A sublimation model for martian south polar ice features.
In their pioneering work, Leighton and Murray argued that the Mars atmosphere, which at present is 95% carbon dioxide, is controlled by vapor equilibrium with a much larger polar reservoir of solid carbon dioxide. Here we argue that the polar reservoir is small and cannot function as a long-term buffer to the more massive atmosphere. Our work is based on modeling of the circular depressions commonly found on the south polar cap. We argue that a carbon dioxide ice layer about 8 meters thick is being etched away to reveal water ice underneath. This is consistent with thermal infrared data from the Mars Odyssey mission.
Byrne
Shane
S
Division of Geological and Planetary Sciences, California Institute of Technology, 1200 East California Boulevard, Pasadena, CA 91125, USA.
Ingersoll
Andrew P
AP
D001272:Atmosphere; D002245:Carbon Dioxide; D004367:Dry Ice; D007053:Ice; D018535:Mars; D008962:Models, Theoretical; D012621:Seasons; D013696:Temperature; D014867:Water
D004367:Dry Ice; D007053:Ice; D014867:Water; D002245:Carbon Dioxide