Other
Scientific paper
Dec 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000dps....32.6506h&link_type=abstract
American Astronomical Society, DPS Meeting #32, #65.06; Bulletin of the American Astronomical Society, Vol. 32, p.1640
Other
Scientific paper
Freezing, evaporation, and melting rates for surface water on Mars have been revisited in the context of short-term or seasonal flow in small channels. In the sparse martian atmosphere, convective cooling or heating is insignificant compared to other heat transfer mechanisms on Mars or compared to convective losses on Earth. It follows that atmospheric temperature is inconsequential to freezing or melting except when it falls below the frostpoint. As a result of the cold martian sky and other exposed surfaces, radiative losses on Mars are several times those experienced on Earth, although still small compared to evaporative cooling. Aside from conductive cooling from a cold stream bed, latent heat of vaporization (i.e. evaporative cooling) is the dominant cause of freezing on Mars. Evaporation per se does not remove significant amounts of water from the reservoir compared to freezing resulting from the corresponding heat loss. In agreement with previous work, the residence time of either free, running water or pooled water (crusted with ice) is found to be comparable to that of water or ice on Earth. Moreover, circumstances can be described in which freezing is nearly completely suppressed and extensive melting will occur, even under a very cold atmosphere. Experimental measurements of the dependence of evaporation rate on atmospheric pressure are presented, apparently for the first time. Prior theories suggested a power law dependence on pressure, but disagreed on the exponent. A scenario for local atmospheric circulation of water vapor is described that would explain occasional or seasonal flow from cold, pole-facing peaks.
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