Physics
Scientific paper
Jan 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998lpico.953q..11f&link_type=abstract
The First International Conference on Mars Polar Science and Exploration, Proceedings of the Conference held at Camp Allen, TX.
Physics
Carbon Dioxide, Mars Surface, Polar Caps, Ice, Dust, Snow, Ice Formation, Infrared Radiation, Thermal Mapping, Mars Global Surveyor
Scientific paper
One of the key processes controlling the geology of the martian polar regions is the seasonal condensation of the atmosphere into CO2 ice caps. These polar caps mostly condense during the polar night, when surface and atmospheric temperature become cold enough to reach the frost point of CO2. Thus, almost all that is known about the formation of the polar caps has come from the Mariner 9 and Viking infrared measurements. These observations showed that the physical processes controlling the condensation are complex, because of the unique radiative and microphysical properties Of CO2 ice condensing in a CO2 atmosphere. For instance, the Infrared Thermal Mapper (IRTM). One of the key processes controlling the geology of the martian polar regions is the seasonal condensation of the atmosphere into CO2 ice caps. These polar caps mostly condense during the polar night, when surface and atmospheric temperature become cold enough to reach the frost point of CO2. Thus, almost all that is known about the formation of the polar caps has come from the Mariner 9 and Viking infrared measurements. These observations showed that the physical processes controlling the condensation are complex, because of the unique radiative and microphysical properties Of CO2 ice condensing in a CO2 atmosphere. For instance, the IRTM instrument observed variable structures exhibiting brightness temperatures far below the physical temperature appropriate for condensed CO, in vapor pressure equilibrium at the expected atmospheric pressure. A detailed analysis of the data suggests that these low brightness temperatures result from the radiative properties of the SMO CO2 ice particles that condense in the atmosphere rather than directly on the surface New observations are being transmitted by Mars Global Surveyor. TES and MOLA data should greatly improve our understand- ing of what is really going on during the cap formation. instrument observed variable structures exhibiting brightness temperatures far below the physical temperature appropriate for condensed CO2 in vapor pressure equilibrium at the expected atmospheric pressure. A detailed analysis of the data suggests that these low brightness temperatures result from the radiative properties of the small CO2 ice particles that condense in the atmosphere rather than directly on the surface New observations are being transmitted by Mars Global Surveyor. TES and MOLA data should greatly improve our understanding of what is really going on during the cap formation.
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