A brittle model for Martian ridges constrained by surface geometry

Details A brittle model for Martian ridges constrained by surface geometry A brittle model for Martian ridges constrained by surface geometry

Nov 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992crasb.315.1397a&link_type=abstract

Academie des Sciences (Paris), Comptes Rendus, Serie II - Mecanique, Physique, Chimie, Sciences de la Terre et de l'Univers (ISS

Mathematics

Logic

2

Geological Faults, Hypervelocity Impact, Mars Craters, Mars Surface, Ridges, Constraints, Mars Volcanoes, Tectonics

Scientific paper

Geometrical relationships between ridges and impact craters, ridges and grabens, and ridges and ancient terrains on Mars show that a purely brittle model for Martian ridges is viable. Ridges are limited by two inverse conjugated faults rooted on a rheological interface situated at a depth of 1 km. The magnitude of shortening associated with a single ridge is about 1 km; the total magnitude of shortening of the Lunae Planum region is about 22 km.

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