Possible lifetime of impact craters on Martian eolian landforms

Details Possible lifetime of impact craters on Martian eolian landforms Possible lifetime of impact craters on Martian eolian landforms

Mar 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997lpi....28..867m&link_type=abstract

Conference Paper, 28th Annual Lunar and Planetary Science Conference, p. 867.

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Hypervelocity Impact, Craters, Mars Surface, Landforms, Calibrating, Lunar Environment

Scientific paper

Density of impact craters on planetary surfaces is a result of two competing processes: crater formation and crater destruction. In previous work, we determined crater densities on various eolian landforms of Mars and compared them with crater densities in the adjacent areas with no or rare obvious eolian landforms. Using crater statistics and a calibration curve, we determined absolute model surface ages of the studied areas assuming that the studied crater populations were the production ones that implied strong predominance of crater formation over the crater destruction. Typically crater densities on the eolian landforms are significantly lower than in the adjacent areas, indicating a lower age for the eolian landforms. The size-frequency distribution of smaller sized craters even with diameters of hundreds of meters deviates often from the standard calibration curve with the typical production slope. This leads to the second possible end-member option for smaller craters: crater populations in the studied areas are the steady-state ones; an equilibrium between crater formation and crater destruction has been reached. This option seems wrong for areas with no or rare eolian landforms, but right for those with abundant eolian landforms. We consider the second option for the studied areas of Mars, creating a theoretical model of this case and comparing the model with observations.

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