Impact craters on Venus - Initial analysis from Magellan

Details Impact craters on Venus - Initial analysis from Magellan Impact craters on Venus - Initial analysis from Magellan

Apr 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991sci...252..288p&link_type=abstract

Science (ISSN 0036-8075), vol. 252, April 12, 1991, p. 288-297. Research supported by JPL and NERC.

Mathematics

Logic

95

Magellan Project (Nasa), Meteorite Craters, Planetary Craters, Planetary Geology, Planetology, Venus Surface, Ejecta, Radar Maps, Volcanoes, Venus, Craters, Impact Craters, Surface, Features, Magellan Mission, Spacecraft Observations, Sar Instrument, Origin, Formation, Cratering, Size, Description, Crater Peaks, Crater Rings, Meteoriods, Atmosphere, Ejecta, Distance, Albedo, Shock Effects, Sappho Patera, Volcanism, Distribution, Resurfacing, Age, Morphology, Physical Properties, Hypotheses, Production Rate,

Scientific paper

The general features of impact craters are described emphasizing two aspects: the effect of the atmosphere on crater and ejecta morphology and the implications of the distribution and appearance of the craters for the volcanic and tectonic resurfacing history of Venus. Magellan radar images reveal 135 craters about 15 km in diameter containing central peaks, multiple central peaks, and peak rings. Craters smaller than 15 km exhibit multiple floors or appear in clusters. Surface flows of material initially entrained in the atmosphere are characterized. Zones of low radar albedo originated from deformation of the surface by the shock or pressure wave associated with the incoming meteoroid surround many craters. A spectrum of surface ages on Venus ranging from 0 to 800 million years indicates that Venus must be a geologically active planet.

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