Far-field tectonics associated with a large impact basin - Applications to Caloris on Mercury and Imbrium on the moon

Details Far-field tectonics associated with a large impact basin - Applications to Caloris on Mercury and Imbrium on the moon Far-field tectonics associated with a large impact basin - Applications to Caloris on Mercury and Imbrium on the moon

Mar 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982e%26psl..58..104f&link_type=abstract

Earth and Planetary Science Letters, vol. 58, no. 1, Mar. 1982, p. 104-115.

Mathematics

13

Far Fields, Lunar Craters, Mercury (Planet), Planetary Craters, Structural Basins, Tectonics, Ejecta, Impact Damage, Lithosphere, Lunar Surface, Mathematical Models, Membrane Structures, Planetary Surfaces, Stress Distribution, Thin Walled Shells, Viscoelasticity, Planets, Mercury (Planet), Moon, Tectonism, Impacts, Basins, Formation, Caloris Basin, Imbrium, Mare, Lithosphere, Models, Perturbations, Stress, Surface, Ejecta, Compression, Scarps, Grabens, Patterns, Distribution, Comparisons, Mathematical Mode

Scientific paper

Lithospheric readjustments after the formation of a large impact crater have been computed. The models predict tectonic perturbations over a major portion of the surface of the planet. The weight of the ejecta and the mechanical perturbations in the crater area give rise to membrane stresses. If the planetary lithosphere is in compression, the direction of maximum compression after the impact is perpendicular to a meridian (in a referential where the basin would be at the north pole). On Mercury the preferential orientation of compressive scarps radial to Caloris is explained in this manner. For a planet in extension grabens perpendicular and parallel to a meridian can appear successively as the mechanical state of the crater area is modified. On the moon this result is consistent with the large-scale tectonics associated with Imbrium.

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