Physics
Scientific paper
Dec 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufm.p53c1535w&link_type=abstract
American Geophysical Union, Fall Meeting 2010, abstract #P53C-1535
Physics
[5420] Planetary Sciences: Solid Surface Planets / Impact Phenomena, Cratering, [6225] Planetary Sciences: Solar System Objects / Mars
Scientific paper
Recent analytical modeling of impact excavation and ejecta emplacement by Barnhart et al., (this meeting) suggests that near surface spectroscopic detections of clays excavated by impact craters will be most abundant for craters less than 25 km in diameter. We tested this hypothesis by examining 321 CRISM data products (provided by NASA/JHU APL) in the Arabia Terra region. Within those CRISM data products, a total of 21 craters were identified as having a hydroxylated silicates signature in their ejecta and/or crater rims. Of these craters, 17 have signatures in their ejecta, and 4 outlining the crater rim. These craters have an average crater diameter of 8.4 kilometers and range in size of 0.4 to 28.8 kilometers in diameter, corroborating our model's hypothesis. These detections, which cluster near Meridiani Planum, suggest the presence of a buried clay layer the formation of which may have required a large aquifer (Andrews-Hanna et al., 2010) or vast sea (Achille and Hynek, 2010). 21 craters (marked in red) located in the Arabia Terra Region on Mars with a hydroxylated silicates signature in their ejecta and/or crater rims.
Barnhart Charles J.
Moore Jeffery M.
Wilhelm Matthias
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