Overview of Venus geology: Preliminary description of terrain units for Venus global geological mapping

Details Overview of Venus geology: Preliminary description of terrain units for Venus global geological mapping Overview of Venus geology: Preliminary description of terrain units for Venus global geological mapping

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992lpico.789...99s&link_type=abstract

In Lunar and Planetary Inst., Papers Presented to the International Colloquium on Venus p 99 (SEE N93-14288 04-91)

Mathematics

Logic

Emissivity, Geological Surveys, Geomorphology, Planetary Geology, Planetary Mapping, Surface Roughness, Terrain, Venus (Planet), Venus Surface, Backscattering, Craters, General Overviews, Mosaics, Reflectance, Tectonics, Thematic Mapping, Volcanoes

Scientific paper

Venus terrain units can be categorized on the basis of morphology, reflectivity, backscatter, roughness, and emissivity. Morphology can be inferred from Magellan left-looking nominal incidence angle image mosaics, right-looking coverage, and more limited left-looking stereo. The typical resolution is about 300 m down to about 120 m near periapsis in the cycle one nominal coverage. The scale of geologic mapping governs definition of mappable terrain units. Initial global mapping is being compiled at a scale of 1:50 million. At this scale, the smallest individual features that can be mapped are about 125 km. The categories of terrain types are plains, complex ridge terrain, features with morphology suggesting volcanic or volcano-tectonic origin, features interpreted to be tectonic in origin, crater units, and surficial units such as splotches and streaks. Brief descriptions of terrain units are provided.

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