, H Nakao, K Nishi, Y Numata, K Ogawa, Y Ohashi, M Ohishi, N Okutomi, A Oohara, K Otsuka, S Saito, Y Sakata, S Sasaki, M Sato, N Sato, S Sato, Y Sato, K Sekido, A Seto, N Shibata, M Shinkai, H Shintomi, T Soida, K Somiya, K Suzuki, T Tagoshi, H Takahashi, H Takahashi, R Takamori, A Takemoto, S Takeno, K Tanaka, T Taniguchi, K Tanji, T Tatsumi, D Telada, S Tokunari, M Tomaru, T Tsubono, K Tsuda, N Tsunesada, Y Uchiyama, T Ueda, K Ueda, A Waseda, K Yamamoto, A Yamamoto, K Yamazaki, T Yanagi, Y Yokoyama, J Yoshida, T Zhu, ZH CA LIGO Sci Collaboration TAMA Collaboration TI Upper limits from the LIGO and TAMA detectors on the rate of gravitational-wave bursts SO PHYSICAL REVIEW D LA English DT Article ID ROTATIONAL CORE COLLAPSE; BLACK-HOLE COALESCENCES; DYNAMICS; NETWORK AB We report on the first joint search for gravitational waves by the TAMA and LIGO collaborations. We looked for millisecond-duration unmodeled gravitational-wave bursts in 473 hr of coincident data collected during early 2003. No candidate signals were found. We set an upper limit of 0.12 events per day on the rate of detectable gravitational-wave bursts, at 90% confidence level. From software simulations, we estimate that our detector network was sensitive to bursts with root-sum-square strain amplitude above approximately 1-3x10(-19) Hz(-1/2) in the frequency band 700-2000 Hz. We describe the details of this collaborative search, with particular emphasis on its advantages and disadvantages compared to searches by LIGO and TAMA separately using the same data. Benefits include a lower background and longer observation time, at some cost in sensitivity and bandwidth. We also demonstrate techniques for performing coincidence searches with a heterogeneous network of detectors with different noise spectra and orientations. These techniques include using coordinated software signal injections to estimate the network sensitivity, and tuning the analysis to maximize the sensitivity and the livetime, subject to constraints on the background. C1 CALTECH, LIGO, Pasadena, CA 91125 USA. Moscow MV Lomonosov State Univ, Moscow 119992, Russia. Syracuse Univ, Syracuse, NY 13244 USA. Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-30167 Hannover, Germany. Univ Wisconsin, Milwaukee, WI 53201 USA. MIT, LIGO, Cambridge, MA 02139 USA. Louisiana State Univ, Baton Rouge, LA 70803 USA. Univ Texas, Brownsville, TX 78520 USA. Texas Southmost Coll, Brownsville, TX 78520 USA. Penn State Univ, University Pk, PA 16802 USA. Leibniz Univ Hannover, D-30167 Hannover, Germany. Max Planck Inst Gravitat Phys, Albert Einstein Inst, D-14476 Golm, Germany. Cardiff Univ, Cardiff CF2 3YB, Wales. Hanford Observ, LIGO, Richland, WA 99352 USA. Univ Glasgow, Glasgow G12 8QQ, Lanark, Scotland. Stanford Univ, Stanford, CA 94305 USA. Northwestern Univ, Evanston, IL 60208 USA. Livingston Observ, LIGO, Livingston, LA 70754 USA. Washington State Univ, Pullman, WA 99164 USA. Univ Oregon, Eugene, OR 97403 USA. Univ Maryland, College Pk, MD 20742 USA. Univ Rochester, Rochester, NY 14627 USA. NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Univ Florida, Gainesville, FL 32611 USA. Univ Michigan, Ann Arbor, MI 48109 USA. Carleton Coll, Northfield, MN 55057 USA. Univ Birmingham, Birmingham B15 2TT, W Midlands, England. Australian Natl Univ, Canberra, ACT 0200, Australia. Inter Univ Ctr Astron & Astrophys, Pune 411007, Maharashtra, India. SE Louisiana Univ, Hammond, LA 70402 USA. Calif State Univ Dominguez Hills, Carson, CA 90747 USA. Embry Riddle Aeronaut Univ, Prescott, AZ 86301 USA. Max Planck Inst Quantum