Scientific and Technical Aerospace Reports Volume 38 July 28, 2000

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20000064708 Jet Propulsion Lab., California Inst. of Tech., Pasadena, CA USA Photochemistry of Saturn’s Atmosphere, 1, Hydrocarbon Chemistry and Comparisons with ISO Observations Moses, Julianne I., Lunar and Planetary Inst., USA; Bezard, Bruno, Observatoire de Paris-Meudon, France; Lellouch, Emmanuel, Observatoire de Paris-Meudon, France; Gladstone, G. Randall, Southwest Research Inst., USA; Feuchtgruber, Helmut, Max- Planck-Inst. fuer Extraterrestrische Physik, Germany; Allen, Mark, Jet Propulsion Lab., California Inst. of Tech., USA; Icarus; 2000; ISSN 0019-1035; Volume I43, pp. 244-298; In English Contract(s)/Grant(s): NASw-4574; NAG5-6915 Report No.(s): LPI-Contrib-982; Copyright; Avail: Issuing Activity To investigate the details of hydrocarbon photochemistry on Saturn, we have developed a one-dimensional diurnally averaged model that couples hydrocarbon and oxygen photochemistry, molecular and eddy diffusion, radiative transfer, and condensation. The model results are compared with observations from the Infrared Space Observatory (ISO) to place tighter constraints on molecular abundances, to better define Saturn’s eddy diffusion coefficient profile, and to identify important chemical schemes that control the abundances of the observable hydrocarbons in Saturn’s upper atmosphere. From the ISO observations, we determine that the column 12 densities of CH3, CH3C2H, and C4H2 above 10 mbar are 4 (sup +2) (sub -1.5) x 10 (exp 13) cm (sup -2), (1.1 plus or minus 0.3) x 10 (exp 15) cm (exp -2), and (1.2 plus or minus 0.3) x 10 (exp 14) cm (sup -2), respectively. The observed ISO emission features also indicate C2H2 mixing ratios of 1.2 (sup +0.9) (sub -0.6) x 10 (exp -6) at 0.3 mbar and (2.7 plus or minus 0.8) x 10 (exp -7) at 1.4 mbar, and a C2H6 mixing ratio of (9 plus or minus 2.5) x 10 (exp -6) at 0.5 mbar. Upper limits are provided for C2H4, CH2CCH2, C3H8, and C6H2 sensitivity of the model results to variations in the eddy diffusion coefficient profile, the solar flux, the CH4 photolysis branching ratios, the atomic hydrogen influx, and key reaction rates are discussed in detail. We find that C4H2 and CH3C2H are particularly good tracers of important chemical processes and physical conditions in Saturn’s upper atmosphere, and C2H6 is a good tracer of the eddy diffusion coefficient in Saturn’s lower stratosphere. The eddy diffusion coefficient must be smaller than approximately 3 x 10 (exp 4) sq cm s (sup -1) at pressures greater than 1 mbar in order to reproduce the C2H6 abundance inferred from ISO observations. The eddy diffusion coefficients in the upper stratosphere could be constrained by observations of CH3 radicals if the low-temperature chemistry of CH3 were better understood. We also discuss the implications of our modeling for aerosol formation in Saturn’s lower stratosphere-diacetylene, butane, and water condense between approximately 1 and 300 mbar in our model and will dominate stratospheric haze formation at nonauroral latitudes. Our photochemical models will be useful for planning observational sequences and for analyzing data from the upcoming Cassini mission. Author Saturn (Planet); Saturn Atmosphere; Photochemical Reactions; Upper Atmosphere; Infrared Astronomy; Mathematical Models 20000064716 NASA Kennedy Space Center, Cocoa Beach, FL USA Titan III Mars Observer Press Showing at the PHSF Aug. 13, 1992; In English; Videotape: 2 min. 30 sec. playing time, in color, no sound Report No.(s): NONP-NASA-VT-2000081554; No Copyright; Avail: CASI; B01, Videotape-Beta; V01, Videotape-VHS Live footage of the Titan 3 Mars Observer is shown at the Payload Hazardous Servicing Facility (PHSF). The Mars Observer is a NASA mission to study the surface, atmosphere, interior and magnetic field of Mars from Martian orbit. CASI Mars Observer; Payloads; Titan 3 Launch Vehicle 20000065630 NASA Kennedy Space Center, Cocoa Beach, FL USA Mars Observer Press Conference Aug. 25, 1993; In English; Videotape: 18 min. 5 sec. playing time, in color, with sound Report No.(s): NONP-NASA-VT-2000081551; No Copyright; Avail: CASI; B02, Videotape-Beta; V02, Videotape-VHS Footage shows Bob MacMillin, NASA’s Public Information Office, as he introduces the Mars Observer Project Manager, Glen Cunningham. Glen is shown addressing the current status of the Mars Observer communication system, the inability of NASA to establish contact, and the action that is currently being taken to establish contact with the spacecraft. Glen is also seen answering questions from both the audience as well as other NASA Centers. CASI Conferences; Mars Observer 230
