Mathematics – Logic
Scientific paper
Dec 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufm.p51b0355m&link_type=abstract
American Geophysical Union, Fall Meeting 2002, abstract #P51B-0355
Mathematics
Logic
1823 Frozen Ground, 1829 Groundwater Hydrology, 1863 Snow And Ice (1827), 6200 Planetology: Solar System Objects (New Field), 6225 Mars
Scientific paper
Malin and Edgett [2000] reported geologic features resembling terrestrial water-carved gullies in the mid and high latitudes of Mars. They occur poleward of about 30§ latitude, primarily in the southern hemisphere. More often they are reported on poleward facing slopes than equatorward facing slopes, though they occur on all orientations of slopes. The morphology of the gullies varies but typically consists of a source region "alcove" of order 100 m wide, v-shaped channels of order 10 m wide leading from the alcove, and a depositional fan. The source regions appear to originate a few hundred meters or less from the top of the local slope and are frequently, but not always, associated with exposed strata of material that appear to exhibit significant cohesive strength. Erosion is best explained by a fluid of some sort and water is considered the most likely candidate from a morphological standpoint. These features are believed to be geologically young by their superposition atop dunes and permafrost polygons; how young is difficult to determine, though a range of older than 20 years to younger than 1 million years is suggested. Models for the formation of these features are diverse, ranging from the canonical water-driven erosion of soil and rock, to both liquid or gaseous carbon-dioxide outbursts, to dry debris flows and wind erosion. Sources of fluid for mobilizing the soil are also diverse, including melting surface ice or snow deposits, melting of near-surface ground ice, and shallow or deep aquifers of water or brines, as well as melting subsurface dry-ice or clathrate deposits. Any viable model needs to be consistent with the breadth of geomorphic observations and should fit within the constraints of the martian climate and thermophysical processes that occur. Models for the formation of martian gullies will be reviewed and discussed in the context of observational data.
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