Water in the Martian crust - Slope-parallel layers in the wall of Melas Chasma are Hesperian-age soil horizons

Details Water in the Martian crust - Slope-parallel layers in the wall of Melas Chasma are Hesperian-age soil horizons Water in the Martian crust - Slope-parallel layers in the wall of Melas Chasma are Hesperian-age soil horizons

Mar 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997lpi....28.1447t&link_type=abstract

Conference Paper, 28th Annual Lunar and Planetary Science Conference, p. 447.

Physics

Mars Surface, Planetary Crusts, Ground Water, Stratigraphy, Topography, Lithology, Erosion, Highlands, Ice

Scientific paper

In the south wall of Melas Chasma, erosional scarps expose color and strength layers in the highlands crust. The layers do not form a coherent stratigraphy; each scarp exposes a different layer sequence, parallel to local prescarp topography. These relations suggest that the layers formed in place by alteration of preexisting material, i.e., the layers are soil horizons. Alteration was most likely mediated by liquid water, probably as intergranular films. The water was likely derived from ground ice.

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