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  • 1
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    Geology of Potrillo maar, New Mexico and northern Chihuahua, Mexico (1965)
    American Journal of Science
    Details
    Publication Date: 1965-05-01
    Print ISSN: 0002-9599
    Electronic ISSN: 1945-452X
    Topics: Geosciences
    Published by American Journal of Science
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    PAPER CURRENT
  • 2
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    Inversion of topography in Martian highlands terrains (1984)
    In:  CASI
    Details
    Publication Date: 2006-04-06
    Description: One unique feature on Mars is the presence of ring furrows which are apparently produced by inversion of topography at the rims of partially buried craters. Ring furrows are flat-floored trenches, circular in plan view, forming rings 7 to 50 km in diameter. The moat is on the order of 0.5 km deep and 2 to 10 km wide, and it surrounds a flat topped circular mesa or plateau that is 5 to 40 km across. The central plateau is at the same elevation or lower than the surrounding plain outside the ring. The circular nature and size range of ring furrows tend to suggest that these features are related to craters partially buried by younger lava flows. The rings have been formed by preferential removal of the exposed crater rims. Ground ice decay, sapping, or fluvial erosion removed the less resistant, porous material of crater rims while leaving the more resistant volcanic flow material. Differential erosion has thus led to a reversal of topography in which the original positive relief of the rim is reduced to a negative relief feature.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA. Washington Rept. of Planetary Geology Program, 1983; p 228-229
    Format: text
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  • 3
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    Progressive impact cratering (1984)
    In:  CASI
    Details
    Publication Date: 2006-04-06
    Description: Most cratering experiments are designed to study the effects of a single hypervelocity impact into a target of uniform properties. Experiments involving multiple impacts are usually limited to low velocity projectiles and unconsolidated target materials. Gault described saturation cratering in an unconsolidated target. Quaide and Oberbeck studied crater forms produced by hypervelocity impact into layered targets. Several investigators have modeled the generation of either a regolith or megaregolith by repeated impact on planetary surfaces. Studies now in progress examine changes in crater morphology and target properties by repeated impact into an initially consolidated target. Current studies employ low velocity projectiles (2 g at 0.5 km/sec) and consolidated salt targets. Records of crater size, morphology, and accumulated ejecta thickness are maintained as impacts collect on the surface.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA. Washington Rept. of Planetary Geol. Program, 1983; p 102-103
    Format: text
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    NASA TECHNICAL REPORTS
  • 4
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    Flood routing of the Maja outflow across Xanthe Terra (1991)
    In:  CASI
    Details
    Publication Date: 2013-08-31
    Description: The object is to trace a single flood crest through the Maja outflow system and to evaluate the effects of topography on ponding and multiple channel routing. Maja Valles provides a good model because it has a single source and a well defined channel system. The 1500 km long Maja Valles originates in Juventae Chasma. The outflow system stretches 1100 km northward along the Lunae Planum/Xanthe Terra boundary, then eastward across the Xanthe Terra highlands. It descends to Chryse Planitia where it extends northeastward toward the middle of the basin. It is concluded that flood routing through multiple channels and retardation in local impoundments are responsible for breakup of the initial flood crest and the formation of multiple flood crests. Recombined flow near the mouths of these canyons results in an extended flow regime and multiple flood surges. As a result of ponding along the flood course, depositional sites are localized and renewed erosion downstream (from ponded sites) results in sediment source areas not greatly removed from depositional sites.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA, Washington, Reports of Planetary Geology and Geophysics Program, 1990; p 140-142
    Format: application/pdf
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  • 5
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    Progress in determining the thickness and distribution of volcanic materials on Mars (1987)
    In:  CASI
    Details
    Publication Date: 2013-08-29
    Description: Volcanic plains and constructs comprise over half the surface of Mars. Volume estimates require sensible estimates of the thickness of volcanic materials. The completion of the 1:2 M Viking photomosaics and a refined geologic map based on Viking photography set the stage for improved thickness studies and volume estimates. Currently, a revised (but incomplete) data base of 740 partially buried craters was compiled using Mars photomosaics at 1:2 M for initial identification and measurement.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst., MEVTV Workshop on Nature and Composition of Surface Units on Mars; p 54-56
    Format: text
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  • 6
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    Thickness of Ridged Plains Materials in Hesperia Planum, Mars (1985)
    In:  CASI
    Details
    Publication Date: 2014-10-08
