Atmospheric and surface retrievals in the Mars polar regions from the Thermal Emission Spectrometer measurements

Details Atmospheric and surface retrievals in the Mars polar regions from the Thermal Emission Spectrometer measurements Atmospheric and surface retrievals in the Mars polar regions from the Thermal Emission Spectrometer measurements

Oct 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008jgre..11310010e&link_type=abstract

Journal of Geophysical Research, Volume 113, Issue E10, CiteID E10010

Physics

2

Planetary Sciences: Solar System Objects: Mars, Planetary Sciences: Solid Surface Planets: Polar Regions, Planetary Sciences: Solid Surface Planets: Atmospheres (0343, 1060), Planetary Sciences: Solid Surface Planets: Ices, Planetary Sciences: Solid Surface Planets: Remote Sensing

Scientific paper

Retrievals of atmospheric temperatures, surface emissivities, and dust opacities in the Mars polar regions from the Thermal Emission Spectrometer (TES) spectra are presented. The retrievals correspond to two types of spectra, characterized by small and large band depths BD25 in the 25-μm band of solid CO2. These two types of spectra have previously been identified with locations covered by slab ice and fluffy CO2 frost, respectively. Above the first atmospheric scale height, there is a correlation between the degree of saturation in the retrieved atmospheric temperatures and the two types of surface, with the high BD25 spectra (``cold spots'') showing larger supersaturations around 1 mbar. This supports the hypothesis that cold spots correspond to locations with potential or actual atmospheric precipitation. Furthermore, the retrieved temperature profiles exhitbit a warming above 1 mbar (15 km), which appears real even when the limited number of independent pieces of information from the measurement (~3) and coarse vertical resolution of the TES instrument above 15 km are considered. The spectral shape of the retrieved surface emissivities in the cold spot locations is consistent with modeling results attributing high BD25 to porosity. For the low BD25 spectra, the retrieved emissivities are spectrally flat but significantly less than unity (0.8-0.9). The cause of these spectrally uniform deviations from blackbody behavior (which are not supported by modeling) remains to be investigated, with a noticeable reduction in the deviation from the blackbody behavior achieved through a zero-radiance-level correction to the TES spectra available from the Planetary Data System.

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