Mathematics – Logic
Scientific paper
Sep 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996dps....28.0209b&link_type=abstract
American Astronomical Society, DPS meeting #28, #02.09; Bulletin of the American Astronomical Society, Vol. 28, p.1059
Mathematics
Logic
Scientific paper
We suggest that fluidization of martian ejecta is caused by the combined effects of abundant liquid water in the target materials and the high radial velocity of ejecta to produce extremely mobile debris/mud-like flows deposits. Because this process requires liquid water, these craters are a powerful tool that provides information about the paleo-location of subsurface water on Mars. As a result, the distribution of these craters suggests a global aquifer at a depth of several hundred meters to several kilometers over much, if not all, of Mars history. Fluidized ejecta has been attributed to the effects of (1) the thin martian atmosphere, or (2) volatiles in the target materials (water or water ice). Experimental crater studies have produced inconclusive results in resolving this controversy. Small-scale (cm) impact experiments performed on fine-grained dry materials in an atmosphere and water-saturated target materials have both produced fluidized ejecta. Explosion experiments performed on wet targets have also produced fluidized ejecta, but none have developed the characteristic distal rampart. Observational data suggests that the Mars atmosphere plays no significant role in fluidization of ejecta. The presence of an atmosphere should affect only the ejecta emplacement processes. Whereas, volatiles in the target materials should affect both crater and ejecta processes. Martian crater studies show a correlation between ejecta types, interior morphology, and associated size frequency distribution. This is consistent with effects of abundant volatiles in the crust, but ruling out atmospheric influences. In addition, calculational studies predict that shock melting of subsurface ice also cannot account for ejecta fluidization. These studies indicate that most martian ejecta are subjected to shock pressures too low (10 GPa) to melt ice. Observational data of ejecta on icy bodies (e.g., Ganymede) support these calculations. Ejecta on these bodies is morphologically similar to lunar ejecta, but not to martian fluidized ejecta.
Boyce Joseph M.
Craddock R.
Roddy David J.
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