Physics
Scientific paper
Dec 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufm.p71a0436k&link_type=abstract
American Geophysical Union, Fall Meeting 2002, abstract #P71A-0436
Physics
5415 Erosion And Weathering, 6225 Mars
Scientific paper
We present forward models of crater lake basin evolution motivated by the identification of intracrater landforms on Mars which exhibit possible evidence for a history of surface water. Proposed lacustrine Martian landforms include shorelines, terraces, and wave cut benches - features that have received considerable attention in terrestrial lacustrine geomorphology but which have never been quantitatively addressed with sufficient rigor on Mars. In particular, the existing body of terrestrial research has yet to be applied adequately to planets of different gravity, temperature (or working fluid) and atmospheric pressure, such as Mars and Titan. Geomorphic evidence of surface water on Mars has important implications for planetary surface evolution, as well as for the continuing exploration of the planet as future landing sites are selected. Here we present the first quantitative forward modeling of shoreline formation under Martain conditions. Model parameters include basin size, initial topography, rock hardness, and the effects of crater impact formation on the subsequent erosional process and on sediment migration within the basin. Equations for erosion are based on terrestrial rocky coastline evolution model and have been modified for martian conditions, for instance how gravity, wind speed, and basin size, especially as the latter affect wave length and amplitude. This model will be modified for Titan as described above to explore intracrater lacustrine and shoreline processes in anticipation of the arrival of the Cassini spacecraft in the Saturn system in 2004.
Asphaug Erik Ian
Bruesch Lindsey S.
Kraal Erin R.
Lorenz Ralph D.
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