Mathematics – Logic
Scientific paper
Dec 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmep43c0763m&link_type=abstract
American Geophysical Union, Fall Meeting 2010, abstract #EP43C-0763
Mathematics
Logic
[0722] Cryosphere / Rock Glaciers, [1616] Global Change / Climate Variability, [5416] Planetary Sciences: Solid Surface Planets / Glaciation, [6225] Planetary Sciences: Solar System Objects / Mars
Scientific paper
We describe the geomorphic record preserved within the highly degraded 80 km diameter Asimov impact crater located within Noachis Terra. The crater has been significantly in-filled since its formation in the Noachian, presumably by sedimentary materials similar to units identified elsewhere in Noachian aged craters. In this case the fill is unusual in that there is an annulus of disconnected valleys adjacent to the interior flanks of the crater wall. High-resolution images reveal that Hesperian-aged layered basalt with distinctive columnar jointing caps the interior crater fill and provides a source of debris that via mass wasting, accumulates in the surrounding annular valleys. Models for the formation of the valleys need to account for the removal of large volumes of crater fill material from below the basaltic cap. One distinct possibility is that the fill material originally contained high proportions of volatiles that have since been lost to the atmosphere. We explore this model and others and investigate the surrounding regions to place further constraints on valley formation. The occurrence of steep slopes (>20 °), relatively narrow (sheltered) valleys, and a source of debris have provided favorable conditions for the preservation of late Amazonian shallow-ice deposits. Detailed mapping reveals morphological evidence for viscous ice flow, in the form of several lobate debris tongues (LDT). Superimposed on LDT are a series of fresh-appearing gullies, with typical alcove, channel, and fan morphologies. The shift from ice-rich viscous-flow formation to gully erosion is best explained as a shift in martian climate, from one compatible with excess snowfall and flow of ice-rich deposits, to one consistent with minor snowfall and gully formation. Available dating suggests that the climate transition occurred >8 Ma, prior to the formation of other small-scale ice-rich flow features identified elsewhere on Mars that have been interpreted to have formed during the most recent phases of high obliquity. Taken altogether, Asimov Crater may contain deposits related to volatile accumulation and loss from two distinct epochs of martian history, further supporting the growing evidence of multiple shifts in the martian climate.
Head James W.
Marchant David R.
Morgan Andrew G.
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