Optical depth and its scale-height in Valles Marineris from HRSC stereo images

Details Optical depth and its scale-height in Valles Marineris from HRSC stereo images Optical depth and its scale-height in Valles Marineris from HRSC stereo images

Jun 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010e%26psl.294..534h&link_type=abstract

Earth and Planetary Science Letters, Volume 294, Issue 3-4, p. 534-540.

Physics

2

Scientific paper

We measured the optical depth of the Martian atmosphere as a function of altitude above two opposing scree walls of the Valles Marineris, from stereo images that were taken with the High Resolution Stereo Camera (HRSC) of Mars Express on June 3, 2004, during orbit 471. The optical depths were measured from contrast differences between the stereo images with the so called “stereo method”. For 7 regions in the northern wall of the Valles, we estimated the optical depth and found values between 1.0 and 1.6. These regions span more than 6 km in altitude and the results show a clear relation with altitude. A fit on these results yielded a scale-height for the optical depth of 14.0 km + 1.3/-1.1 km. The expected local pressure-scale height is smaller: 11.5-12.0 km. The difference is most likely explained by small (around 1.5%) offset errors in the intensity calibration of HRSC images. We also selected 9 regions in the opposing southern wall and from these we measured values of optical depth in the range 1.3-1.5. Our result suggests the presence of clouds above this part of the Valles because the optical depth appears almost independent of the surface altitude. Possibly these are banner clouds, forming at the edge of the canyon, that contain dust that is blown over the canyon by winds from the high plains to the South.

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