    Description: The thickness distribution of plains-forming materials in Hesperia Planum is determined by the diameter of partially buried craters. As with all Martian thickness studies, the distribution of measured thicknesses is sparse due to a low number of suitable partially buried craters. The resulting isopach of plains materials has a low level of confidence but is sufficient for generalized thickness trends. The mean of the thickness estimates is 360 + or - 120 m. The isopach of plains-forming materials exhibits an uneven thickness distribution. Average thickness, determined by grid sampling over the region, is 216 + or - 153 m. Local lenses exceed 500 m. A fifth order trend surface provides a partial match (coefficient of correlation = 0.657) to the isopach.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA, Washington Repts. of Planetary Geol. and Geophys. Program; p 242-244
    Format: text
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  • 7
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    Ridged Plains of Lunae Planum: Thickness Distribution Revised (1985)
    In:  CASI
    Details
    Publication Date: 2014-10-08
    Description: New data are used to revise the isopach of plains-forming material in the Lunae Planum region. The distribution of data points in the region has not increased; consequently, the new map is still valid for generalized thickness trends only. The isopach map is based on a total of 65 points; 32 points represent thickness estimates at partially buried craters. The remaining 33 points define the limits of plains-forming materials (zero thickness). Suitable buried craters are randomly distributed and sparse near the western edge and northern portion of the area. The overall thickness trend is similar to the previously mapped distribution, but there is a significant reduction in thickness values.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA, Washington Repts. of Planetary Geol. and Geophys. Program; p 237-238
    Format: text
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  • 8
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    Duration and rates of discharge: Maja Valles, Mars (1992)
    In:  CASI
    Details
    Publication Date: 2013-08-29
    Description: The 1600 km-long Maja Valles outflow system of Mars consists of three major divisions including the upper valley on Lunae Planum, the canyon section across Xanthe Terra, and the lower valley across western Chryse Planitia. Although water released from the source in Juventae Chasma could reach the terminus of the present day valley system in central Chryse Planitia within 44 hours, the original outflow did not traverse the Martian surface in a direct path. It ponded along its course on northern Lunae Planum and near the western edge of Chryse Planitia significantly prolonging the lifetime of surface flow. Calculation of pond volumes and discharge rates through various parts of the channel system indicates that water flowed through this system for nearly a (terrestrial) year. Discharge rates from the various basins along the Maja channels and the maximum flow rates within the various channels are calculated. With this data, it is possible to place reasonable estimates of the minimum length of time required to drain the various impoundments and the duration of flow in various parts of the channel system. The results of these calculations are discussed.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst., Twenty-Third Lunar and Planetary Science Conference; p 15-18
    Format: text
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  • 9
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    Stratigraphy of the south polar region of Ganymede (1987)
    In:  CASI
    Details
    Publication Date: 2013-08-31
    Description: A preliminary assessment is made of the stratigraphy and geology in the south polar region of the Jovian satellite, Ganymede. Geologic mapping is based on inspection of Voyager images and compilation on an airbrush base map at a scale of 1:5M. Illumination and resolution vary greatly in the region. Approximately half of the quadripole is beyond the terminator. Low angle illumination over a large part of the area precludes distinction of some units by albedo characteristics. Several types of grooved terrain and groove related terrain occur in the southern polar region. Grooves typically occur in straight to curvilinear sets or lanes. Bright lanes and grooved lanes intersect at high angles outlining polygons of dark cratered terrain. Groove sets exhibit a range of ages as shown by superposition or truncation and by crater superposition ages.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA, Washington, Reports of Planetary Geology and Geophysics Program, 1986; p 508-510
    Format: application/pdf
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  • 10
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    The Martian sedimentary record (1987)
    In:  CASI
    Details
    Publication Date: 2013-08-29
    Description: The differences between the surface geology of Mars and earth are discussed. Sedimentary processes and fluvial systems on Mars are examined. Surface mapping reveals the more recent depostional patterns. In future missions, radar sounding, active seismic systems, and on site deep drilling may be required to fully document the depositional history. For the present, identification of sedimentary layers must rest on localities of tectonic or erosional windows, detection of buried surfaces by indirect methods, and deposition or off lap patterns of distribution.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst., MEVTV Workshop on Nature and Composition of Surface Units on Mars; p 51-53
    Format: text
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