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  • 1
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    Lunar impact basins and crustal heterogeneity - New western limb and far side data from Galileo (1992)
    In:  Other Sources
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    Publication Date: 2011-08-24
    Description: Multispectral images of the lunar western limb and far side obtained from Galileo reveal the compositional nature of several prominent lunar features and provide new information on lunar evolution. The data reveal that the ejecta from the Orientale impact basin (900 kilometers in diameter) lying outside the Cordillera Mountains was excavated from the crust, not the mantle, and covers pre-Orientale terrain that consisted of both highland materials and relatively large expanses of ancient mare basalts. The inside of the far side South Pole-Aitken basin (greater than 2000 kilometers in diameter) has low albedo, red color, and a relatively high abundance of iron- and magnesium-rich materials. These features suggest that the impact may have penetrated into the deep crust or lunar mantle or that the basin contains ancient mare basalts that were later covered by highlands ejecta.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Science (ISSN 0036-8075); 255; 570-576
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  • 2
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    Cratering of planetary satellites (1986)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: Recent findings concerning craters and cratering populations on the satellites of Jupiter and Saturn are discussed. Current understanding of cratering mechanics is reviewed with emphasis placed on scaling and ejecta and the differences between cratering in rock and ice. Evidence from crater statistics regarding cratering histories on various planetary satellites is discussed and connections are made with what is known about the cratering record on the terrestrial bodies. Consideration is given to the source populations and an attempt is made to summarize and critique the various scenarios that have been proposed for linking the cratering records on the various planets and satellites. It is noted that early Voyager Uranus results seem compatible with the present summary.
    Keywords: LUNAR AND PLANETARY EXPLORATION
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  • 3
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    Cratering of the Uranian satellites (1991)
    In:  Other Sources
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    Publication Date: 2011-08-24
    Description: Available crater counts and their interpretations are reviewed, with emphasis on essential scaling considerations and comparisons with hypotheses developed for interpreting the cratering records on other planets and satellites. New approaches are employed to scaling based on new measurements of crater depths and morphology, which show craters in ice to be unexpectedly different from those in rock. It is found that the published crater counts on the Uranian satellites, despite mutual inconsistencies, can be interpreted as compatible with cratering by the heliocentric population of cometary bodies that was responsible for much of the cratering of the satellites of Jupiter and Saturn. Scaling arguments are applied to the catastrophic breakup of icy satellites and ring particles. The importance of large-scale collisions in disrupting the inner Uranian satellites is found to depend on the shape of the size distribution of cometary bodies at large sizes.
    Keywords: LUNAR AND PLANETARY EXPLORATION
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  • 4
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    New spectral observations of Callisto and leading/trailing hemisphere distinctions (1991)
    In:  CASI
    Details
    Publication Date: 2013-08-31
    Description: In December 1989 and January 1990, new observations of the leading and trailing edges of Callisto were made from the NASA Infrared Telescope Facility on Mauna Kea in Hawaii. Using the Cool Grating Array Spectrometer, spectral coverage was obtained from 1.89 to 2.46 microns and from 2.8 to 4.2 microns for both the leading and trailing hemispheres. In addition, spectral coverage of the leading hemisphere was obtained from 1.30 to 2.55 microns and from 4.2 to 4.8 microns. Interpretations of the data are given.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA, Washington, Reports of Planetary Geology and Geophysics Program, 1990; p 294-295
    Format: application/pdf
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  • 5
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    Evidence for ammonium-bearing minerals in Ceres (1991)
    In:  CASI
    Details
    Publication Date: 2013-08-31
    Description: Evidence for ammonium-bearing minerals was found on the surface of the largest asteroid Ceres. The presence of ammonium-bearing clays suggests that Ceres has experienced a period of alteration by substantial amounts of an ammonium-bearing fluid. The presence of the ammonium-bearing clays does not preclude Ceres maintaining a volatile inventory in the core or in a volatile-rich zone at some distance below the surface. Telescopic observations of Ceres, using the 3.0 meter NASA Infrared telescope facility prompted this reevaluation of its surface mineralogy.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst., 22nd Lunar and Planetary Science Conference; p 31-33
    Format: application/pdf
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  • 6
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    Mercury (1988)
    In:  Other Sources
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    Publication Date: 2016-03-09
    Description: Papers are presented on future observations of and missions to Mercury, the photometry and polarimetry of Mercury, the surface composition of Mercury from reflectance spectrophotometry, the Goldstone radar observations of Mercury, the radar observations of Mercury, the stratigraphy and geologic history of Mercury, the geomorphology of impact craters on Mercury, and the cratering record on Mercury and the origin of impacting objects. Consideration is also given to the tectonics of Mercury, the tectonic history of Mercury, Mercury's thermal history and the generation of its magnetic field, the rotational dynamics of Mercury and the state of its core, Mercury's magnetic field and interior, the magnetosphere of Mercury, and the Mercury atmosphere. Other papers are on the present bounds on the bulk composition of Mercury and the implications for planetary formation processes, the building stones of the planets, the origin and composition of Mercury, the formation of Mercury from planetesimals, and theoretical considerations on the strange density of Mercury.
