Implications for Venusian plains resurfacing from geomorphic mapping and impact crater densities

Details Implications for Venusian plains resurfacing from geomorphic mapping and impact crater densities Implications for Venusian plains resurfacing from geomorphic mapping and impact crater densities

Mar 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997lpi....28..527h&link_type=abstract

Conference Paper, 28th Annual Lunar and Planetary Science Conference, p. 527.

Astronomy and Astrophysics

Astrophysics

1

Planetary Craters, Hypervelocity Impact, Venus Surface, Plains, Geomorphology, Chronology, Synthetic Aperture Radar

Scientific paper

Two main lines of evidence are most often cited when describing a possible mechanism for Venusian resurfacing. First and most importantly, the impact crater distribution cannot be distinguished from one that is completely spatially random. Second, there is a dearth of volcanically embayed craters on the surface. These two observations have been the linchpin of an accepted paradigm in Venusian resurfacing, the catastrophic resurfacing model. The catastrophic model implies a rapid, large scale lava flooding and tectonic event, which would have erased all evidence of earlier craters, followed by the cessation, or at least rapid waning, of resurfacing activity on Venus. Original thinking on the catastrophic hypothesis suggested that the resurfacing tailed off in about 10 Myr. New work suggests this period may have lasted as long as 100 Myr. While this conclusion is by far the most simple, it is certainly not a unique interpretation of the evidence. Alternatives are discussed.

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