Venus impact craters: Implications for atmospheric and resurfacing processes from Magellan observations

Details Venus impact craters: Implications for atmospheric and resurfacing processes from Magellan observations Venus impact craters: Implications for atmospheric and resurfacing processes from Magellan observations

Jun 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991pggp.rept..334p&link_type=abstract

In NASA, Washington, Reports of Planetary Geology and Geophysics Program, 1990 p 334-335 (SEE N92-10728 01-91)

Physics

Geophysics

Atmospheric Effects, Ejecta, Magellan Spacecraft (Nasa), Meteorite Craters, Planetary Evolution, Venus Surface, Backscattering, Geochronology, Radar Data, Radar Scattering, Scattering Cross Sections, Venus (Planet)

Scientific paper

Observations of impact craters on Venus by Magellan yield important insights into: (1) atmospheric effects on the formation of impact craters and their attendant ejecta deposits and (2) the resurfacing history of the planet. Most craters smaller than 15 km are classified as irregular; they possess irregularly shaped rims, and multiple hummocky floors. The irregular nature of these craters is interpreted to be the consequence of breakup and dispersion of incoming meteoroids by the dense atmosphere. Two major ejecta facies of venusian impact craters are hummocky ejecta and outer ejecta. A number of craters documented in the Magellan images possess often non-radial, flow-like ejecta indicative of a low viscosity materials. Approximately half of the impact craters observed with the Magellan radar are partially or wholly surrounded by areas with low radar backscatter cross sections.

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