The Common Ion Effect in Deposition of Martian (e.g., Allan Hills 84001) carbonates

Details The Common Ion Effect in Deposition of Martian (e.g., Allan Hills 84001) carbonates The Common Ion Effect in Deposition of Martian (e.g., Allan Hills 84001) carbonates

Jan 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998mmws.workq..58w&link_type=abstract

Workshop on the Issue Martian Meteorites: Where do we Stand and Where are we Going?, p. 58

Other

Carbonates, Evaporation, Lakes, Mars (Planet), Mars Surface, Sulfates, Water, Ions, Snc Meteorites, Geochemistry, Magnesium, Sulfur Oxides

Scientific paper

The most plausible model for origin of the carbonates in the ALH84001 meteorite involves deposition from a playa lake or zone of groundwater that underwent evaporative concentration at or near the surface of Mars. A key constraint for such a model is the virtual absence of sulfate in ALH84001. In a simple closed-system evaporation sequence, abundant sulfate would be expected to form from any plausible martian lake or shallow groundwater. However, several factors would potentially alter the course of the evaporation-deposition sequence enough to engender extremes of sulfate/carbonate fractionation, including the extremely low sulfate/carbonate ratio of ALH84001. Assuming the evaporating water body was transient in nature (i.e., the product of a flood), the water level could easily have been receding during the evaporation-deposition process, and we need only assume that carbonate deposition, but not sulfate deposition, occurred before the water level receded below the level where ALH84001 was perched. Occlusion of pores by incipient sulfate precipitation, in the outer fringes of the rock that ultimately became ALH84001 and/or in overlying solid materials, might also have reduced the yield of sulfate deposition in ALH84001. Another factor that probably played a key role is the common ion effect.

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