Opt, D-85748 Garching, Germany. Univ Illes Balears, E-07122 Palma de Mallorca, Spain. Columbia Univ, New York, NY 10027 USA. Loyola Univ, New Orleans, LA 70118 USA. Vassar Coll, Poughkeepsie, NY 12604 USA. Salish Kootenai Coll, Pablo, MT 59855 USA. CALTECH, CaRT, Pasadena, CA 91125 USA. Hobart & William Smith Coll, Geneva, NY 14456 USA. Trinity Univ, San Antonio, TX 78212 USA. Louisiana Tech Univ, Ruston, LA 71272 USA. Univ Tokyo, Inst Cosm Ray Res, Kashiwa, Chiba 2778582, Japan. Univ Tokyo, Dept Astron, Bunkyo Ku, Tokyo 1130033, Japan. Univ Tokyo, Dept Phys, Bunkyo Ku, Tokyo 1130033, Japan. Natl Astron Observ, Tokyo 1818588, Japan. Univ Tokyo, Earthquake Res Inst, Bunkyo Ku, Tokyo 1130032, Japan. Hirosaki Univ, Fac Sci & Technol, Hirosaki, Aomori 0368561, Japan. Niigata Univ, Fac Sci, Niigata 9502102, Japan. Osaka Univ, Grad Sch Sci, Toyonaka, Osaka 5600043, Japan. Tohoku Univ, Grad Sch Sci, Sendai, Miyagi 9808578, Japan. High Energy Accelerator Res Org, Tsukuba, Ibaraki 3050801, Japan. Tokyo Inst Technol, Meguro Ku, Tokyo 1528551, Japan. Osaka City Univ, Grad Sch Sci, Sumiyoshi Ku, Osaka 5588585, Japan. Ochanomizu Univ, Bunkyo Ku, Tokyo 1128610, Japan. Hiroshima Univ, Dept Phys, Hiroshima 7398526, Japan. Kyoto Univ, Fac Sci, Sakyo Ku, Kyoto 6068502, Japan. Tokyo Denki Univ, Chiyoda Ku, Tokyo 1018457, Japan. Univ Tokyo, Dept Adv Mat Sci, Kashiwa, Chiba 2778561, Japan. Miyagi Univ Educ, Dept Phys, Sendai, Miyagi 9800845, Japan. Univ Electrocommun, Inst Laser Sci, Chofu, Tokyo 1828585, Japan. Tokai Univ, Fac Engn, Div Precis Engn, Hiratsuka, Kanagawa 2591292, Japan. Waseda Univ, Shinjyuku Ku, Tokyo 1698555, Japan. Univ Tokyo, Grad Sch Arts & Sci, Meguro Ku, Tokyo 1538902, Japan. RIKEN, Wako, Saitama 3510198, Japan. Kyoto Univ, Yukawa Inst Theoret Phys, Sakyo Ku, Kyoto 6068502, Japan. Univ Tokyo, Grad Sch Sci, Res Ctr Early Universe, Tokyo 1130033, Japan. Natl Inst Adv Ind Sci & Technol, Tsukuba, Ibaraki 3058563, Japan. Univ Illinois, Dept Phys, Urbana, IL 61801 USA. RP CALTECH, LIGO, Pasadena, CA 91125 USA. RI van Putten, Maurice/F-5237-2011; ANDO, MASAKI/G-4989-2014; MIYAMA, Shoken/A-3598-2015; Vecchio, Alberto/F-8310-2015; Ottaway, David/J-5908-2015; Ottewill, Adrian/A-1838-2016; Messaritaki, Eirini/D-7393-2016; Tarallo, Marco/B-2096-2012; Sigg, Daniel/I-4308-2015; Harms, Jan/J-4359-2012; Frey, Raymond/E-2830-2016; Ward, Robert/I-8032-2014; Freise, Andreas/F-8892-2011; Kawabe, Keita/G-9840-2011; Finn, Lee Samuel/A-3452-2009; Agresti, Juri/G-8168-2012; Taniguchi, Keisuke/G-2694-2011; Mitrofanov, Valery/D-8501-2012; Bilenko, Igor/D-5172-2012; Allen, Bruce/K-2327-2012; Chen, Yanbei/A-2604-2013; Barker, David/A-5671-2013; Pitkin, Matthew/I-3802-2013; Liu, Sheng/K-2815-2013; Vyatchanin, Sergey/J-2238-2012; Lueck, Harald/F-7100-2011; Sylvestre, Julien/A-8610-2009; Beausoleil, Raymond/C-5076-2009; Kawazoe, Fumiko/F-7700-2011; McClelland, David/E-6765-2010; Hild, Stefan/A-3864-2010; Schutz, Bernard/B-1504-2010; Casey, Morag/C-9703-2010; Rowan, Sheila/E-3032-2010; Strain, Kenneth/D-5236-2011; Raab, Frederick/E-2222-2011; OI Stuver, Amber/0000-0003-0324-5735; Zweizig, John/0000-0002-1521-3397; Fairhurst, Stephen/0000-0001-8480-1961; ANDO, MASAKI/0000-0002-8865-9998; Vecchio, Alberto/0000-0002-6254-1617; Ottewill, Adrian/0000-0003-3293-8450; Tarallo, Marco/0000-0001-5169-4987; Sigg, Daniel/0000-0003-4606-6526; Frey, Raymond/0000-0003-0341-2636; Ward, Robert/0000-0001-5503-5241; Whelan, John/0000-0001-5710-6576; Finn, Lee