20000065631 NASA Kennedy Space Center, Cocoa Beach, FL USA TITAN III/Mars Observer Flow Tape for Playback Aug. 11, 1992; In English; Videotape: 10 min. playing time, in color, with sound Report No.(s): NONP-NASA-VT-2000081553; No Copyright; Avail: CASI; B01, Videotape-Beta; V01, Videotape-VHS Footage shows components for the Mars Observer Spacecraft during checkout. Arrival of the navigation system is also shown. CASI Titan 3 Launch Vehicle; Mars Observer 20000065653 National Air and Space Museum, Center for Earth and Planetary Studies, Washington, DC USA Lunar Polar Topography Derived from Clementine Stereoimages Cook, A. C., National Air and Space Museum, USA; Watters, T. R., National Air and Space Museum, USA; Robinson, M. S., Northwestern Univ., USA; Spudis, P. D., Lunar and Planetary Inst., USA; Bussey, D. B. J., European Space Agency. European Space Research and Technology Center, ESTEC, Netherlands; Journal of Geophysical Research; May 25, 2000; ISSN 0148-0227; Volume 105, No. E5, pp. 12,023-12,033; In English Report No.(s): Paper-199JE001083; Copyright; Avail: Issuing Activity Clementine stereoimagery has been used to produce digital elevation models of the Moon, at a scale of about 1 km/pixel. These models cover regions poleward of 60 degree in both hemispheres and reveal topography beyond that covered by the Clementine laser altimeter or Earth-based radar. by combining these polar terrain models with the current Clementine laser altimeter data we have produced a global topographic map of the lunar surface. Several topographic features in the new polar topographic data set are described, including three previously unrecognized pre-Nectarian impact basins. Several known basins have also been mapped, including the southern extent of the South Pole-Aitken basin, and other previously suspected basins have been verified. Author Lunar Surface; Lunar Topography; Relief Maps; Stereophotography; Selenography; Selenology; Moon; Lunar Maps 20000067676 Jet Propulsion Lab., California Inst. of Tech., Pasadena, CA USA Drift Loss-Cone Distributions Electrons in the Jovian Synchrotron Zone from 06 and VIP4 Models Wang, K., Jet Propulsion Lab., California Inst. of Tech., USA; Bolton, S. J., Jet Propulsion Lab., California Inst. of Tech., USA; Gulkis, S., Jet Propulsion Lab., California Inst. of Tech., USA; Levin, S. M., Jet Propulsion Lab., California Inst. of Tech., USA; [2000]; 1p; In English; No Copyright; Avail: Issuing Activity; Abstract Only Relativistic electrons (10-50 MeV) play an important role to account for the observed synchrotron decimetric radiation in Jupiter’s inner radiation belt (L is less than 4). A detailed knowledge of these electron distributions is required to understand the synchrotron emission observations and the associated on-going physical processes. In this paper, instead of assuming electrons drift along constant L-shell at the magnetic equator as many earlier studies adopted, we calculate the size of the theoretical driftloss cone for relativistic electrons using both the O6 and VIP4 magnetic field models. Model maps of the synchrotron emission for specific electron distributions are shown for comparison. Author Relativistic Particles; Electrons; Electron Distribution; High Energy Electrons; Synchrotron Radiation 92 SOLAR PHYSICS �� 20000067637 NASA Marshall Space Flight Center, Huntsville, AL USA The Solar-B Mission Davis, John M., NASA Marshall Space Flight Center, USA; [2000]; 1p; In English; 31st, 19-22 Jun. 2000, Stateline, NV, USA; Sponsored by American Astronomical Society, USA; No Copyright; Avail: Issuing Activity; Abstract Only The Solar-B mission is a joint enterprise between Japan, the United States of America and the UK. The collaboration is led by ISAS, the Japanese Institute for Space and Astronautical Science (ISAS), NASA and PPARC (Particle Physics and Astrophysics Research Council) play supporting roles in the development of the scientific objectives and provision of the scientific instruments. The mission’s primary objective is to conduct a systems study of the solar atmosphere through the acquisition of coordinated measurements of the photosphere, the transition region/low corona and the upper corona using three instruments: an optical telescope, an extreme ultraviolet imaging spectrometer and a soft x-ray telescope. Drs. Saku Tsuneta (NAOJ) and Alan 231
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Scientific and Technical Aerospace
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Introduction Scientific and Technic
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Subject Divisions Table of Contents
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ground equipment and systems. For a
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Subject Categories of the Division
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48 Oceanography 139 Includes the ph
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72 Atomic and Molecular Physics 191
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Document Availability Information T
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Avail: NASA Public Document Rooms.
