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  • 1
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    Emplacement of multiple flow units on very shallow slopes, east Kawelu Planitia flow field, Venus (1993)
    In:  CASI
    Details
    Publication Date: 2013-08-31
    Description: Lobate flows with variable radar brightness occur at several locations on Venus. Here we present preliminary mapping results for a lava flow field on the eastern side of Kawelu Planitia, centered at approximately 41 deg N, 251 deg E. Numerous individual flows of varying brightness can be traced for up to 400 km at this location. Megallan image F-MIDRP.40N251;1 contains two major flow complexes as well as a distinct minor flow field associated with a volcanic dome. The southern flow field (unit F) changes from radar dark to radar bright in a convex arc from west to east. The flow path is diverted by a ridge system (unit B) and associated N-S faulted zone (unit A) evident in the Magellan altimetry data. The 130-km-long radar-bright flow field located at 41.5 deg N and 249-250 deg E is comprised of a narrow, channeled flow (unit E) overlying an intermediate brightness flow (unit D), all of which appears to emanate from a solitary dome at 249 deg E. The southern lobe of unit E disappears under a broad leveed channel (41.3 deg N, 250.1 deg E) in unit 5, only to reappear south of the unit 5 boundary. The source of this largest flow field is not evident, but could be associated with the region of small domes west of the F-MIDRP image (centered at 41 deg N, 246 deg E). Another possible source is the fractured area south of unit C. The flow complex is clearly a conglomeration of many flow episodes, not necessarily from a single source.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst., Twenty-Fourth Lunar and Planetary Science Conference. Part 2: G-M; p 637-638
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  • 2
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    Geologic mapping of MTM quads 40292 and 40297: In the Utopian lowlands north of the Nilosyrtis Mensae, Mars (1991)
    In:  CASI
    Details
    Publication Date: 2013-08-31
    Description: Geologic mapping at 1:500,000 scale of the Mars transverse Mercator (MTM) quads 40292 and 40297 is being conducted under the auspices of the Mars Geologic Mapping Program. The study area is located in the southwestern portion of Utopia Planitia immediately north of the Nilosyrtis Mensae, between latitudes 37.5 and 42.5 degrees and longitudes 290 and 300 degrees. The goals of the mapping are to identify the major geologic features in the study area and to determine the sequence and scope of the geologic events that have modified the lowland side of the global dichotomy boundary in this region in order to at least partially constrain models of dichotomy boundary origin and evolution. The progress made towards achieving these goals is reported.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA, Washington, Reports of Planetary Geology and Geophysics Program, 1990; p 471-473
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  • 3
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    Thermal properties of channels in the Aeolis Quadrangle: Topographic traps for Aeolian materials (1987)
    In:  CASI
    Details
    Publication Date: 2013-08-31
    Description: Analysis of high spatial resolution (down to 2 to 5 km) thermal data that shows the presence of aeolian debris mantling in topographic traps such as some channels is presented. In cases where this occurs, even if the mantle is thin, it can prevent remote sensing analysis of actual compositional differences that may characterize the true floors of the features.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: MECA Symposium on Mars: Evolution of its Climate and Atmosphere; p 126-128
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  • 4
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    Physical properties of surface materials on Martian volcanoes: Dust-covered lava and ash (1988)
    In:  CASI
    Details
    Publication Date: 2013-08-29
    Description: Remote sensing measurements provide information about the Martian surface at scales smaller than can be inferred from imaging data alone. Measurements of Martian volcanoes obtained at visual, infrared, and radar wavelengths are discussed in order to evaluate the physical properties. A related issue involves identifying possible ash deposits by distinctive or anomalous physical characteristics.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst., NASA MEVTV Program Working Group Meeting: Volcanism on Mars; p 19-21
    Format: text
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  • 5
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    High resolution Viking Orbiter images: A useful data source for testing the viability of geomorphic processes attributed to Martian landforms (1987)
    In:  CASI
    Details
    Publication Date: 2013-08-29
    Description: The diversity of landforms visible in the Viking images of Mars have led to a proliforation of geomorphic agents proposed to be active in shaping the Martian surface. While it is likely that numerous different processes have contributed to the geomorphology of Mars throughout Martian history, it is important that proposed Martian geomorphic agents be subjected to critical scrutiny by the scientific community. High resolution Viking Orbiter images represent a data set for investigating geomorphic processes on Mars. Geologic mapping of Mars can take place at a variety of scales, utilizing a variety of image resolutions, but an interpretation of the history of individual landforms is dependent upon the best available spatial resolution. These high resolution images provide the opportunity to examine proposed Martian geomorphic processes. It is clear that researchers may not interpret features in the same way but it is important that high resolution images of candidate features be made available to the scientific community so that a consensus can be reached. This procedure can provide a way to refine the understanding of geomorphic processes on Mars.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: MEVTV Workshop on Nature and Composition of Surface Units on Mars; p 140-142