Samuel/0000-0002-3937-0688; Agresti, Juri/0000-0001-6119-2470; Allen, Bruce/0000-0003-4285-6256; Pitkin, Matthew/0000-0003-4548-526X; Lueck, Harald/0000-0001-9350-4846; Sylvestre, Julien/0000-0001-8136-4348; McClelland, David/0000-0001-6210-5842; Strain, Kenneth/0000-0002-2066-5355; Taylor, Ian/0000-0001-5040-0772; Aulbert, Carsten/0000-0002-1481-8319; Freise, Andreas/0000-0001-6586-9901; Whiting, Bernard F/0000-0002-8501-8669; Veitch, John/0000-0002-6508-0713; Nakano, Hiroyuki/0000-0001-7665-0796; Papa, M.Alessandra/0000-0002-1007-5298 NR 30 TC 40 Z9 40 U1 2 U2 16 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD DEC PY 2005 VL 72 IS 12 AR 122004 DI 10.1103/PhysRevD.72.122004 PG 16 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 997US UT WOS:000234274900008 ER PT J AU Buchman, LT Bardeen, JM AF Buchman, LT Bardeen, JM TI Schwarzschild tests of the Wahlquist-Estabrook-Buchman-Bardeen tetrad formulation for numerical relativity SO PHYSICAL REVIEW D LA English DT Article ID SPECIAL ORTHONORMAL FRAMES; BOUNDARY VALUE-PROBLEM; GENERAL-RELATIVITY; HYPERBOLIC FORMULATIONS; ASHTEKAR FORMULATION; EINSTEIN EQUATIONS; VARIABLES; GRAVITY; SYSTEMS AB A first order symmetric hyperbolic tetrad formulation of the Einstein equations developed by Estabrook and Wahlquist and put into a form suitable for numerical relativity by Buchman and Bardeen (the WEBB formulation) is adapted to explicit spherical symmetry and tested for accuracy and stability in the evolution of spherically symmetric black holes (the Schwarzschild geometry). The lapse and shift, which specify the evolution of the coordinates relative to the tetrad congruence, are reset at frequent time intervals to keep the constant-time hypersurfaces nearly orthogonal to the tetrad congruence and the spatial coordinate satisfying a kind of minimal rate of strain condition. By arranging through initial conditions that the constant-time hypersurfaces are asymptotically hyperbolic, we simplify the boundary value problem and improve stability of the evolution. Results are obtained for both tetrad gauges ("Nester" and "Lorentz") of the WEBB formalism using finite difference numerical methods. We are able to obtain stable unconstrained evolution with the Nester gauge for certain initial conditions, but not with the Lorentz gauge. C1 CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. Univ Washington, Dept Phys, Seattle, WA 98195 USA. RP Buchman, LT (reprint author), CALTECH, Jet Prop Lab, Pasadena, CA 91125 USA. NR 47 TC 8 Z9 8 U1 0 U2 1 PU AMERICAN PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 1550-7998 J9 PHYS REV D JI Phys. Rev. D PD DEC PY 2005 VL 72 IS 12 AR 124014 DI 10.1103/PhysRevD.72.124014 PG 14 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 997US UT WOS:000234274900051 ER PT J AU Sturrock, PA Caldwell, DO Scargle, JD Wheatland, MS AF Sturrock, PA Caldwell, DO Scargle, JD Wheatland, MS TI Power-spectrum analyses of Super-Kamiokande solar neutrino data: Variability and its implications for solar physics and neutrino physics SO PHYSICAL REVIEW D LA English DT Article ID TIME-SERIES ANALYSIS; UNEVENLY SPACED DATA; RESONANT AMPLIFICATION; ROTATING STARS; OSCILLATIONS; FLUX; MATTER; PERIODICITY; SPECTROSCOPY; ENHANCEMENT AB Since rotational or similar modulation of the solar neutrino flux would seem to be incompatible with the currently accepted theoretical interpretation of the solar neutrino deficit, it is important to determine whether or not such modulation occurs. There have been conflicting claims as to whether or not power-spectrum analysis of the Super-Kamiokande solar neutrino data yields indication of variability. Comparison of these claims is complicated by