Formation of Martian flood features by release of water from confined aquifers

Details Formation of Martian flood features by release of water from confined aquifers Formation of Martian flood features by release of water from confined aquifers

Jun 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979jgr....84.2995c&link_type=abstract

Journal of Geophysical Research, vol. 84, June 10, 1979, p. 2995-3007.

Astronomy and Astrophysics

Astrophysics

176

Aquifers, Floods, Hydrology, Mars Surface, Water Flow, Channels, Ground Water, Planetary Evolution, Porous Materials, Terrain Analysis, Volcanoes, Mars, Water, Channels, Topography, Erosion, Origin, Volcanism, Meteoroid Impacts, Permafrost, Pressure, Flow, Brecciation, Rocks, Cooling, Floods, Craters, Martian

Scientific paper

It is proposed that the rapid release of water under great pressure from deeply buried aquifers is responsible for the formation of the Martian channels suggestive of catastrophic flooding (outflow channels). Fine channels in the Martian surface suggest the presence of surface water early in the history of the planet, which would have entered the ground water system through the porous near-surface rocks. Subsequent global cooling would have trapped the ground water under a thick permafrost layer and formed a system of confined aquifers. High pore pressures within the aquifers are considered to have triggered the breakout of water from the aquifers at rates of from 10 to the 5th to 10 to the 7th cu m/sec, which would be prevented from reentering the ground water system by the layer of permafrost. Outflow from the aquifer is also considered to have caused the undermining of adjacent areas and the collapse of the surface to form areas of chaos, often associated with channels.

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