Other
Scientific paper
Apr 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003eaeja.....7259h&link_type=abstract
EGS - AGU - EUG Joint Assembly, Abstracts from the meeting held in Nice, France, 6 - 11 April 2003, abstract #7259
Other
Scientific paper
Rock glaciers form on earth when sublimation concentrates debris on the surface of active glaciers. Continued flow of the underlying glacier through internal deformation produces ridges and lobes of sublimation till on top of the glacier. Debris thickness increases downslope and spoon-shaped proximal depressions commonly form at rock glacier heads when sublimation exceeds accumulation, as in the case of changing climatic conditions. We have found evidence for rock glacier deposits in several environments on Mars: 1) on volcanic mountain flanks (Tharsis Montes) in equatorial regions; 2) in crater interiors at specific latitudes and orientations; 3) in association with impact basin rims and interiors; and 4) in several other environments. We assess the morphology of these deposits to infer initial conditions, to examine evidence for snow accumulation patterns in past martian history, and to address the most likely locations of preserved ice and atmospheric samples from past martian history.
Head James W.
Marchant David R.
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