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Applicant -- Planetary Microclimates: From permanently shadowed regions on Ceres to Martian alcoves

Wednesday, September 21, 2016

Topographically induced temperature extremes often play a defining role for the presence of volatiles. On Ceres, permanently shadowed regions harbor bright water ice deposits. On the Moon, small cold traps may have preserved volatiles that are more easily accessible by rovers than those in large cold traps. And on Mars, the alcoves of gullies and Recurring Slope Lineae create conditions for the formation of dry ice or liquid water. We use models to address each of these phenomena that yield an increasingly better understanding of cold-trapping in the Mercury-Moon-Ceres continuum and the cause of seasonal mass wasting on Mars.

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