Other
Scientific paper
Dec 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufm.p53a1435w&link_type=abstract
American Geophysical Union, Fall Meeting 2008, abstract #P53A-1435
Other
5415 Erosion And Weathering, 5420 Impact Phenomena, Cratering (6022, 8136), 5464 Remote Sensing
Scientific paper
The approximately 750 m diameter and 75 m deep Victoria crater in Meridiani Planum, Mars, presents evidence for significant degradation including a low, serrated, raised rim characterized by alternating alcoves and promontories, a surrounding low relief annulus, and a floor partially covered by dunes. The amount and processes of degradation responsible for the modified appearance of Victoria crater were evaluated using images obtained in situ by the Mars Exploration Rover Opportunity in concert with a digital elevation model (DEM) created using orbital HiRISE images. Opportunity traversed along the north and northwest rim and annulus and sufficiently characterized features visible in the DEM, thereby enabling detailed measurements of rim relief, ejecta thickness, and wall slopes around the entire degraded, primary impact structure. Victoria retains a 5 m raised rim consisting of 1 to 2 m of uplifted rocks overlain by 3 m of ejecta at the rim crest. The rim is 120 to 220 m wide and is surrounded by a dark annulus reaching an average of 590 m beyond the raised rim. Comparison between observed morphology and that expected for pristine craters 500 to 750 m across indicate the original, pristine crater was close to 600 m in diameter. Hence, the crater has been erosionally widened by approximately 150 m and infilled by about 50 m of sediments. Eolian processes are responsible for modification at Victoria, but lesser contributions from mass wasting or other processes cannot be ruled out. Erosion by prevailing winds is most significant along the exposed rim and upper walls and accounts for roughly 50 m widening across a WNW to ESE diameter. The volume of material eroded from the crater walls and rim is about 20 percent less than the volume of sediments partially filling the crater, indicating eolian infilling from sources outside the crater over time. The annulus formed when less than 1 m deflation of the ejecta created a lag of more resistant hematite spherules that trapped darker, regional basaltic sands.
Cohen Adam B.
Geissler Paul Eric
Golombek Matthew P.
Grant Alex J.
Kirk Randolph L.
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