Scientific and Technical Aerospace Reports Volume 39 April 6, 2001

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20010022983 NASA Goddard Space Flight Center, Greenbelt, MD USA Code Sharing and Collaboration: Experiences from the Scientist’s Expert Assistant Project and their Relevance to the Virtual Observatory Jones, Jeremy, NASA Goddard Space Flight Center, USA; Grosvenor, Sandy, Booz-Allen and Hamilton, Inc., USA; Wolf, Karl, Commerce One, Inc., USA; Li, Connie, Commerce One, Inc., USA; Koratkar, Anuradha, Space Telescope Science Inst., USA; [2001]; 1p; In English; Astronomical Data Analysis, 29 Jul. - 3 Aug. 2001, San Diego, CA, USA; Sponsored by International Society for Optical Engineering, USA; No Copyright; Avail: Issuing Activity; Abstract Only In the Virtual Observatory (VO), software tools will perform the functions that have traditionally been performed by physical observatories and their instruments. These tools will not be adjuncts to VO functionality but will make up the very core of the VO. Consequently, the tradition of observatory and system independent tools serving a small user base is not valid for the VO. For the VO to succeed, we must improve software collaboration and code sharing between projects and groups. A significant goal of the Scientist’s Expert Assistant (SEA) project has been promoting effective collaboration and code sharing between groups. During the past three years, the SEA project has been developing prototypes for new observation planning software tools and strategies. Initially funded by the Next Generation Space Telescope, parts of the SEA code have since been adopted by the Space Telescope Science Institute. SEA has also supplied code for SOFIA, the SIRTF planning tools, and the JSky Open Source Java library. The potential benefits of sharing code are clear. The recipient gains functionality for considerably less cost. The provider gains additional developers working with their code. If enough users groups adopt a set of common code and tools, defacto standards can emerge (as demonstrated by the success of the FITS standard). Code sharing also raises a number of challenges related to the management of the code. In this talk, we will review our experiences with SEA - both successes and failures - and offer some lessons learned that may promote further successes in collaboration and re-use. Author Observatories; Virtual Reality; Computer Programs 20010023280 Lembaga Penerbangan dan Antariksa Nasional, Solar and Space Environment, Jakarta, Indonesia New Crescent Moon Visibility in Indonesia Visibilitas Hilal Di Indonesia Djamaluddin, T., Lembaga Penerbangan dan Antariksa Nasional, Indonesia; Warta LAPAN; October 2000; ISSN 0126-9754; Volume 2, No. 4, pp. 137-145; In Malay-Indonesian; Copyright; Avail: Issuing Activity Research on crescent visibility in Indonesia has not been conducted yet systematically based on astronomical analysis to obtain the criteria of possibility of crescent sighting. While, the criteria are needed in determining the beginning of Islamic calendar, especially for Ramadhan, Shawal, and Zulhijjah. This analysis is conducted to overcome such a problem, by using documentation of crescent sighting during 1962-1997 in Indonesia. The results can be concluded as follows: Crescent sighting with low altitude tends to be reported from less then 3 location, likely due to misjudging of foreground object (e.g. lamp) considered as crescent. Misjudging of the crescent due to misidentification of planet Venus or Mercury is proved for low altitude crescent sighting. After eliminating foreground and background objects, it is obtained the criteria of crescent visibility in Indonesia: (1). Moon age should be is greater than 8 hours. (2). Moon-Sun angle should be is greater than 5,6 deg. (3). Moon-Sun altitude difference should be is greater than 3 deg (crescent’s altitude is greater than 2 deg) for Moon-Sun azimuth difference of approximately 6 deg, while for Moon-Sun azimuth difference is less than 6 deg, it is needed more altitude difference. For Moon-Sun azimuth difference of about 0 deg, the altitude difference should be is greater than 9 deg. Author Moon; Sun; Visibility; Indonesia 20010026229 Smithsonian Astrophysical Observatory, Cambridge, MA USA EUV and X-Ray Variability in Seyfert Galaxies: A Study with Simultaneous EUVE and SAX Observations Final Report, 1 Apr. 1998 - 31 Mar. 2000 Fruscione, Antonella, Smithsonian Astrophysical Observatory, USA; March 2001; 2p; In English Contract(s)/Grant(s): NAG5-7115; No Copyright; Avail: CASI; A01, Hardcopy; A01, Microfiche Only one target (RE 1034+393) was awarded to this grant out of the two asked. The work relative to this object has been completed and one paper summarizing the results was prepared for the astronomical literature. Author Extreme Ultraviolet Explorer Satellite; Seyfert Galaxies; Extreme Ultraviolet Radiation; Variability; Ultraviolet Astronomy 278
