Impact craters and Venus resurfacing history

Details Impact craters and Venus resurfacing history Impact craters and Venus resurfacing history

Oct 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992jgr....9715923p&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 97, no. E10, p. 15,923-15,948.

Physics

196

Planetary Craters, Planetary Geology, Venus Surface, Meteorite Craters, Planetary Evolution, Tectonics, Volcanology

Scientific paper

The history of resurfacing by tectonism and volcanism on Venus is reconstructed by means of an analysis of Venusian impact crater size-frequency distributions, locations, and preservation states. An atmospheric transit model for meteoroids demonstrates that for craters larger than about 30 km, the size-frequency distribution is close to the atmosphere-free case. An age of cessation of rapid resurfacing of about 500 Ma is obtained. It is inferred that a range of surface ages are recorded by the impact crater population; e.g., the Aphrodite zone is relatively young. An end-member model is developed to quantify resurfacing scenarios. It is argued that Venus has been resurfacing at an average rate of about 1 sq km/yr. Numerical simulations of resurfacing showed that there are two solution branches that satisfy the completely spatially random location restraint for Venusian craters: a is less than 0.0003 (4 deg diameter circle) and a is greater than 0.1 (74 deg diameter circle).

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