The dust scale height of the Martian atmosphere in Vallis Marineris from HRSC stereo images

Details The dust scale height of the Martian atmosphere in Vallis Marineris from HRSC stereo images The dust scale height of the Martian atmosphere in Vallis Marineris from HRSC stereo images

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005dps....37.3336h&link_type=abstract

American Astronomical Society, DPS meeting #37, #33.36; Bulletin of the American Astronomical Society, Vol. 37, p.1567

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Scientific paper

The Martian atmosphere contains large and variable amounts of dust and other aerosols. The High Resolution Stereo Camera (HRSC) onboard the European orbiter Mars Express is a powerful tool for studying the distribution of dust in Mars' atmosphere. An essential parameter for such studies is the optical depth, which can often be estimated from contrast differences between HRSC stereo images with the so called `stereo method'. Software for this purpose has been developed at the MPS in Lindau Germany. The method uses map-projected ortho-images and complementary data on the imaging geometry from photogrammetric software developed at DLR.
On June 3, 2004, during orbit 471 of Mars Express, HRSC imaged regions in and around Vallis Marineris in stereo; these span height differences of more than 10 km. Obviously, the amount of dust in the Martian atmosphere varies with altitude. We used the images to study how optical depth depends on altitude. We used the Southern wall of the Vallis to estimate the atmospheric dust scale-height and found 13 km plus or minus 1 km. Independent of altitude, the measured optical depths show important (up to about a factor of two) local variations on horizontal scales of a few tens of kilometers, that may well be related to winds and obstacles like crater walls and mountains.

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