Scientific and Technical Aerospace Reports Volume 38 July 28, 2000

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the abundance pattern of the heavy (Z greater than or = 56) n-capture elements in most giants is well-matched to a scaled Solar System tau-process nucleosynthesis pattern. The onset of the main tau-process can be seen at [Fe/H] approx. = -2.9; this onset is consistent with the suggestion that low mass Type 2 supernovae are responsible for the tau-process. Contributions from the s-process can first be seen in some stars with metallicities as low as [Fe/H] approx. -2.75, and are present in most stars with metallicities [Fe/H] greater than -2.3. The appearance of s-process contributions as metallicity increases presumably reflects the longer stellar evolutionary timescale of the (low-mass) s-process nucleosynthesis sites. The lighter n-capture elements (SR-Y-Zr) are enhanced relative to the heavier tau-process element abundances. Their production cannot be attributed solely to any combination of the Solar System tau- and main s-processes, but requires a mixture of material from the tau-process and from an additional n-capture process which can operate at early Galactic time. This additional process could be the weak s-process in massive (approx.25 Solar Mass) stars, or perhaps a second tau-process site, i.e. different than the site that produces the heavier (Z greater than or = 56) n-capture elements. Author Neutrons; Capture Effect; Galaxies; Heavy Elements; Massive Stars; Metallicity; Nuclear Reactions; Solar System 20000067652 NASA Marshall Space Flight Center, Huntsville, AL USA Laboratory Studies of Optical Characteristics and Condensation Processes of Cosmic Dust Particles Spann, J. F., Jr., NASA Marshall Space Flight Center, USA; Abbas, M. M., NASA Marshall Space Flight Center, USA; Venturini, C. C., Alabama Univ., USA; [2000]; 1p; In English; 8th; Physics of Dusty Plasma, 26-28 Apr. 2000, Santa Fe, NM, USA; No Copyright; Avail: Issuing Activity; Abstract Only Information about the optical characteristics and physical processes involving cosmic dust particles is vital for interpretation of astronomical observations and an understanding of the formation and processing of dust in the evolutionary cycle of matter in the interstellar medium. Cosmic dust particles are formed in a variety of astrophysical environments such as in cool stellar outflows and circumstellar envelopes. Definitive knowledge of the nature, composition, and physical processes of cosmic dust grains, however, can only be inferred from astronomical observations through laboratory experiments on the analogs of hypothesized dust particles and with modeling calculations. Laboratory investigations of the nature, composition, and optical characteristics of cosmic dust particles are being, carried out at many institutions with a variety of experimental techniques. Despite a wealth of available data, however, many basic issues remain unresolved. An experimental facility based on suspension of dust particles in electrodynamic balance in a pressure/temperature controlled environment in a cavity has been operational at the NASA Marshall Space Flight Center, and is currently being employed for studies of dust particle charging mechanisms using electron beams and with UV radiation. In this paper, we discuss two general classes of experiments under planning stages that may be simultaneously carried out on this facility for cosmic dust investigations (i) Infrared optical characteristics (extinction coefficients and scattering phase functions) of the analogs of hypothesized of cosmic dust particles, such as natural and synthetic amorphous silicates with varying compositions, amorphous carbon grains, polycyclic aromatic hydrocarbons (PAHs), and icy core-mantle particles etc. The initial spectral range under consideration is 1-25 micrometers, to be extended to the far infrared region in the future (ii) Condensation of volatile gases on nucleus dust particles to be investigated for planetary and astrophysical environments. Author Condensing; Cosmic Dust; Optical Properties; Astrophysics; Particles 20000067677 California Inst. of Tech., Pasadena, CA USA The ISO View of Star Forming Galaxies Helou, George, California Inst. of Tech., USA; [1999]; 1p; In English; No Copyright; Avail: Issuing Activity; Abstract Only ISO studies of normal galaxies in the local Universe have revealed basic new properties whose significant implications for the star formation process and cosmology are only starting to be understood. This review will touch on the general results of a statistical nature, and provide a quick summary of the profusion of exciting results on individual objects. In the mid-infrared, PHT- S has established that the spectra of star forming galaxies between 6 and-13microns are dominated by the Aromatic Features in Emission (AFE), and show little variation as a function of the heating intensity. The Carriers of the AFE (CAFE) are thus a universal component of dust with standard properties, and contribute between 10 and 25% of the total dust luminosity. In addition to AFE, the spectra show a low-level continuum detectable at wavelengths longer than 3.5microns whose origin is still under investigation. The mid-infrared colors formed as the ratio of flux densities in the 6.75micron and the 15micron bands of ISO-CAM remain essentially constant and near unity for quiescent and mildly active galaxies. As dust heating increases further, the 15micron flux increases steeply compared to 6.75microns, indicating that dust heated to 100K
