Localization of Martian ridges by impact craters: Mechanical and chronological implications

Details Localization of Martian ridges by impact craters: Mechanical and chronological implications Localization of Martian ridges by impact craters: Mechanical and chronological implications

Feb 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995jgr...100.3251a&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 100, no. E2, p. 3251-3262

Mathematics

Logic

13

Geochronology, Geological Faults, Landforms, Mars Craters, Spatial Distribution, Elastic Properties, Rheology, Rocks, Stress Concentration, Stresses

Scientific paper

The eastern flank of the Tharsis dome (Mars) is affected by compressional ridges. It is shown that the position of the ridges is strongly influenced by the existence of impact craters. The distribution of crater-ridge distances has been measured in the Coprates area. This distribution shows that the intersection of ridges and impact craters with a diameter larger than 4 km is four times as frequent as a homogeneous and random distribution of craters relative to what ridges would produce. Very detailed geometric studies of relationships between intersecting ridges and craters show that these craters are older than the ridges. This localization implies that (1) ridges are superficial structures rooted at shallow depths in the megaregolith, and (2) the ridging phase occurred some time after the deposit of the ridged plain unit material, probably during the upper Hesperian. Detailed geometrical studies of ridge edges and graben/ridge width relationships suggest that ridges are bounded by two reverse faults with different offsets, and that the rheological boundary on which ridges and graben are rooted is around 1.5 km deep. Three ways are possible for an impact crater to localize strain in a regional uniaxial compressional stress field. In all three cases, the initiation of the ridges occurs in the area where a low-strength and/or stress concentration envelope around the crater is nearest to the low-strength decollement level.

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