Martian landslides-classification and genesis (original) (raw)

A large number of variables affect the morphology of landslide deposits including the nature of the rupture surface, physical properties of the failed mass (lithology, stratification, strength), the volume of the slide, height of fall, surface gravity, adjacent topography, and the nature and efficiency of any lubricating mechanisms. Study of Viking images has revealed the presence of numerous landslide scars and deposits on the walls and floors of Valles Marineris (1). Over 20 large landslides (volume >10 billion m3) are located in Ius and Tithonium Chasmas alone. A variety of landslide morphologies exists. Schroder (2) defined the surface of rupture (A in ) as the surface along which the rock mass becomes unattached, the foot line (FL) as the line of intersection between the lower part of the surface of rupture and the original ground surface, and the surface of translation (B) as the surface below the foot line over which the slide has moved. The position of the landslide deposit relative to the surface of rupture can be used to classify three types of landslide features. Those landslide deposits which lie predominantly upon the surface of rupture, topographically higher than the foot line are herein called Class I landslides. Class II landslides have substantial areas above the surface of rupture and the surface of translation. Class III deposits lie entirely over the surface of translation, essentially all of the material has been transported away from the surface of rupture. This geomorphic classification is preferred for martian landslides because it is simple, does not depend on the composition of the slide mass and is nongenetic, but still allows comparisons that give insight into slide development.

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