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Variations in the onset diameter for Martian layered ejecta morphologies and their implications for subsurface volatile reservoirs
Author(s) -
Barlow Nadine G.,
Koroshetz John,
Dohm James M.
Publication year - 2001
Publication title -
geophysical research letters
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.007
H-Index - 273
eISSN - 1944-8007
pISSN - 0094-8276
DOI - 10.1029/2000gl012804
Subject(s) - ejecta , geology , impact crater , tharsis , martian , aquifer , regolith , latitude , mars exploration program , geomorphology , geochemistry , astrobiology , groundwater , physics , geotechnical engineering , geodesy , quantum mechanics , supernova
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.