the fact that the relevant articles may use different data sets, different methods of analysis, and different procedures for significance estimation. The purpose of this article is to clarify the role of power-spectrum analysis. To this end, we analyze primarily the Super-Kamiokande 5-day data set, and we use a standard procedure for significance estimation as used by the Super-Kamiokande collaboration. We then analyze this data set, with this method of significance estimation, using six methods of power-spectrum analysis. Five of these have been used in published articles, and the other is a method that might have been used. We find that, with one exception, the results of these calculations are consistent with those of previously published analyses. We find that the power of the principal modulation (that at 9.43 yr(-1)) is greater in analyses that take account of error estimates than in the basic Lomb-Scargle analysis that does not take account of error estimates. The corresponding significance level ranges between 98% and 99.3%, depending on the details of the analysis. Concerning the recent article by Koshio, we find that we can reproduce the results of his power-spectrum analysis but not the results of his Monte Carlo simulations, and we have a suggestion that may account for the difference. We also comment on a recent article by Yoo et al. We discuss, in terms of subdominant processes, possible neutrino-physics interpretations of the apparent variability of the Super-Kamiokande measurements, and we suggest steps that could be taken to resolve the question of variability of the solar neutrino flux. C1 Stanford Univ, Ctr Space Sci & Astrophys, Stanford, CA 94305 USA. Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA. NASA, Ames Res Ctr, Moffett Field, CA 94035 USA. Univ Sydney, Sch Phys, Sydney, NSW 2006, Australia. RP Stanford Univ, Ctr Space Sci & Astrophys, Varian 302, Stanford, CA 94305 USA. RI Wheatland, Michael/G-1958-2016 OI Wheatland, Michael/0000-0001-5100-2354 NR 42 TC 30 Z9 30 U1 0 U2 0 PU AMER PHYSICAL SOC PI COLLEGE PK PA ONE PHYSICS ELLIPSE, COLLEGE PK, MD 20740-3844 USA SN 2470-0010 EI 2470-0029 J9 PHYS REV D JI Phys. Rev. D PD DEC PY 2005 VL 72 IS 11 AR 113004 DI 10.1103/PhysRevD.72.113004 PG 14 WC Astronomy & Astrophysics; Physics, Particles & Fields SC Astronomy & Astrophysics; Physics GA 997UN UT WOS:000234274400007 ER PT J AU Vilas, F Cobian, PS Barlow, NG Lederer, SM AF Vilas, F Cobian, PS Barlow, NG Lederer, SM TI How much material do the radar-bright craters at the Mercurian poles contain? SO PLANETARY AND SPACE SCIENCE LA English DT Article DE mercury; cratering; surfaces; planets; radar; terrestrial planets; ices ID POLAR ANOMALIES; ICE DEPOSITS; GROUND ICE; STABILITY; WATER AB The depth-to-diameter (d/D) ratios were determined for 12 craters located near the Mercurian north pole that were identified by Harmon et al. (2001, Icarus 149) as having strong depolarized radar echos. We find that the mean d/D value of these radar-bright craters is 2 the mean d/D value of the general population of non-radar-bright craters in the surrounding north polar region. Previous studies, however, show no difference between d/D values of Mercurian polar and equatorial crater populations, suggesting that no terrain softening which could modify crater structure exists at the Mercurian poles (Barlow et al., 1999, 194, Icarus 141). Thus, the change in d/D is governed by a change in crater depth, probably due to deposition of material inside the crater. The volume of infilling material, including volatiles, in the