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  • LUNAR AND PLANETARY EXPLORATION  (138)
  • INSTRUMENTATION AND PHOTOGRAPHY  (3)
  • 1
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    First earthshine photography from lunar orbit, part S (1972)
    In:  CASI
    Details
    Publication Date: 2005-11-30
    Description: The first photographs of the moon taken with earthshine illumination by the Apollo 15 crew were examined. Emphasis in the analysis was placed on a comparison of predicted exposures and obtained exposures. The results of the investigation indicate the following: (1) The predicted exposure of the maria areas and the obtained exposures were in reasonably close agreement. (2) The apparent-albedo values obtained for the floor of Aristarchus Crater are seven times greater than those for the maria.
    Keywords: INSTRUMENTATION AND PHOTOGRAPHY
    Type: NASA. Manned Spacecraft Center Apollo 15 Prelim. Sci. Rept.; 7 p
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  • 2
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    Near-terminator photography, part R (1972)
    In:  CASI
    Details
    Publication Date: 2005-11-30
    Description: The advantages resulting from the use of near-terminator photography in lunar surface investigations are discussed. It is pointed out that, under near-terminator conditions, small changes in slope produce greater contrast changes than at high sun elevation angles. This desirable phenomenon is confirmed by an examination of the near-terminator photography taken during the Apollo 15 mission. Many of the photographs obtained show lunar surface areas within a few degrees of the terminator and are therefore of significant geologic interest. In addition, many geologic features stand out in a distinct manner not normal in conventional lunar photography, thus providing additional data on the surface morphology and the configuration of a large number of lunar surface structures.
    Keywords: INSTRUMENTATION AND PHOTOGRAPHY
    Type: NASA. Manned Spacecraft Center Apollo 15 Prelim. Sci. Rept.; 6 p
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  • 3
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    Near-terminator and earthshine photography (1973)
    In:  CASI
    Details
    Publication Date: 2006-01-11
    Description: Photographic results obtained during the Apollo 17 flight for the near terminator and earthshine conditions are discussed. Lunar surface photographs taken in the vicinity of the sunshine terminator provide important information that is not obtained on photographs taken at higher sun evaluation angles. Earthshine photography also provides data on low relief, crater morphology, and small scale structures. Examples of photographs of the lunar surface taken under both conditions are provided.
    Keywords: INSTRUMENTATION AND PHOTOGRAPHY
    Type: NASA. Johnson Space Center Apollo 17 Prelim. Sci. Rept.; 7 p
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  • 4
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    Venus: The nature of the surface from Venera panoramas (1984)
    In:  CASI
    Details
    Publication Date: 2006-04-06
    Description: Images of the surface of Venus obtained by the Soviet Venera 9, 10, 13 and 14 landers are analyzed to provide a basis for understanding the nature of geologic processes operating there. Bedrock is exposed at the Venera 10, 13 and 14 sites and is characterized by semi-continuous, flat polygonal to subrounded patches up to several meters in width. The bedrock surface is often dominated by sub horizontal to horizontal layered plates with thicknesses of several cm and abundant linear and polygonal vertical fractures. Soils (particles 1 cm) are abundant at the Venera 9, 10 and 13 sites, but are uncommon at Venera 14. Features indicative of a strong aeolian influence (moats, dunes, wind tails) are not observed. Several hypotheses are considered for the origin of the bedrock surfaces, and it is concluded that bedrock originated from surface lava flows. The relative freshness of features observed by the Veneras suggests that erosion rates are very low or that some bedrock surfaces are geologically young.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA. Washington Repts. of Planetary Geol. Program; p 76-78
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  • 5
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    Venus banded terrain: Evaluation of tectonic models for the origin of banding (1984)
    In:  CASI
    Details
    Publication Date: 2006-04-06
    Description: A tectonic orgin for Venus banded terrain is consistent with band spacing. Both compressional (folding) and extensional models for band formation can fit present observations. Band spacing cannot distinguish among scenarios for global heat loss and for the origin of highland terrain. Tectonic models for band formation indicate that the surface brittle layer in the venus highlands is no more than a few kilometers thick.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA. Washington Repts. of Planetary Geol. Program; p 74-75
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  • 6
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    Venus: Global distribution of Pioneer-Venus radar roughness and reflectivity and global correlation of altimetry, roughness and reflectivity observations (1984)
    In:  CASI
    Details
    Publication Date: 2006-04-06
