Mathematics – Logic
Scientific paper
Dec 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufm.p53f..01s&link_type=abstract
American Geophysical Union, Fall Meeting 2010, abstract #P53F-01
Mathematics
Logic
[5416] Planetary Sciences: Solid Surface Planets / Glaciation, [5422] Planetary Sciences: Solid Surface Planets / Ices, [5445] Planetary Sciences: Solid Surface Planets / Meteorology, [6225] Planetary Sciences: Solar System Objects / Mars
Scientific paper
The floors and walls of many mid-latitude (~30-60°) craters on Mars appear to be mantled by relatively young material(s) with distinct morphology and erosional properties [1,2]. Collectively, this material (“fill”) is often interpreted as ice-rich, with emplacement and modification related to climatically controlled/induced processes [1,3]. Here, I document material and associated landforms within 38 craters between ~4-12°S and ~335-355°W in the Sinus Sabaeus region (south of Schiaparelli Crater) that appear morphologically similar to material and landforms within mid-latitude craters. The morphological similarities between the equatorial and mid-latitude fill material suggest that they potentially share a similar composition, are subjected to similar erosional processes, and share a similar emplacement mechanism. Nearly all craters containing fill material in Sinus Sabaeus are ~2.0-9.0 km in diameter (median 5.3 km) and they tend to be relatively young with steep interior wall slopes of ~15-30°. At least 30 additional craters in the region display evidence suggestive of past fill presence. A survey of available Mars Reconnaissance Orbiter Context Camera (CTX) data at equatorial latitudes did not identify this material or evidence for its former presence within any other equatorial craters. Near-surface ice is unstable at equatorial latitudes under present conditions, suggesting that emplacement could have occurred under different climate conditions in the past. High-obliquity (35-45°) general circulation model simulations [4] show surface ice accumulation in Sinus Sabaeus and Tharsis, where similar material and landforms have been documented within steep-walled depressions and troughs [5]. The documentation of this material in Sinus Sabaeus is consistent with the hypothesis that past obliquity-driven climate change resulted in equatorward volatile migration on Mars. This fill material is >80-100 m thick in some craters. It is unclear from available data whether any relict ice is currently present at these locations, although the equatorial setting suggests that if present, this ice is likely buried by a thick, insulating debris layer or a near-surface layer of reduced permeability. References: [1] Squyres, S.W. and M.H. Carr, Science, 231, 249-252, 1986. [2] Shean, D.E., LPSC 41, 1509, 2010. [3] Head, J.W. et al., EPSL, 294, 306-320, 2010. [4] Levrard, B. et al., Nature, 431, 1072-1075, 2004. [5] Shean, D.E. et al., JGR, E03004, 2007.
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