radar-bright craters is significantly greater than predicted by proposed mechanisms for the emplacement of either water ice or sulfur. (c) 2005 Elsevier Ltd. All rights reserved. C1 NASA, Lyndon B Johnson Space Ctr, Planetary Astron Grp, KR, Houston, TX 77058 USA. Calif State Univ San Bernardino, Dept Phys, San Bernardino, CA 92407 USA. No Arizona Univ, Dept Phys & Astron, Flagstaff, AZ 86011 USA. RP Vilas, F (reprint author), Univ Arizona, Multiple Mirror Telescope Observ, POB 210065, Tucson, AZ 85721 USA. EM Faith.Vilas-1@nasa.gov NR 13 TC 8 Z9 8 U1 0 U2 0 PU PERGAMON-ELSEVIER SCIENCE LTD PI OXFORD PA THE BOULEVARD, LANGFORD LANE, KIDLINGTON, OXFORD OX5 1GB, ENGLAND SN 0032-0633 J9 PLANET SPACE SCI JI Planet Space Sci. PD DEC PY 2005 VL 53 IS 14-15 BP 1496 EP 1500 DI 10.1016/j.pss.2005.07.003 PG 5 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 000CY UT WOS:000234439700009 ER PT J AU Davis, RN Polites, ME Trevino, LC AF Davis, RN Polites, ME Trevino, LC TI Autonomous component health management with failed component detection, identification, and avoidance SO PROCEEDINGS OF THE INSTITUTION OF MECHANICAL ENGINEERS PART G-JOURNAL OF AEROSPACE ENGINEERING LA English DT Article DE autonomous component health management (ACHM); failure detection and isolation; failure detection and reconfiguration; integrated vehicle health monitoring (IVHM) ID SYSTEMS AB This article describes a novel scheme for autonomous component health management (ACHM) with failed actuator detection and identification and failed sensor detection, identification, and avoidance. This new scheme has features that are very superior to those with triple redundant sensing and voting, yet requires fewer sensors; it can be applied to any system with redundant sensing. Relevant background to the ACHM scheme is provided in this article. Simulation results for its application to a single-axis spacecraft attitude control system with a third-order plant and dual-redundant measurements of the system states are presented. The ACHM scheme fulfills key functions needed by an integrated vehicle health monitoring (IVHM) system. It is autonomous; is adaptive; works in real time; provides optimal state estimation; identifies failed components; avoids failed components; reconfigures for multiple failures, reconfigures for intermittent failures; works for hard-over, soft, and zero-output failures; and works for both open- and closed-loop systems. The ACHM scheme combines a prefilter that generates preliminary estimates of the system states, detects and identifies failed sensors and actuators, and avoids failed sensors in generating preliminary estimates of the system states with a fixed-gain Kalman filter that provides model-based state estimates, which are utilized in the failure detection logic, and generates optimal estimates for the system states. The simulation results show that ACHM can successfully detect, identify, and avoid sensor failures that are single or multiple; persistent and intermittent; and hard-over, soft, and zero-output types. It is now ready to be tested on a computer model of an actual system. C1 Univ Alabama, Dept Aerosp Engn & Mech, Tuscaloosa, AL 35487 USA. Univ Maryland, Dept Aeronaut Engn, College Pk, MD 20742 USA. NASA, George C Marshall Space Flight Ctr, Spacecraft & Vehicle Syst Dept, Adv Sensors & Hlth Management Syst Branch, Huntsville, AL 35812 USA. RP Davis, RN (reprint author), Univ Alabama, Dept Aerosp Engn & Mech, Box 870280, Tuscaloosa, AL 35487 USA. NR 8 TC 4 Z9 4 U1 0 U2 2 PU PROFESSIONAL ENGINEERING PUBLISHING LTD PI WESTMINISTER PA 