    Keywords: LUNAR AND PLANETARY EXPLORATION
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  • 7
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    Spectral properties of water ice and contaminants (1985)
    In:  Other Sources
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    Publication Date: 2019-06-28
    Description: For remote sensing studies of ices in the solar system, it is important to understand the optical properties of water ice, and mixtures of ice and particulate materials. The present paper has the objective to review the current understanding of the spectral properties of ice, and mixtures of ice and particulates. The review is to provide a basis for the understanding of the remote sensing of ice. It is found that reflectance spectra of ice-soil intimate mixtures are complex, nonlinear functions of the optical and physical properties of the components which comprise the surface.
    Keywords: LUNAR AND PLANETARY EXPLORATION
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  • 8
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    Spectral Units on Europa and Ganymede (1985)
    In:  CASI
    Details
    Publication Date: 2014-10-09
    Description: Comparisons of Europa and Ganymede multispectral data show that Ganymede is less spectrally variable than Europa. Four major spectral units dominate Ganymede, corresponding to the ancient cratered terrain and the grooved terrain in the leading and trailing hemispheres. A hemispheric asymmetry in UV absorption definitely exists on Ganymede, although it is not so strong as that on Europa. Comparison of normalized spectra for the four major units shows that the sense of the asymmetry (more absoption toward shorter wavelengths on the trailing hemisphere) is also the same on the two bodies. This hemispheric asymmetry is interpreted as evidence of alteration of the surface by magnetospheric bombardment or micrometorite bombardment. It is concluded that the pattern observed represents a steady state involving both of these exogenic modifying agents. The spectral changes which could be produced by these two processes are grain size alteration and changes in composition. The spectral effects of variation in water ice grain size are fairly well known. Laboratory experiments are being conducted to study the spectral effects of sulfur irradiation on water ice.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA, Washington Repts. of Planetary Geol. and Geophys. Program, 1984; p 413-414
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  • 9
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    First Direct Detection of Clay Minerals on Mars (1985)
    In:  CASI
    Details
    Publication Date: 2014-10-09
    Description: Magnesian clays or clay-type minerals were conclusively detected in the martian regolith. Near-IR spectral observations of Mars using the Mauna Kea 2.2-m telescope show weak but definite absorption bands near microns. The absorption band positions and widths match those produced by combined OH stretch and Mg-OH lattice modes and are diagnostic of minerals with structural OH such as clays and amphiboles. Likely candidate minerals include serpentine, talc, hectorite, and sponite. There is no spectral evidence for aluminous hydroxylated minerals. No distinct band occurs at 2.55 microns, as would be expected if carbonates were responsible for the 2.35 micron absorption. High-albedo regions such as Elysium and Utopia have the strongest bands near 2.35 microns, as would be expected for heavily weathered soils. Low-albedo regions such as Iapygia show weaker but distinct bands, consistent with moderate coatings, streaks, and splotches of bright weathered material. In all areas observed, the 2.35-micron absorption is at least three times weaker than would be expected if well-crystallized clay minerals made up the bulk of bright soils on Mars.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA, Washington Repts. of Planetary Geol. and Geophys. Program, 1984; p 391-392
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  • 10
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    Cratering on Gaspra (1993)
    In:  Other Sources
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    Publication Date: 2019-01-25
    Description: The October 1991 Galileo flyby of Gaspra shows that its crater population is dominated by fresh craters several hundred meters in diameter and smaller. They appear to represent a production population because the spatial density is relatively low (few overlaps) and because fresh craters are very abundant; equilibrium could be attained at diameters near to or below the resolution limit of the best image. These craters are the first direct record of the population of main-belt asteroids some tens of meters in diameter. Craters primarily from the highest resolution, 'high phase' image, on which over 600 craters are visible in 90 sq. km were counted, measured, and classified; earlier counts were made on the lower resolution four-color images, which show an order of magnitude fewer craters because of the resolution limit. The population index (exponent of the differential power law approximately describing the crater sizes) has a very high negative value (-4.3 +/- 0.3, meaning that the log-log slope is 'steep'), appreciably steeper than the value of -3.5 thought to reflect collisional equilibrium according to theory.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Twenty-fourth Lunar and Planetary Science Conference. Part 1: A-F; p 269-270
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