90 ASTROPHYSICS �� 20010022633 Stanford Univ., Center for Turbulence Research, Stanford, CA USA In Pusuit of Structures in Protoplanetary Disks Umurhan, O.M., Stanford Univ., USA; Annual Research Briefs - 2000: Center for Turbulence Research; December 2000, pp. 17-30; In English; See also 20010022631; No Copyright; Avail: CASI; A03, Hardcopy; A03, Microfiche This brief summarizes work devoted to studying the linear stability of baroclinic protoplanetary Keplerian disks. This work largely builds on the foundation and fundamental results obtained by Barranco, Marcus, and Umurhan (hereafter BMU) which presented a model to describe structures in weakly baroclinic Keplerian disks. Interest in protoplanetary disks has grown since the discovery of the first of what are now dozens of extrasolar planets around F and G type stars. The apparent ubiquity of planets suggests that the nebular disks (or protoplanetary disks), out of which these stars are born, must be susceptible to the development of structures. However, theoretical work (see references in BMU) argues that purely pressure-supported gaseous barotropic Keplerian disks do not undergo any known type of hydrodynamic instabilities. The basis for this claim is that the strong rotation in Keplerian shear flows manages to suppress any of the usual instabilities seen in laboratory shear flows such as the Taylor- Couette and Kelvin-Helmholtz instabilities. Some investigators have gone so far as to claim that protoplanetary disks are featureless objects totally bereft of vortical structures or long-lasting stable patterns. to counter this assertion, some investigators have suggested that the protoplanetary disk is sufficiently magnetized to undergo a magneto-rotational instability as first explored by Chandresekhar using linear analysis and later demonstrated numerically by Balbus, Hawley, and Stone for fully nonlinear flows. However, Desch has indicated that disks suspected to be around solar type stars will be too cool and weakly ionized such that local dust particles in short time will sweep up the ionization in the gas, leaving the fluid nearly neutral. What little ionization is left in the disk is too little to allow strong coupling to an external magnetic field. Thus this mechanism is unlikely to play an important role in the formation of planets at the radii where the large gas giants are observed to reside. The point of view taken by BMU is that a weakly baroclinic Keplerian disk will produce the type of shear flow that will promote hydrodynamical instabilities. The assumption was that the added component of vertical shear driven by baroclinic effects generates coherent structures in an otherwise featureless protoplanetary disk. to isolate this effect they derived a number of asymptotic reductions of the 3D Euler equations in cylindrical geometry with a central mass source. Author Baroclinity; Shear Flow; Stability; Mathematical Models 20010025059 NASA Ames Research Center, Moffett Field, CA USA Identification of Gas Phase PAHs in Absorption Towards Protostellar Sources Bregman, Jesse D., NASA Ames Research Center, USA; Temi, Pasquale, NASA Ames Research Center, USA; [2000]; 10p; In English; Sponsored in part by ESA Member States: France, Germany, the Netherlands and the UK Contract(s)/Grant(s): RTOP 344-02-00-99; No Copyright; Avail: CASI; A02, Hardcopy; A01, Microfiche The infrared emission bands (also known as the UIR bands.) have recently been observed in absorption at 3.25 micrometers in the ices surrounding a few proto-stellar objects at 11.2 micrometers in MonR2, and at 6.2 micrometers towards two sources near the galactic center. The UIR bands have been observed in emission for many years, but identifying these bands has proven to be both difficult and contentious as no one has yet found a single material that provides a good match to the features. However, most investigators agree that some form of carbon-based material with aromatic bonds is the most likely candidate, and many arguments favor free molecules (polycyclic aromatic hydrocarbons, PAHs) as the carriers of at least the narrow emission bands. Since the emission arises not from a single molecule but from a family of molecules, identifying which PAHs are contributing to the infrared emission bands is difficult. The identification is further complicated by the fact that the emission at short wavelengths is dominated by small molecules while at long wavelengths it is dominated by large molecules. Thus, for example, the emission at 3.3 micrometers is from a different mix of molecules than those which produce the 11.2 micrometer band. to complicate matters further, the molecular mix includes both neutral and ionic species. In absorption, the same mixture of molecules contributes at all wavelengths and the molecules should be neutral, potentially simplifying comparisons with lab data. Also, absorption strengths measured in the lab are directly applicable to interstellar absorption bands without the need to model an emission spectrum of an unknown mixture of ionized and neutral PAHs. In this paper we show that a mixture of argon matrix isolated PAH molecules can reproduce the 3.25 micrometers absorption band seen in the ISO SWS spectra of four embedded Infrared 279
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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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Subject Categories of the Division
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73 Nuclear Physics 263 Includes nuc
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Document Availability Information T
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Avail: NASA Public Document Rooms.
