Characterization of Martian near-subsurface materials by determination of cohesion and angle of internal friction

Details Characterization of Martian near-subsurface materials by determination of cohesion and angle of internal friction Characterization of Martian near-subsurface materials by determination of cohesion and angle of internal friction

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992msat.work..152s&link_type=abstract

In Lunar and Planetary Inst., Workshop on the Martian Surface and Atmosphere Through Time p 152-153 (SEE N92-28988 19-91)

Physics

Avalanches, Cohesion, Internal Friction, Mars (Planet), Mars Surface, Planetary Geology, Slopes, Topography, Weathering, Bedrock, Debris, Failure, Gradients, Gravitation, High Resolution, Imaging Techniques, Mars Observer, Relief Maps, Spectra, Stability

Scientific paper

Back-analysis (reconstruction) of the stability of thirty avalanche chutes was performed in the very limited areas where high resolution imaging overlapped with available 1:500 K topographic map coverage. A new technique was developed to incorporate the third dimension (width) of an avalanche chute in stability back-analysis in order to yield unambiguous values of cohesion and angle of internal friction. The procedure is based upon extending the ordinary method of slices to three dimensions, in order to construct avalanche chute cross-sections whose widths and depths vary as a function of gradient, gravity, density of material, and phi and c. Applying the technique to the well documented slide at Lodalen, Norway as a test produces excellent correspondence with reality. Generally, the technique reveals that the width:depth ratio of any avalanche chute decreases with increasing contrast between the average slope angle and the angle of internal friction. Applying this technique to the martian avalanche chute yields results consistent with indications from earlier work, but with greater certainty. Values of cohesion and angle of internal friction identify the materials at the time of failure as moderately cohesive debris. If Sharp's identification of these features as avalanche chutes is correct, then the results here imply that weathering processes have had a significant effect to depths of tens of meters (where failure has occured) below the martian surface. It is also implied that on relatively steep slopes within Valles Marineris, sizable, unaltered, unmantled bedrock exposures for high resolution spectral and spatial scanning by Mars Observer may be scarce.

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