1 BIRDCAGE WALK, WESTMINISTER SW1H 9JJ, ENGLAND SN 0954-4100 J9 P I MECH ENG G-J AER JI Proc. Inst. Mech. Eng. Part G-J. Aerosp. Eng. PD DEC PY 2005 VL 219 IS G6 BP 483 EP 495 DI 10.1243/095441005X30270 PG 13 WC Engineering, Aerospace; Engineering, Mechanical SC Engineering GA 006QK UT WOS:000234911800002 ER PT J AU Stothers, RB AF Stothers, RB TI Stratospheric transparency derived from total lunar eclipse colors, 1801-1881 SO PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC LA English DT Review ID GREENLAND ICE CORE; EXPLOSIVE VOLCANISM; ILLUMINATION; ERUPTION; PERIOD; RECORD; MOON; LAW AB Contemporary journals have been searched for published accounts of the observed colors of total lunar eclipses in the period 1801 - 1881. The result is a catalog of 31 reported lunar eclipses. A dark eclipse on a clear night usually implies the presence of significant turbidity in the Earth's stratosphere arising from a recent volcanic eruption. The totally eclipsed Moon became invisible ( or nearly so) in the year after the great 1815 eruption of Tambora. Eclipse data compiled here cast doubt on any significant penetration of the stratosphere for a number of other large volcanic eruptions, but are too sparsely distributed in time to say anything conclusive about certain others. C1 NASA, Goddard Inst Space Studies, New York, NY 10025 USA. RP NASA, Goddard Inst Space Studies, 2880 Broadway, New York, NY 10025 USA. EM rstothers@giss.nasa.gov NR 163 TC 3 Z9 3 U1 0 U2 1 PU IOP PUBLISHING LTD PI BRISTOL PA TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND SN 0004-6280 EI 1538-3873 J9 PUBL ASTRON SOC PAC JI Publ. Astron. Soc. Pac. PD DEC PY 2005 VL 117 IS 838 BP 1445 EP 1450 DI 10.1086/497016 PG 6 WC Astronomy & Astrophysics SC Astronomy & Astrophysics GA 993KE UT WOS:000233952200012 ER PT J AU Bradshaw, RC Schmidt, DP Rogers, JR Kelton, KF Hyers, RW AF Bradshaw, RC Schmidt, DP Rogers, JR Kelton, KF Hyers, RW TI Machine vision for high-precision volume measurement applied to levitated containerless material processing SO REVIEW OF SCIENTIFIC INSTRUMENTS LA English DT Article ID THERMAL-EXPANSION; LIQUID-METALS; DENSITY; COPPER AB By combining the best practices in optical dilatometry with numerical methods, a high-speed and high-precision technique has been developed to measure the volume of levitated, containerlessly processed samples with subpixel resolution. Containerless processing provides the ability to study highly reactive materials without the possibility of contamination affecting thermophysical properties. Levitation is a common technique used to isolate a sample as it is being processed. Noncontact optical measurement of thermophysical properties is very important as traditional measuring methods cannot be used. Modern, digitally recorded images require advanced numerical routines to recover the subpixel locations of sample edges and, in turn, produce high-precision measurements. (c) 2005 American Institute of Physics. C1 Univ Massachusetts, Dept Mech & Ind Engn, Amherst, MA 01003 USA. NASA, George C Marshall Space Flight Ctr, Huntsville, AL 35812 USA. Washington Univ, Dept Phys, St Louis, MO 63130 USA. RP Hyers, RW (reprint author), Univ Massachusetts, Dept Mech & Ind Engn, Amherst, MA 01003 USA. EM hyers@ecs.umass.edu RI Hyers, Robert/G-3755-2010 NR 16 TC 30 Z9 30 U1 1 U2 9 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0034-6748 J9 REV SCI INSTRUM JI Rev. Sci. Instrum. PD DEC PY 2005 VL 76 IS 12 AR 125108 DI 10.1063/1.2140490 PG 8 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA 998SU UT WOS:000234340500044 