Mathematics – Logic
Scientific paper
Dec 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufm.p72c..02k&link_type=abstract
American Geophysical Union, Fall Meeting 2002, abstract #P72C-02
Mathematics
Logic
5416 Glaciation, 5462 Polar Regions, 5470 Surface Materials And Properties, 6020 Ice, 6225 Mars
Scientific paper
H2O is directly observed on Mars in the vapor state and as a solid in clouds, surface frosts, and as the permanent North polar cap. Liquid H2O is not stable at the surface of Mars under current conditions. However, first-order stability of the solid requires only that the mean annual saturation pressure, derived from the physical temperature, be below the mean annual H2O vapor pressure; this condition occurs widely on Mars, and there has been a general expectation of abundant ice in the soil/regolith. Odyssey GRS observations suggest extensive water-ice, beneath about 400 kg/m2 of soil, around the south pole. Although water ice is prominent and abundant near the North pole, until recently (this conference) water ice had not been observed at the surface in the south polar region; new thermal observations indicate dirty water-ice is directly exposed in isolated locations there. Water ice is expected to accumulate in the seasonal CO2 cap, but the amounts are on the order of 0.1 kg/m2 and are expected to sublime in less than a sol after the disappearance of solid CO2. Transient brightenings have been observed on or near the summer north polar cap, and off the edge of the winter seasonal cap at the Viking II site, all at temperatures too high for CO2. These are consistent over years in their general region, but vary in detail between years. Specific areas well away from the perennial cap show late-summer brightness and temperature behavior suggesting solid ice immediately (cm) below the surface. Comparison of diurnal and annual temperature variations suggest permafrost surrounds the north polar cap. There are countless inferences of the presence of water-ice in the indeterminent present or past on geomorphological grounds. Water is probably common as interstital ice or with relatively minor fractions of dirt over much of Mars. Precise locations and depths will become increasing well known as exploration techniques improve.
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