Impact-Induced Melting of Near-Surface Water Ice on Mars

Details Impact-Induced Melting of Near-Surface Water Ice on Mars Impact-Induced Melting of Near-Surface Water Ice on Mars

Jul 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aipc..706.1484s&link_type=abstract

SHOCK COMPRESSION OF CONDENSED MATTER - 2003: Proceedings of the Conference of the American Physical Society Topical Group on Sh

Physics

Condensed Matter

5

Mars, High-Pressure And Shock Wave Effects In Solids And Liquids, Shock Wave Interactions And Shock Effects

Scientific paper

All fresh and many older Martian craters with diameters greater than a few km are surrounded by ejecta blankets which appear fluidized, with morphologies believed to form by entrainment of liquid water. We present cratering simulations investigating the outcome of 10 km s-1 impacts onto models of the Martian crust, a mixture of basalt and ice at an average temperature of 200 K. Because of the strong impedance mismatch between basalt and ice, the peak shock pressure and the pressure decay profiles are sensitive to the mixture composition of the surface. For typical impact events, about 50% of the excavated ground ice is melted by the impact-induced shock. Pre-existing subsurface liquid water is not required to form observed fluidized ejecta morphologies, and the presence of rampart craters on different age terranes is a useful probe of ground ice on Mars over time.

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