Biology
Scientific paper
Oct 1978
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978stin...7913980w&link_type=abstract
Presented at the 9th Ann. Meeting of the Div. for Planetary Sci., Am. Astron. Soc., Boston, 29 Oct. 1977
Biology
Evaporation, Ice, Mars Atmosphere, Mars Surface, Water Vapor, Atmospheric Pressure, Evaporation Rate, Exobiology, Insolation, Melting, Surface Reactions, Turbulent Diffusion
Scientific paper
The evaporation rate of water ice on the surface of a planet with an atmosphere involves an equilibrium between solar heating and radiative and evaporative cooling of the ice layer. The thickness of the ice is governed principally by the solar flux which penetrates the ice layer and then is conducted back to the surface. Evaporation from the surface is governed by wind and free convection. In the absence of wind, eddy diffusion is caused by the lower density of water vapor in comparison to the density of the Martian atmosphere. For mean martian insolations, the evaporation rate above the ice is approximately 10 to the minus 8th power gm/sq cm/s. Evaporation rates are calculated for a wide range of frictional velocities, atmospheric pressures, and insolations and it seems clear that at least some subset of observed Martian channels may have formed as ice-chocked rivers. Typical equilibrium thicknesses of such ice covers are approximately 10m to 30 m; typical surface temperatures are 210 to 235 K.
Sagan Carl
Wallace David
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