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  • 1
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    Planetary astronomy (1986)
    In:  CASI
    Details
    Publication Date: 2006-02-14
    Description: Comets were studied during their relatively quiescent phases at large distances from the sun. This program, has resulted in a variety of CCD images of comets in several visible and near-IR bands selected to sample the continuum, rather than emission features. The most extensive dataset was obtained for P/Halley during January 1985 (plus scattered earlier data), near the time the comet turned on. The data were reduced in a preliminary fashion. Other comets predicted to be relatively inactive (including Neujmin 1 and Arend-Rigaux) were most active than expected. P/Gehrels 3 was also observed.
    Keywords: ASTRONOMY
    Type: NASA, Washington Reports of Planetary Astronomy, 1985; p 82-84
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  • 2
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    Epsilon Aurigae (1985)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: In April 1984, fourth contact ended the two year long eclipse of Epsilon Aurigae. An astrometric study of the study of the system was carried out by Van de kamp (1978) leading to the conclusion that the orbit is seen very close to edge on. The eclipse was monitored by a number of groups from the ground and from spacecraft such as the IUE. Ultraviolet observations of the system from IUE have thrown new light on the nature of the system that led to the conclusion that the secondary object is probably a cold, dusty accretion disk surrounding a star that is completely hidden inside the disk.
    Keywords: ASTRONOMY
    Type: Astrophysics and Space Science (ISSN 0004-640X); 110; 1, Ma
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  • 3
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    Families of minor planets (1979)
    In:  Other Sources
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    Publication Date: 2011-08-17
    Description: Physical studies of individual family members show that at least the Themis, Eos, Koronis, Nysa/Hertha, and Budrosa families of minor planets are the result of the breakup of discrete parent bodies. Only a few families have been studied in detail, and even in those few cases, the full force of observational techniques has not been applied. Crucial for the understanding of families and their parent bodies are detailed physical studies of family members; precise mineralogical interpretation of observational data to identify the geochemistry of the parent bodies; and studies of the collisional evolution of family members.
    Keywords: ASTRONOMY
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  • 4
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    Pre-eclipse ultraviolet spectra of Epsilon Aurigae (1982)
    In:  Other Sources
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    Publication Date: 2011-08-18
    Description: Existing high dispersion, long wavelength IUE, high dispersion long and short wavelength, and Balloon borne ultraviolet stellar spectrograph (BUSS) spectra providing a baseline measurement of the ultraviolet spectrum of the Epsilon Aurigae system before eclipse are reviewed. Plans for ultraviolet spectrum IUE observations during the 1982 to 1984 eclipse of Epsilon Aurigae are presented.
    Keywords: ASTRONOMY
    Type: Advan. in Ultraviolet Astron.; p 505-508
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  • 5
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    Planetary astronomy (1991)
    In:  CASI
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    Publication Date: 2013-08-31
    Description: The goal is to use a variety of observational techniques and instruments, and to reduce, interpret, and synthesize ground based astronomical data concerning small bodies in the solar system, especially the asteroids, in order to study the compositions, physical characteristics, population properties, and evolution of these bodies. Progress was made in the following areas: faint asteroid taxonomy survey; photometric geodesy of Main Belt asteroids; and Main Belt and Near Earth Asteroids synthesis studies.
    Keywords: ASTRONOMY
    Type: NASA, Washington, Reports of Planetary Astronomy, 1991; p 27-28
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  • 6
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    Planetary astronomy (1991)
    In:  CASI
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    Publication Date: 2013-08-31
    Description: Many asteroids are known to be non-spherical, as revealed by changes in their brightness as they rotate (light curves) and present varying cross-sections to view. Models of collisional evolution of the asteroid belt suggest that many of the larger asteroids are shattered rubble piles, consisting of fragments bound together by gravity. If these assemblages are sufficiently weak, they should relax to equilibrium shapes that depend only on their spin periods and densities. Thus, if shape of an asteroid is known, one might infer its density and internal structure.
    Keywords: ASTRONOMY
    Type: NASA, Washington, Reports of Planetary Astronomy, 1991; p 149
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  • 7
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    Near-Earth asteroids: Observer alert network and database analysis (1991)
    In:  CASI
    Details
    Publication Date: 2013-08-31
    Description: The Planetary Science Institute (PSI) was funded by SERCulpr to develop a communication network to alert observers of newly discovered near-earth asteroids (NEA's). This network is intended to encourage observers to obtain physical observations of NEA's, which are needed in order to characterize and assess the resource potential of these bodies. This network was declared operational in October 1990 via an announcement to the asteroid observing community. The PSI is also supported to develop the Near-Earth Asteroid Database (NEAD), a comprehensive database of physical and dynamical data on NEA's. In the past year, the database was updated on newly discovered NEA's during 1990, and new data on radar observations and dynamical classifications were added.
    Keywords: ASTRONOMY
    Type: Arizona Univ., NASA Space Engineering Research Center for Utilization of Local Planetary Resources; 7 p
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  • 8
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    Collisional evolution of asteroids - Populations, rotations, and velocities (1979)
    In:  Other Sources
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    Publication Date: 2011-08-17
    Description: The collisional evolution of various initial populations of asteroids is simulated numerically and compared with the present asteroid size-frequency distribution to find those populations which collisionally relax to the present belt. Both orbital and size distributions are treated, as well as the simultaneous evolution of two collisionally interacting populations with different physical properties. If the initial belt distribution was a power law, the initial belt population at the time when the present high-collision speed was established was probably only modestly larger than the present population. However, other distributions allow a more massive early belt. The rotational evolution due to collisions of asteroids with power-law distributions is also examined and compared with observations, leading to conclusions generally in agreement with those of size evolution. The high-collision speed in the present belt is likely due to Jupiter. Gravitational stirring by massive Jupiter-scattered planetesimals or secular resonances sweeping through the belt are the most probable mechanisms.
    Keywords: ASTRONOMY
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  • 9
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    The 1982 eclipse of 31 Cygni (1984)
    In:  Other Sources
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    Publication Date: 2011-08-18
    Description: UBV photometry and optical-UV spectroscopy of the primary eclipse of the long period Zeta Aurigae-like system 31 Cygni are reported. The precise timings made possible by the photometry imply that the spectral features could be due to an accretion shock associated with a hot star embedded in an extended chromosphere surrounding the red supergiant. The data also suggest an extended clumpy structure to the atmosphere of the late-type supergiant in the binary.
    Keywords: ASTRONOMY
    Type: Astrophysical Journal, Part 1 (ISSN 0004-637X); 281; 751-759
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  • 10
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    Planetary astronomy (1979)
    In:  CASI
    Details
    Publication Date: 2019-06-27
    Description: Activities summarized relate to spectrophotometric observations and analysis of asteroids; further observations of the peculiar asteroid 624 Hektor; the search for further asteroid close encounters suitable for mass determination; the infrared search for intra-Mercurial bodies; the search for Venus ashen light; multicolor areal photometry of Uranus and Neptune; and ground-based observations of the Galilean satellites to support the Voyager mission. The following topics are examined: (1) Hektor: the largest highly elongated asteroid; (2) Uranus: disk structure within the 7300 Angstrom methane band; (3) Neptune: limb brightening within the 7300 Angstrom methane band; (4) Neptune's rotation period: a correlation and a speculation on the effect of the disk brightness distribution; (5) observing report on 1979 activities at Kitt Peak National Observatory; and (6) dynamical evolution of intra-Mercurial planetesimals.
    Keywords: ASTRONOMY
    Type: NASA-CR-162526
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