    Description: An improved version of the Pionner-Venus orbital data was used for a statistical analysis of global radar roughness and (alpha(0)) (rho) reflectivity. Classification maps of the venusian surface are produced in a supervised manner on the basis of statistical and empirical studies of the individual data sets. The primary objective is to assess the degree of homogeneity of surface radar properties within topographic provinces in order to map possible geologic boundaries. Maps were produced by correlating two data sets at a time. Classification of specific regions, such as Ishtar, has demonstrated that distinct geological units can be identified.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA. Washington Repts. of Planetary Geol. Program; p 81-82
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  • 7
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    Theoretical aspects of photoclinometric terrain profiling on the Galilean satellites (1984)
    In:  CASI
    Details
    Publication Date: 2006-04-06
    Description: For large parts of the surfaces of the Galilean satellites there is no stereoscopic high resolution imagery, and so for shadow-free regions far from the terminator, the only method of obtaining topograpic information is photoclinometry, the technique of converting brightness variations into local surface tilts and hence into topographic profiles and contour maps. The conversion from brightness changes to slopes require knowledge of the angular photometric function for the type of planetary surface terrain being analyzed, i.e., the relationship describing the brightness of the surface as a function of the angles of incidence (I) and emergence (E) of light at a surface element. In order to investigate the effects of these changes on the shapes of topographic profiles deduced from the functions, an area of grooved terrain (lines 500-505, samples 550-650 on frame 20640.27 0060J2) using wide ranges of values of all the adjustable parameters in Hapke's new photometric function were analyzed.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA. Washington Repts. of Planetary Geol. Program; p 27-28
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  • 8
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    Elysium Region, Mars: Characterization of tectonic features (1984)
    In:  CASI
    Details
    Publication Date: 2006-04-06
    Description: In this paper the tectonic features of the Elysium region are identified and characterized. Identification of features was made using USGS controlled photomosaics (Elysium quadrangle, and portions of Amenthes and Cebrenia quadrangles); Viking Orbiter photographic data were used in individual cases to assist in identification. The positions and orientations of tectonic features can then be used, in conjunction with estimates of the mass of the volcanic load obtained from gravity modelling, to constrain the thickness of the elastic lithosphere in the region.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA. Washington Rept. of Planetary Geology Program, 1983; p 291-292
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  • 9
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    Surface compositions in the Aristarchus Region: Implications for regional stratigraphy (1984)
    In:  CASI
    Details
    Publication Date: 2006-04-06
    Description: Near infrared reflectance spectra for the Aristachus region, obtained using the 2.2m UH telescope at the Mauna Kea Observatory, were reduced and analyzed. The spectra obtained for the central peak, southern floor, southwestern wall, eastern wall, and northwestern wall of Aristachus crater exhibit shallow continuum slopes, relatively strong feldspar bands, pyroxene bands stronger than those typically seen in the spectra of fresh higland features, and pyroxene band centers near l micrometer suggesting the dominance of Ca rich clinopyroxene. The spectrum of the south rim of Aristachus is quite distinct from those of other crater units. The position of Aristrchus on the plateau/mare boundary raises questions concerning compositional variations in crater ejects deposits.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA. Washington Rept. of Planetary Geology Program, 1983; p 250-252
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  • 10
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    Geology of Maxwell Montes, Venus (1984)
    In:  CASI
    Details
    Publication Date: 2006-04-06
    Description: Maxwell Montes represent the most distinctive topography on the surface of Venus, rising some 11 km above mean planetary radius. The multiple data sets of the Pioneer missing and Earth based radar observations to characterize Maxwell Montes are analyzed. Maxwell Montes is a porkchop shaped feature located at the eastern end of Lakshmi Planum. The main massif trends about North 20 deg West for approximately 1000 km and the narrow handle extends several hundred km West South-West WSW from the north end of the main massif, descending down toward Lakshmi Planum. The main massif is rectilinear and approximately 500 km wide. The southern and northern edges of Maxwell Montes coincide with major topographic boundaries defining the edge of Ishtar Terra.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA. Washington Repts. of Planetary Geol. Program; p 79-80
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