The Dust Scale Height Of The Martian Atmosphere Around Pavonis Mons From Hrsc Stereo Images

Details The Dust Scale Height Of The Martian Atmosphere Around Pavonis Mons From Hrsc Stereo Images The Dust Scale Height Of The Martian Atmosphere Around Pavonis Mons From Hrsc Stereo Images

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dps....38.6030h&link_type=abstract

American Astronomical Society, DPS meeting #38, #60.30

Astronomy and Astrophysics

Astronomy

Scientific paper

The Martian atmosphere contains large and variable amounts of aerosols, mainly consisting of airborne dust. 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 August 17, 2005, during orbit 902 of Mars Express, HRSC imaged Pavonis Mons and regions around it in stereo; these span height differences of over 10 km. Obviously, the amount of dust in the Martian atmosphere varies with elevation. We used the images to study how optical depth depends on altitude. This yielded a scale-height of 10.8 km within an one sigma range of 10.0_11.7 km. Independent of altitude, the measured optical depths showed very strong local variations due to localized clouds.

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