Variations in the onset diameter for Martian layered ejecta morphologies and their implications for subsurface volatile reservoirs

Details Variations in the onset diameter for Martian layered ejecta morphologies and their implications for subsurface volatile reservoirs Variations in the onset diameter for Martian layered ejecta morphologies and their implications for subsurface volatile reservoirs

Aug 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001georl..28.3095b&link_type=abstract

Geophysical Research Letters, Volume 28, Issue 16, p. 3095-3098

Physics

24

Planetology: Solid Surface Planets: Impact Phenomena (Includes Cratering), Planetology: Solid Surface Planets: Remote Sensing, Planetology: Solid Surface Planets: Tectonics, Planetology: Solar System Objects: Mars

Scientific paper

We investigated regional variations in the onset diameter of craters displaying a single layer ejecta morphology within +/-30° latitude using Viking imagery. Our results generally agree with those of previous studies which show onset diameters of 5 to 6 km in the equatorial region, but we have identified localized regions with unusually small onset diameters. The largest region is located in Solis and Thaumasia Planae. The 3-5 km onset diameter range in this area indicates a near-surface ice-rich reservoir (depth ~110 m). This unusual concentration of near-surface ice may have resulted from magmatic-driven uplifts associated with the Tharsis rise, which modified parts of a regional aquifer/drainage basin system and resulted in the transfer and concentration of subsurface volatiles in this region.

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