ER PT J AU Singal, J Wollack, E Kogut, A Limon, M Mirel, P Lubin, P Seiffert, M AF Singal, J Wollack, E Kogut, A Limon, M Mirel, P Lubin, P Seiffert, M TI Design and performance of sliced-aperture corrugated feed horn antennas SO REVIEW OF SCIENTIFIC INSTRUMENTS LA English DT Article ID MODE CONVERTERS; RADIATION AB We report on the design of corrugated feed horn microwave antennas at 3.3, 5.6, 7.8, and 10.2 GHz for the absolute radiometer for cosmology, astrophysics, and diffuse emission experiment. These horns have low sidelobe symmetrical beams with 12 degrees full width at half power, and three noteworthy features: a 30 degrees slice at the aperture, a profiled rather than a linear taper, and a slowly varying groove depth along the length of the horn. The profiled taper and varying groove depth provided a narrow beam given the existing physical spatial constraints of the instrument in which the horns are used. The 30 degrees slice was necessary for instrumental considerations and has a minimal effect on the symmetry of the beam. The slice reduces the effective aperture radius and overall length to that corresponding to an unsliced horn with an aperture at roughly the middle of the slice and does not introduce any undesirable effects. (c) 2005 American Institute of Physics. C1 Univ Calif Santa Barbara, Greenbelt, MD 20771 USA. NASA Goddard Space Flight Ctr, Greenbelt, MD 20771 USA. Sci Syst & Applicat Inc, Greenbelt, MD 20771 USA. Jet Propuls Lab, Pasadena, CA 91109 USA. RP Singal, J (reprint author), Univ Calif Santa Barbara, Code 665,Bldg 21, Greenbelt, MD 20771 USA. RI Wollack, Edward/D-4467-2012; OI Wollack, Edward/0000-0002-7567-4451; Limon, Michele/0000-0002-5900-2698 NR 7 TC 6 Z9 6 U1 0 U2 0 PU AMER INST PHYSICS PI MELVILLE PA CIRCULATION & FULFILLMENT DIV, 2 HUNTINGTON QUADRANGLE, STE 1 N O 1, MELVILLE, NY 11747-4501 USA SN 0034-6748 J9 REV SCI INSTRUM JI Rev. Sci. Instrum. PD DEC PY 2005 VL 76 IS 12 AR 124703 DI 10.1063/1.2148990 PG 4 WC Instruments & Instrumentation; Physics, Applied SC Instruments & Instrumentation; Physics GA 998SU UT WOS:000234340500033 ER PT J AU Sullivan, DG Shaw, JN Rickman, D Mask, PL Luvall, JC AF Sullivan, DG Shaw, JN Rickman, D Mask, PL Luvall, JC TI Using remote sensing data to evaluate surface soil properties in Alabama ultisols SO SOIL SCIENCE LA English DT Article ID SPECTRAL REFLECTANCE PROPERTIES; ORGANIC-MATTER; SPECTROSCOPY; MINERALOGY; IRON AB Evaluation of surface soil properties via remote sensing could facilitate soil survey mapping, erosion prediction, and allocation of agrochemicals for precision management. The objective of this study was to evaluate the relationship between soil spectral signature and surface soil properties in conventionally managed row crop systems. High-resolution remote sensing data were acquired over bare fields in the Coastal Plain, Appalachian Plateau, and Ridge and Valley provinces of Alabama using the Airborne Terrestrial Applications Sensor multispectral. scanner. Soils ranged from sandy Kandiudults to fine textured Rhodudults. Surface soil samples (0 to 1 cm) were collected from 161 sampling points for gravimetric soil water content, soil organic carbon, particle size distribution, and citrate dithionite extractable iron content. Surface roughness and crusting were also measured during sampling. Two methods of analysis were evaluated: (1) multiple linear regression using common spectral band ratios and (2) partial least-squares regression. Our data show that thermal infrared spectra are highly, linearly related to soil organic carbon, sand