Quantitative analysis of the extensional tectonics of Tharsis bulge, Mars - Geodynamic implications

Details Quantitative analysis of the extensional tectonics of Tharsis bulge, Mars - Geodynamic implications Quantitative analysis of the extensional tectonics of Tharsis bulge, Mars - Geodynamic implications

Jul 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993jgr....9813097t&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 98, no. E7, p. 13,097-13,108.

Mathematics

Logic

14

Craters, Geodynamics, Geological Faults, Mars Surface, Tectonics, Topography, Mars Volcanoes, Planetary Crusts, Planetary Evolution, Quantitative Analysis, Mars, Tharsis, Analysis, Tectonics, Geodynamics, Extension, Surface, Features, Impact Craters, Shape, Elipicity, Strain, Faulting, Stress, Thaumasia, Alba Patera, Tempe, Elongation, Mareotis Fossae, Motion, Morphology, Topography, Origin, Formation, Depth, Gravity Effects, Viscosity, Parameters, Lunar Palus, Corprates, Model, Gravity Field, Grabens, Dist

Scientific paper

The amount of horizontal strain on the Martian Tharsis bulge is quantified in order to provide further information on the tectonic evolution of this province. About 10 percent of the Tharsis surface bulge exhibits elliptical impact craters, which are the largest strain markers in the solar system. It is shown that these strain ellipses indicate more strain than could be due to the bulge building alone. The existence of such intensely deformed areas, the direction of the extensive strain, the localization of these areas on the bulge crest or on the top of topographic slopes, and the evidence of nonthinned crust under these areas may all be explained by gravitational slidings of the bulge surface over the topographic slope. This sliding would be possible because of the presence of a decollement level two kilometers below the surface, and because of the prefracturation which have made the detachment possible.

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