Abstract
Meteoritic bombardment of the lunar surface results in an erosion process that tends to soften the topography. A simplified mathematical model illustrating the erosion of lunar craters is presented. The model takes into consideration the angular distribution of impacting meteorites and ejecta and the topography and mechanical properties of the lunar surface. Calculations indicate that craters 1, 10, and 100 meters in diameter disappear almost completely after 107, 108, and 109 years, respectively. The results of this study suggest that the minimum depth of debris in the maria is a few meters. Processes other than erosion due to small meteoritic masses, such as volcanic activity, isostatic compensation, and the infrequent impact of a large meteoroid, would be necessary to significantly modify the relief of craters larger than a kilometer in diameter.
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