and clay content. Soil organic carbon content was the most difficult to quantify in these highly weathered systems, where soil organic carbon was generally < 1.2%. Estimates of sand and clay content were best using partial least-squares regression at the Valley site, explaining 42 to 59% of the variability. In the Coastal Plain, sandy surfaces prone to crusting limited estimates of sand and clay content via partial least-squares and regression with common band ratios. Estimates of iron oxide content were a function of mineralogy and best accomplished using specific band ratios, with regression explaining 36 to 65% of the variability at the Valley and Coastal Plain sites, respectively. C1 USDA ARS, SE Watershed Res Lab, Tifton, GA 31794 USA. Auburn Univ, Dept Agron & Soils, Auburn, AL 36849 USA. NASA Global Hydrol & Climate Ctr, Huntsville, AL 35805 USA. Auburn Univ, Alabama Cooperat Extens Serv, Auburn, AL 36849 USA. RP Sullivan, DG (reprint author), USDA ARS, SE Watershed Res Lab, POB 946, Tifton, GA 31794 USA. EM dgs@tifton.usda.gov; jnshaw@acesag.auburn.edu OI Rickman, Doug/0000-0003-3409-2882 NR 40 TC 11 Z9 15 U1 2 U2 5 PU LIPPINCOTT WILLIAMS & WILKINS PI PHILADELPHIA PA 530 WALNUT ST, PHILADELPHIA, PA 19106-3261 USA SN 0038-075X J9 SOIL SCI JI Soil Sci. PD DEC PY 2005 VL 170 IS 12 BP 954 EP 968 DI 10.1097/01.ss.0000187350.39611.d7 PG 15 WC Soil Science SC Agriculture GA 998ZZ UT WOS:000234359700002 ER PT J AU Rampino, MR Caldeira, K AF Rampino, MR Caldeira, K TI Major perturbation of ocean chemistry and a 'Strangelove Ocean' after the end-Permian mass extinction SO TERRA NOVA LA English DT Article ID CALCIUM-CARBONATE SATURATION; PEAT-FORMING PLANTS; TRIASSIC BOUNDARY; PHANEROZOIC TIME; BRITISH-COLUMBIA; ATMOSPHERIC CO2; REVISED MODEL; SOUTH-AFRICA; EVENT; BASIN AB The severe mass extinction of marine and terrestrial organisms at the end of the Permian Period (c. 251 Ma) was accompanied by a rapid (< 100 000 years and possibly < 10 000 years) negative excursion of c. 3 parts per thousand in the delta(13)C of the global surface oceans and atmosphere that persisted for some 500 000 years into the Early Triassic. Simulations with an ocean-atmosphere/carbon-cycle model suggest that the isotope excursion can be explained by collapse of ocean primary productivity, and changes in the delivery and cycling of carbon in the oceans and on land. Model results suggest that severe reduction of marine productivity led to an increase in surface-ocean dissolved inorganic carbon and a rapid, short-term increase in atmospheric pCO(2) (from a Late Permian base of 850 ppm to c. 2500 ppm). Increase in surface ocean alkalinity may have stimulated the widespread microbial and abiotic shallow-water carbonate deposition seen in the earliest Triassic. The model is also consistent with a long-term (> 1 Ma) decrease in sedimentary burial of organic carbon in the early Triassic. C1 NYU, Earth & Environm Sci Program, New York, NY 10003 USA. NASA, Goddard Inst Space Studies, New York, NY 10025 USA. Carnegie Inst Washington, Dept Global Ecol, Stanford, CA 94305 USA. RP Rampino, MR (reprint author), NYU, Earth & Environm Sci Program, 100 Washington Sq E,Room 1009, New York, NY 10003 USA. EM mrr1@nyu.edu RI Caldeira, Ken/E-7914-2011 NR 37 TC 48 Z9 51 U1 2 U2 20 PU BLACKWELL PUBLISHING PI OXFORD PA 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND SN 0954-4879 J9 TERRA NOVA JI Terr. Nova PD DEC PY 2005 VL 17 IS 6 BP 554 EP 559 DI 10.1111/j.1365-3121.2005.00648.x PG 6 WC Geosciences, Multidisciplinary SC Geology GA 987LQ UT WOS:000233519800009 ER EF