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NASA CASI Price Tables — Effectiv
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ALABAMA AUBURN UNIV. AT MONTGOMERY
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��
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20000061433 Pisa Univ., Dipartiment
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English; 34th; 34th Thermophysics C
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ciency of the generated derivative
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20000063509 NASA Glenn Research Cen
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05 AIRCRAFT DESIGN, TESTING AND PER
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A long tradition of aerodynamic des
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sonic and transonic cases will be p
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20000061449 British Aerospace Publi
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20000064593 NASA Langley Research C
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performance required for a proposed
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ment cost and create better product
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tion (NPSS), is focused on the inte
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surface measurement techniques used
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with emphasis on the search for lin
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20000063520 NASA Kennedy Space Cent
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primary issues for it’s adaptatio
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Footage shows the night vertical ta
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20000067665 NASA Kennedy Space Cent
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necessary for ignition modeling, or
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engine lifetime, and high power ope
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24 COMPOSITE MATERIALS ��
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ments. For the screening of liner m
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formation of a neutral, fluorescent
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20000065655 Ames Lab., IA USA Funda
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This is a second Triennial Conferen
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of completely charged PSSNa solutio
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20000064100 NASA Langley Research C
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Spacecraft in low Earth orbit (LEO)
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Pressure gradients, i.e. pressure h
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agreed that the NO(sub x) levels co
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tectural approach to extending the
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20000064078 Physics and Electronics
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20000064925 Institute for Human Fac
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20000062455 National Inst. of Stand
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Added Analysis (Risk Reduction); 6)
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shipboard electrical power generati
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20000067664 Jet Propulsion Lab., Ca
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other, The theoretical framework go
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figures compare the lift and pitchi
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ment phase demonstrate desired feat
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esolution mode with resolving power
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to track 1% or 0.5% changes was hig
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20000067643 NASA Marshall Space Fli
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37 MECHANICAL ENGINEERING ��
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solver based on overset grid techno
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20000067659 NASA Marshall Space Fli
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20000064621 Rensselaer Polytechnic
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that for a specific example of a be
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km x 1000 km). As with the nearly c
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20000064527 Analytical Imaging and
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20000064533 Austin State Univ., Dep
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20000064539 California Univ., Inst.
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in Yellowstone National Park. We ar
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terns of community hysteresis based
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tion model (DEM) fitting to the sca
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The Carolina slate belt is a 10- to
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20000063373 Los Alamos National Lab
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20000064912 New Energy and Industri
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and discusses the issues and resear
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The objective of this study was to
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distributions with engine test resu
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7.6, while the 1926 events appear t
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We investigate the compositional di
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Flight Center, USA; Moore, T. E., N
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This report presents the Applied Me
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in Goa, India, by 3 - 4 days. Wind
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51 LIFE SCIENCES (GENERAL) Includes
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20000062717 Joint Inst. for Nuclear
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during 50% (SD 4%) of the breathing
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20000064711 Massachusetts Inst. of
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The analysis of this smaller data s
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vided a functional helmet mount. Th
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61 COMPUTER PROGRAMMING AND SOFTWAR
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The goal of multi-image classificat
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20000063526 Defence Science and Tec
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85 dB amplifier design evolved by o
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20000064594 New Mexico Univ., Elect
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20000064615 NASA Ames Research Cent
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declarations with a pattern recogni
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containing point where interpolatio
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has his own responsibility, while t
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the people, documents and projects
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and experimental technology, many o
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tems. In particular this applicatio
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Page 239 and 240: ecoming almost too cumbersome to be
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Page 257 and 258: A ABERRATION, 143, 198 ABRASION, 22
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Page 267 and 268: SPACE PLATFORMS, 38 SPACE PROBES, 2
Page 269 and 270: WIND PROFILES, 137 WIND TUNNEL TEST
Page 271 and 272: Brown, Andy, 38 Brown, April S., 20
Page 273 and 274: Grosvenor, C. A., 70 Grosvenor, J.
Page 275 and 276: Lu, Gui-Ying, 50 Lugg, Desmond J.,
Page 277 and 278: Robertson, Tony, 39 Robinson, Jeffr
Page 279: Warner, J. D., 63 Warren, James, 16
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