Physics
Scientific paper
Dec 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007agufm.p34a..07m&link_type=abstract
American Geophysical Union, Fall Meeting 2007, abstract #P34A-07
Physics
5420 Impact Phenomena, Cratering (6022, 8136), 5480 Volcanism (6063, 8148, 8450), 6225 Mars, 8426 Mud Volcanism, 8450 Planetary Volcanism (5480, 6063, 8148)
Scientific paper
HiRISE images of the impact crater Tooting (~29 km dia., located at 23.4°N, 207.5°E) on Mars have revealed a remarkable series of lobate flows on the southern rim, wall and floor of the crater. The origin of these flows has not yet been determined, but their spatial distribution and morphology could indicate that they are flows of impact melt, mudflows, or lava flows. Tooting crater shows numerous signs of being very young (very few superposed impact craters, very high depth/diameter ratio, high thermal inertia ejecta, and a well preserved set of secondary craters), and so allows detailed analysis of these unusual flows, which appear to be almost pristine. We have developed a 2-meter digital elevation model of Tooting using stereo HiRISE images to characterize the flows, which in general are <10 m thick. Four distinct flow fields have been identified: (1) an extensive flow field on the S rim that appears to be solidified melt sheet ~2.5 km x 1.7 km in size that has four 200 to 600 m long flows with festoon ridges on their surface. (2) A single lobate flow on the SW rim that originates from a smooth "catchment area" of low relief close to the crater rim crest. Five discrete segments of this flow exist, including a 1.3 km segment with a discrete 15 m wide central channel and three lobate distal margins. (3) A set of 7 lobes ~700 m long on the inner S wall. These lobes have very well defined central channels ~25 m wide and levees <4 m wide. (4) A lobe complex on S floor that includes lobes >30 m thick and 300 m wide. These flows no doubt formed in an unusual environment, probably including extensive amounts of impact melt, volatiles released from the substrate, and highly unstable slopes on the crater rim. Tooting crater therefore displays a novel planetary flow field; the correct identification of the origin of these flows holds significance for understanding the role of volatiles in the impact cratering process, the potential of thermal anomalies existing within the crater cavity for extended period of time, and the emplacement of the ejecta. We are therefore developing numerical models, based on the rheology of lava flows, in order to help to resolve the origin of this flow field.
Garbeil Harold
Mouginis-Mark Peter J.
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