Polar Cap Formation and Evolution of Martian Atmosphere

Details Polar Cap Formation and Evolution of Martian Atmosphere Polar Cap Formation and Evolution of Martian Atmosphere

Aug 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000mpse.conf..184y&link_type=abstract

International Conference on Mars Polar Science and Exploration, p. 184

Mathematics

Logic

Mars (Planet), Mars Surface, Mars Environment, Polar Caps, Climate Models, Water, Atmospheric Circulation, Radiation Effects, Greenhouse Effect, Carbon Dioxide

Scientific paper

Several lines of geological evidence strongly suggest that H2O was once distributed globally over the Martian surface. At present, however, the surface H2O is observed only at the polar caps. Under what climate conditions did H2O gather to the polar caps? To shed light on this question, we construct a climate model including atmospheric transport processes of H2O to polar cap. Among the studies on Martian climate, widely accepted one is Gierasch and Toon (1973) (G&T). They suggested that the Martian atmospheric pressure is determined by the CO2 vapor pressure on the polar cap because CO2, the main atmospheric component, can condense onto the polar cap. In order to test this idea, they estimated the polar surface temperature by using a simple energy balance model which includes the effect of radiation, heat advection between polar surface and atmosphere, and that between equatorial and polar atmospheres. Assuming the vapor pressure equilibrium between the CO2 polar cap and the atmosphere, this model can reproduce the present atmospheric pressure as a stable solution. However, the G&T model has several problems. They assumed the equatorial temperature to be constant. In fact, the equatorial temperature should be determined by the energy balance. Furthermore, seasonal variation of the polar temperature is neglected. In addition, greenhouse effect is not taken into account. Additional information is contained in the original extended abstract.

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