Modeling Mass Movements - Validation for Planetary Studies.

Details Modeling Mass Movements - Validation for Planetary Studies. Modeling Mass Movements - Validation for Planetary Studies.

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufm.p22d..01b&link_type=abstract

American Geophysical Union, Fall Meeting 2001, abstract #P22D-01

Mathematics

Logic

1824 Geomorphology (1625), 5400 Planetology: Solid Surface Planets

Scientific paper

High-resolution images acquired by MOC show gullies on the walls of impact craters and valleys on Mars. Deposits associated with these gullies have been interpreted as characteristic of debris flow. Evidence for mass movements are increasingly being identified on the terrestrial planets and moons. Traditionally planetary scientists, constrained by available imaging data, have used geomorphologic arguments to make broad interpretations of the physics governing mass movements. Recent acquisitions of higher-resolution topography and imagery on Mars and Eros allow for re-evaluations of the physics and possible rheological characteristics of mass movements, including the presence of water, in planetary environments. Use of these data requires calibration and testing of any physical models of flows through rigorous terrestrial fieldwork. In this study, we test applications of two empirical models to provide more direct estimates of the dynamics of proposed mass movements on Mars. We obtained topographic profiles and superelevation data over two sites: Generals Slide debris flow in Madison, VA and Chaos Jumbles, CA. At Madison, we tested two versions of a Chezy-type model that applies to fast moving flows with suspension: (1) assumes constant volumetric flow rate while (2) uses actual flow speed estimated from superelevation data. In both cases we, focus on the empirical parameter C whose magnitude gauges energy dissipation in a flow. We obtain estimates for the absolute magnitude and variations in C along the channel, which we compare to additional geomorphologic and eye-witness evidence. Results indicate that the second approach provided information on the flow behavior most consistent with the geomorphic evidence. In addition, our analysis suggests that the main event at the Gernerals Slide was a wet debris flow, consistent with eye-witness evidence at the site. Given this validation, Chezy-type modeling has application for planetary studies with data such as MOLA providing topographic parameters and MOC the geomorphic indicators used to calculate flow speeds. At the Chaos Jumbles rock avalanche we will test a basal glide model where movement rate increases linearly with flow thickness.

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