Impact crater degradation on venusian plains

Details Impact crater degradation on venusian plains Impact crater degradation on venusian plains

Feb 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994georl..21..289i&link_type=abstract

Geophysical Research Letters, vol. 21, no. 4, p. 289-292

Physics

27

Backscattering, Computerized Simulation, Degradation, Ejecta, Erosion, Meteorite Craters, Monte Carlo Method, Planetary Craters, Radar Imagery, Tectonics, Venus (Planet), Venus Surface, Volcanoes, Weathering, Fracturing, Graphs (Charts), Radar Signatures, Rates (Per Time), Remote Sensing, Steady State, Tables (Data), Venus, Impact Craters, Plains, Backscatter, Morphology, Comparison, Ejecta, Volcanism, Crater Floor, Fractures, Eolian Effects, Deposits, Weathering, Tectonism, Monte Carlo Method, Simulation,

Scientific paper

In venusian plains, impact craters without extensive low backscatter ejecta deposits are more likely to have low backscatter floors, be embayed by volcanic deposits, and exhibit fractures as compared to craters with extensive low backscatter ejecta. We interpret these trends as evidence of ongoing degradation of low backscatter ejecta by aeolian activity, weathering, and volcanism. Using a crater age sequence based on extent of preservation of low backscatter ejecta, together with Monte Carlo simulations, we find that tectonic activity has extended over a longer time period than volcanism.

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