HR: 1340h
AN: P13A-0991    [Abstracts]
TI: Survey of Martian Alluvial Fans
AU: * Kraal, E R
EM: ekraal@es.ucsc.edu
AF: UCSC Earth Science Department, 1156 High Street, Santa Cruz, CA 95064 United States
AU: Moore, J
EM: jeff.moore@nasa.gov
AF: UCSC Earth Science Department, 1156 High Street, Santa Cruz, CA 95064 United States
AU: Asphaug, E
EM: asphaug@es.ucsc.edu
AF: NASA Ames, NASA Ames Research Center, MS 245-3, Moffet Field, CA 94035-1000 United States
AU: Howard, A
EM: alanh@virginia.edu
AF: University of Virginia, Department of Environmental Sciences 291 McCormick Rd, P.O. Box 400123, Charlottesville, VA 22904 United States
AB: Recent higher resolution images of the Martian surface reveal another complex geomorphic surface process - alluvial fans. Alluvial fans composed of water-transported, loose sediment deposited as the flow moves from steep, eroding terrain to low-gradient depositional basins. Martian alluvial fans are concentrated along crater rims where they erode into the higher surround topography depositing sediment into the crater interior. Initial work by Moore and Howard [2004] examined some of these fans in a band from 0-30 S. Their initial results included fan statistics, such as area and slope, and indicated that the fans were clustered in discrete areas. However, this survey was hampered by incomplete image coverage. We present the progress of our continuing, planet wide survey of alluvial fans. Specifically we focus on understanding if alluvial fans are indeed clustered in particular areas and if so, why. In addition, we expand fan statistics to include a comparison of fan volume to eroded area.
DE: 5415 Erosion and weathering
DE: 6225 Mars
SC: Planetary Sciences [P]
MN: 2004 AGU Fall Meeting