CO2 permafrost and Martian topography

Details CO2 permafrost and Martian topography CO2 permafrost and Martian topography

Jun 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978icar...34..568l&link_type=abstract

Icarus, vol. 34, June 1978, p. 568-580. Research supported by the University of Alberta.

Physics

7

Carbon Dioxide, Mars Surface, Permafrost, Topography, Erosion, Phase Transformations, Planetary Evolution, Water, Mariner 9, Viking 2 Lander, Erosional Agents, Viking 1 Lander, Coprates, Chasma, Water, Erosion, Ice, Clathrate, Mars, Topography, Evolution, Carbon Dioxide, Permafrost, Regolith

Scientific paper

The role of CO2 permafrost as an erosive agent on Mars is considered. In the CO2-H2O system, with a CO2 triple point at 217 K and 5.1-bar pressure, carbon dioxide solid, liquid, or gas, CO2 clathrate, and ice are possible stable phases in the range of temperatures and pressures likely to be encountered in the Martian regolith. It is argued that conditions may exist in which CO2 permafrost is extensive on Mars, provided that adequate CO2 is available: the maximum ratio of H2O:CO2 required in the subsurface pore space system is 17:3. Erosional processes likely to result from such permafrost are block slumping, leading to canyon development; pit chains along faults; chaotic terrain where massive permafrost destruction has occurred; large-scale flows of slurry; and perhaps even the flash floods which create channels.

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