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  • 6
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    Preliminary geologic mapping near the Nilosyrtis Mensae, Mars (1990)
    In:  CASI
    Details
    Publication Date: 2013-08-31
    Description: Virtually the entire map area is mantled by an irregular deposit of material that is apparently fine-grained and erodible. It is also extremely young, as there is not a single crater larger than 1 km in the map area that was emplaced atop the mantle. Knobs abound in the study area; many are presumably caused by the mantling of pre-existing topography. In many cases the older knob of the core is exposed. Many such knob cores are surrounded by small scarplets; it is not yet clear whether the scarplets are the eroded edges of mantle beds that at one time draped over the knob core and have been subsequently exposed by erosion, or whether they are eroded versions of lobate debris aprons. Many craters in the study area contain concentric crater fill, which may indicate downslope movement of volatile-rich materials or repeated cycles of aeolian gradation.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Scientific Results of the NASA-Sponsored Study Project on Mars: Evolution of Volcanism, Tectonics, and Volatiles; p 306-307
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  • 7
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    Present imaging limitations to providing a geological assessment of potential sample return sites on Mars (1988)
    In:  CASI
    Details
    Publication Date: 2013-08-31
    Description: A Mars sample return mission will provide a huge increase in knowledge about the region explored by the roving vehicle. However, presently there are some important limitations on the extent to which the geology of a potential site can be understood prior to landing the sample return vehicle on Mars. These limitations could affect not only the potential science return of the mission but also the safety of the vehicle. These limitations are examined.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Workshop on Mars Sample Return Science; p 186-187
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  • 8
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    Scientific results of the NASA-sponsored study project on Mars: Evolution of volcanism, tectonics, and volatiles (1990)
    In:  CASI
    Details
    Publication Date: 2019-06-28
    Description: The objectives of the Mars: Evolution of Volcanism, Tectonics, and Volatiles (MEVTV) project are to outline the volcanic and tectonic history of Mars; to determine the influence of volatiles on Martian volcanic and tectonic processes; and to attempt to determine the compositional, thermal, and volatile history of Mars from its volcanic and tectonic evolution. Available data sets were used to test general models of the volcanic and tectonic history of Mars.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA-CR-188056 , NAS 1.26:188056 , LPI-TR-90-06
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  • 9
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    Comparison of flank modification on Ascraeus and Arsia Montes volcanoes, Mars (1993)
    In:  Other Sources
    Details
    Publication Date: 2019-01-25
    Description: Geologic mapping of the Tharsis Montes on Mars is in progress as part of the Mars Geologic Mapping Program of NASA. Mapping of the southern flanks of Ascraeus Mons at 1:500,000 scale was undertaken first followed by detailed mapping of Arsia Mons; mapping of Pavonis Mons will begin later this year. Results indicate that each of the Tharsis volcanoes displays unique variations on the general 'theme' of a martian shield volcano. Here we concentrate on the flank characteristics on Ascraeus Mons and Arsia Mons, the northernmost and southernmost of the Tharsis Montes, as illustrative of the most prominent trends.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst., Twenty-Fourth Lunar and Planetary Science Conference. Part 3: N-Z; p 1575
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  • 10
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    Numerical simulation of lava flows: Applications to the terrestrial planets (1993)
    In:  Other Sources
    Details
    Publication Date: 2019-01-25
    Description: Lava flows are the visible expression of the extrusion of volcanic materials on a variety of planetary surfaces. A computer program described by Ishihara et al. appears to be well suited for application to different environments, and we have undertaken tests to evaluate their approach. Our results are somewhat mixed; the program does reproduce reasonable lava flow behavior in many situations, but we have encountered some conditions common to planetary environments for which the current program is inadequate. Here we present our initial efforts to identify the 'parameter space' for reasonable numerical simulations of lava flows.
    Keywords: GEOPHYSICS
    Type: Lunar and Planetary Inst., Twenty-Fourth Lunar and Planetary Science Conference. Part 3: N-Z; p 1577-1578
    Format: text
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