Statistics – Computation
Scientific paper
Dec 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufm.p51b1430s&link_type=abstract
American Geophysical Union, Fall Meeting 2010, abstract #P51B-1430
Statistics
Computation
[1810] Hydrology / Debris Flow And Landslides, [5415] Planetary Sciences: Solid Surface Planets / Erosion And Weathering, [6225] Planetary Sciences: Solar System Objects / Mars, [8020] Structural Geology / Mechanics, Theory, And Modeling
Scientific paper
High-resolution MOC, THEMIS, HiRISE, and HRSC image data and geomorphologic characterization based on MOLA-derived topography are being used as input for discrete element modeling to simulate slope failure in Valles Marineris. Two landslides have been selected for detailed analysis. The first landslide, in Coprates Chasma, has a strongly arcuate and recessional 4-km-high main scarp, and a runout length of approximately 70 km to the opposing canyon wall. The landslide deposit or transported material has a hummocky topography. The second landslide, in Ganges Chasma, has a 3-4 km high main scarp, a complex rupture surface with a displaced block, and a runout length of approximately 25 km. The landslide deposit is characterized by longitudinal ridges and furrows. The main scarp and displaced material of a landslide provide insight into the mechanical nature of the surface and shallow subsurface of Mars. We use two-dimensional discrete element models oriented parallel with the slide direction to examine the effects of mechanical layering upon the morphology of slip surfaces, scarps, and transported deposits that form as a result of slope failure on Mars. The initial geometry of the models is designed to replicate the height and length of each study site and to capture the observed and interpreted mechanical stratigraphy. Discrete element particle diameters range from approximately 30-60 m; a compromise between model fidelity and computation time. Bond properties (i.e., bond stiffness and strength), which control the macroscale behavior, are adjusted between layers to produce variable mechanical stratigraphic configurations. Our models were conducted under Mars gravity (3.71 m/s2) using a pre-slide free surface that dips 60°. Model results show that an initial slip surface forms some distance from the lateral free surface and subsequently migrates away from the free surface in discrete increments producing a well-developed main scarp. The models also show rotated blocks of competent strata, localized zones of shear displacement and distributed flow of weaker materials. Model geometries are similar to morphologic features observed in both landslides. For example, the Coprates Chasma model shows a well-developed main scarp as well as a hummocky, irregular upper surface across the displaced material that is similar to topographic profiles from MOLA data. The Ganges Chasma model also shows a well-developed scarp and an irregular deposit that includes several displaced and rotated blocks. These preliminary results demonstrate the power of discrete element modeling as an appreciable step toward a new understanding of the stratigraphy and mechanical nature of the upper crust of Mars.
Hooper Donald M.
Sims Darrell W.
Smart Kevin J.
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