The Infrared Signature of Martian Polar Clouds

Details The Infrared Signature of Martian Polar Clouds The Infrared Signature of Martian Polar Clouds

Nov 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001dps....33.3409f&link_type=abstract

American Astronomical Society, DPS Meeting #33, #34.09; Bulletin of the American Astronomical Society, Vol. 33, p.1099

Astronomy and Astrophysics

Astronomy

Scientific paper

CO2 clouds in the Martian polar night have been monitored by the Mars Global Surveyor (MGS) Laser Altimeter experiment (MOLA) and used to derive a catalog of cloud locations and morphologies that spans the period from March 1998 to July 2001. For much of that time, the MGS Thermal Emission Spectrometer experiment (TES) viewed Mars from the same nadir direction as MOLA at wavelengths between 5.8 and 67μ m. Following the method first adopted by Kieffer et al., polar TES measurements have been interpolated to 15, 18, and 25μ m wavelengths, representing emission dominated, respectively, by an atmospheric region at about 20+/-5 km altitude; by the lowest scale height above the Martian surface; and by the surface itself. The MOLA cloud catalog has been combined with TES data to create polar maps of emission temperature when MOLA clouds were not observed, at intervals of 10o in Ls, and at each of the three chosen TES wavelengths. The cloud catalog was used again to determine emission temperatures at those times when MOLA and, by inference, TES, were observing CO2 clouds. The average temperature difference between the times when clouds were present and absent is significant at 18 and 25μ m, but not noticeable at 15μ m.

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