gas, show variations that have remained controversial in their interpretation. In particular, as the galaxy become more active in star formation, its [CII] flux weakens relative to total dust emission while the [OI] does not. This behavior has attracted much interest because it extrapolates to the most active galaxies, making them weaker in [CII] than previously expected. Several explanations for the effect have been advanced, and will be discussed in this review. Spectroscopy with SWS has measured molecular hydrogen in galaxies, providing a powerful handle on the warm molecular gas content. SWS and CAM-CVF studies targeting ionic fine-structure lines have demonstrated their value as diagnostics of the radiation field. Author Star Formation; Active Galaxies; Radiation Distribution; Cosmology; Fine Structure 91 LUNAR AND PLANETARY SCIENCE AND EXPLORATION �� 20000061490 NASA Kennedy Space Center, Cocoa Beach, FL USA Titan III Mars Observer Arrival and Uncrating at PHSF Jul. 09, 1992; In English; Videotape: 8 min. 25 sec. playing time, in color, with sound Report No.(s): NONP-NASA-VT-2000081540; No Copyright; Avail: CASI; B01, Videotape-Beta; V01, Videotape-VHS Live footage of the uncrating and the arrival of the Titan III Mars Observer to the Payload Hazardous Servicing Facility (PHSF) is presented. The Mars Observer’s mission is to study the surface, atmosphere, interior and magnetic field of Mars from Martian orbit. At the PHSF, fueling of the spacecraft with its orbit insertion and attitude control propellants will occur. This will be followed by mating to the Transfer Orbit Stage (TOS). This is the upper stage that will provide the final thrust to propel the spacecraft on its 11-month journey to Mars. CASI Mars (Planet); Mars Missions; Mars Observer; Payloads; Titan 3 Launch Vehicle 20000061966 Jet Propulsion Lab., California Inst. of Tech., Pasadena, CA USA Report on the Loss of the Mars Polar Lander and Deep Space 2 Missions Albee, Arden, California Inst. of Tech., USA; Battel, Steven, Battel Engineering, USA; Brace, Richard, Jet Propulsion Lab., California Inst. of Tech., USA; Burdick, Garry, Jet Propulsion Lab., California Inst. of Tech., USA; Casani, John, Jet Propulsion Lab., California Inst. of Tech., USA; Lavell, Jeffrey, NASA Langley Research Center, USA; Leising, Charles, Jet Propulsion Lab., California Inst. of Tech., USA; MacPherson, Duncan, Jet Propulsion Lab., California Inst. of Tech., USA; Burr, Peter; Dipprey, Duane; Mar. 22, 2000; 178p; In English; No Copyright; Avail: CASI; A09, Hardcopy; A02, Microfiche NASA’s Mars Surveyor Program (MSP) began in 1994 with plans to send spacecraft to Mars every 26 months. Mars Global Surveyor (MGS), a global mapping mission, was launched in 1996 and is currently orbiting Mars. Mars Surveyor ’98 consisted of Mars Climate Orbiter (MCO) and Mars Polar Lander (MPL). Lockheed Martin Astronautics (LMA) was the prime contractor for Mars Surveyor ’98. The Jet Propulsion Laboratory (JPL), California Institute of Technology, manages the Mars Surveyor Program for NASA’s Office of Space Science. MPL was developed under very tight funding constraints. The combined development cost of MPL and MCO, including the cost of the two launch vehicles, was approximately the same as the development cost of the Mars Pathfinder mission, including the cost of its single launch vehicle. The MPL project accepted the challenge to develop effective implementation methodologies consistent with programmatic requirements. Derived from text Launch Vehicles; Losses; Mars Atmosphere; Space Probes; Mars Polar Lander; Costs 20000062312 Jet Propulsion Lab., California Inst. of Tech., Pasadena, CA USA Rock Abrasion on Mars: Clues from the Pathfinder and Viking Landing Sites Bridges, N. T., Jet Propulsion Lab., California Inst. of Tech., USA; Parker, T. J., Jet Propulsion Lab., California Inst. of Tech., USA; Kramer, G. M., Minnesota Univ., USA; [2000]; 3p; In English; No Copyright; Avail: CASI; A01, Hardcopy; A01, Microfiche A significant discovery of the Mars Pathfinder (MPF) mission was that many rocks exhibit characteristics of ventifacts, rocks that have been sculpted by saltating particles. Diagnostic features identifying the rocks as ventifacts am elongated pits, flutes, and grooves (collectively referred to as ”flutes” unless noted otherwise). Faceted rocks or rock portions, circular pits, rills, and possibly polished rock surfaces are also seen and could be due, to aeolian abrasion. Many of these features were initially identified in rover images, where spatial resolution generally exceeded that of the IMP (Imager for Mars Pathfinder) camera. These images had two 227
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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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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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Page 267 and 268: SPACE PLATFORMS, 38 SPACE PROBES, 2
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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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