Shallow Martian 'sills' - Intrusions or extrusions?

Details Shallow Martian 'sills' - Intrusions or extrusions? Shallow Martian 'sills' - Intrusions or extrusions?

Mar 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997lpi....28..463g&link_type=abstract

Conference Paper, 28th Annual Lunar and Planetary Science Conference, p. 463.

Mathematics

1

Mars Surface, Lava, Flow Distribution, Mars Craters, Mineral Deposits, Mathematical Models, Ice, Stratigraphy

Scientific paper

Thick ridged lava flows occurring south and northwest of Elysium Mons, southwest of Olympus Mons, and in the Amazonis region of Mars are associated with an etched friable deposit more than 25 m thick (based on shadow measurements of pedestal craters found within the deposit) with a feathered margin. It is proposed here that this friable deposit, regardless of origin, was present before the eruption of the textured lavas, and that the lavas were emplaced beneath it. Observations and results from numerical models further suggest that the deposit contained intergranular ice during the eruption. This scenario has broad implications for the stratigraphy of a large region on Mars.

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