Mathematics – Logic
Scientific paper
Dec 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufm.p21b1665l&link_type=abstract
American Geophysical Union, Fall Meeting 2011, abstract #P21B-1665
Mathematics
Logic
[5415] Planetary Sciences: Solid Surface Planets / Erosion And Weathering, [5464] Planetary Sciences: Solid Surface Planets / Remote Sensing, [6225] Planetary Sciences: Solar System Objects / Mars
Scientific paper
Gale is an impact crater of 150 km in diameter, formed at Late Noachian/Early Hesperian located close to the dichotomy boundary and to the Medusae Fossae Formation. This crater is partially filled by a crescent-shaped mound of layered deposits up to 5 km thick and 6000 km2 in area, for which several origins have been proposed including volcanic, eolian, and fluviatile and lacustrine processes, precipitation as spring deposits, and a combination of several origins. The past presence of water is attested by the occurrence of many channels carved into the deposits and the crater rim, and of phyllosilicates and sulfates located in the lowest part of the deposits. Hence, Gale crater is a site of high interest to understand the evolution of the geochemical and climatic environment of the region through time, and may have had favorable conditions for supporting life in the past. This will be studied in situ by Curiosity (Mars Science Laboratory) from August 2012. In order to better constrain the history of Gale and the origin of its deposits, a geologic map of Gale crater based on the analysis of the orbital data CTX (~ 6 m/pixel) and HiRISE (25-32 cm/pixel) was produced. The geometry of the layered deposits was measured from HiRISE DEM. The geological units and landforms were defined according to their location, physical characteristics, albedo, erosion patterns, and mineralogical composition. Five main units were identified within the mound of layered deposits, which are interpreted as mainly airfall deposits including aeolian dunes. North of the mound, linear lobate features and a fan-shaped feature might have resulted from mass-wasting processes (i.e., landslides, debris flows, or viscous flows). The crater fill units correspond to deposits located on the rims and on the floor of the crater. They are incised by many valleys and superposed by sinuous ridges, interpreted as fluvial channels and inverted channels respectively. These crater fill units are interpreted as colluvial and alluvial deposits. Fan-shaped deposits are located at the outlet of canyons incised into the mound and the crater rim that may correspond to alluvial fans and/or fan deltas. Subhorizontal terraces, fan deltas, valleys and canyons, phyllosilicates and sulfates as well as mass-wasting deposits could be related in origin to a shallow lake that existed at a time when some of the mound units were already formed.
Fueten Frank
Hauber Ernst
Jaumann Ralf
Le Deit Laetitia
Mangold Nicolas
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