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Hardcopy & Microfiche Prices Code N
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ALABAMA AUBURN UNIV. AT MONTGOMERY
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03 AIR TRANSPORTATION AND SAFETY
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work of the JAA had established thi
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20010024868 Federal Aviation Admini
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20010023437 Defence Science and Tec
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The Models for Aeroelastic Validati
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20010025824 Pratt and Whitney Aircr
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20010023064 NASA Langley Research C
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17 SPACE COMMUNICATIONS, SPACECRAFT
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20010026207 NASA, Washington, DC US
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The objective of the proposed resea
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20010022640 Stanford Univ., Center
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ustion, showing that these can have
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20010026184 Oak Ridge National Lab.
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film. Subsequent electroless metal
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20010024029 Houston Univ., Dept. of
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equipment indicate a change in the
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interaction, the main gas products
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Contract(s)/Grant(s): W-7405-eng-48
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for detecting and measuring deviato
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work, additional significant effect
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20010026182 Oak Ridge National Lab.
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20010024162 Army Research Lab., Ade
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matching funds. MIRSL purchased an
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20010023557 North Dakota State Univ
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20010026217 Princeton Univ., NJ USA
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20010024108 Center for Naval Analys
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undertaken to isolated it are descr
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non-buoyant axisymmetric jet issuin
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point. The other turbulent problem
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20010024042 Houston Univ., Dept. of
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The research carried out in the Hea
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along the heater surface and depart
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cal transducers. Additionally, the
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tial for its successful commercial
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This project represents a combined
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20010024910 Johns Hopkins Univ., De
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e caused by a non-uniform temperatu
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metric shear cell, employed upon th
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20010024919 Alabama Univ., Huntsvil
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Newtonian fluids in the laboratory,
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Boussinesq convection where due to
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20010024930 Creare, Inc., Hanover,
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Illumination of a space-borne objec
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The hydrodynamics near steadily mov
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to be done is the full coupled syst
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liquid crystal host. Since the ulti
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the inorganic synthesis using press
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when the buoyancy is removed, for e
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20010024956 NASA Ames Research Cent
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2.2-second drop tower at NASA Glenn
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we have examined the dynamical beha
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position of the interface. An oscil
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the first time, non-intrusive, high
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’axial curvature pressure’. A t
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moons when disturbed by low velocit
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particle size was studied. In a den
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colliding drops. The viscous resist
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20010024983 Notre Dame Univ., Physi
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20010024986 TDA Research, Inc., Whe
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drop deposition, using Schiaffino a
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and extended to reduced gravity flo
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from an isolated bubble regime to a
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20010025000 Case Western Reserve Un
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our experimental measurements and w
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sured using a hot film probe flush
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the stationary bubble entrains anot
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we have collaborated on 3D experime
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of the most attractive characterist
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apply either steady shear flow perp
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20010025024 NASA, Washington, DC US
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neously the gamma scattered method
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20010023125 Colorado Univ., Lab. fo
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Contract(s)/Grant(s): F19628-95-C-0
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ics Technology Letters; March 2000;
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The BOREAS RSS-1 team collected sur
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ically corrected; however, files of
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with wavelength bands specific to t
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20010022099 NASA Goddard Space Flig
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within the polygon). There are thre
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A03, Hardcopy; A01, Microfiche Cana
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storms in Africa and smoke plumes f
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Greenland, with the objective of qu
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The BOReal Ecosystem-Atmosphere Stu
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The BOREAS TGB-8 team collected dat
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Report No.(s): NASA/TM-2000-209891/
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The BOREAS TF-10 team collected tow
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cally Active Radiation (FPAR) absor
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tributing to the overall understand
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cal ’tour de force’ allows EPV
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20010023558 Texas Univ., Center for
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the atmospheric concentrations of m
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20010023278 Lembaga Penerbangan dan
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Atmospheric radiation in the infrar
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20010022976 Desert Research Inst.,
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The primary purpose of AASERT Grant
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with only small ice-covered areas r
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Task 2 - abstraction of Medical rec
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non-steroidal activators of the rec
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20010023796 Massachusetts Univ. Med
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20010024166 Chicago Univ., Chicago,
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20010025069 Cleveland Clinic Founda
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Prior to 1994, measurement of tumor
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20010025730 Illinois Univ., Broad o
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Page 283 and 284: from the Lagrangian of the system.
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Page 337 and 338: ATMOSPHERIC RADIATION, 163, 205 ATM
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Cledassou, R., 311 Clemmet, J., 306
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Gorelick, N., 294 Gorevan, S. P., 4
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Kupinski, Matthew A., 256 Kuznetz,
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Parks, C. H., 249 Parr, T. P., 38 P
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Swisdak, Michael M., Jr., 37 Szalew
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