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Atmospheric conditions on early Mars and the missing layered carbonates
Author(s) -
Bullock Mark A.,
Moore Jeffrey M.
Publication year - 2007
Publication title -
geophysical research letters
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.007
H-Index - 273
eISSN - 1944-8007
pISSN - 0094-8276
DOI - 10.1029/2007gl030688
Subject(s) - noachian , hesperian , mars exploration program , atmosphere (unit) , atmosphere of mars , geology , carbonate , astrobiology , tharsis , precipitation , atmospheric escape , geochemistry , martian , materials science , meteorology , physics , metallurgy
Widespread, massive layered sediments, studied by surface rovers and Mars‐orbiting spectrometers, are found to be rich in sulfates. No similarly massive carbonates have been detected. We present the results of coupled atmospheric and geochemical calculations of the formation of the sulfate‐rich Meridiani sediments, and offer an explanation for why extensive layered carbonates are not found there or elsewhere on Mars. Large scale volcanism from the build‐up of Tharsis during the late Noachian would have injected large amounts of SO 2 into the atmosphere. Efficient photochemical conversion of SO 2 to H 2 SO 4 would have caused widespread sulfuric acid/water clouds, similar to those seen on Venus today. Precipitation from these clouds and acidification of surface water would have sustained a thick, warm CO 2 atmosphere via carbonate inhibition. Such an atmosphere could have been subjected to loss to space via impact erosion and sputtering. Once atmospheric SO 2 gas production dropped and waters become more alkaline, the remaining CO 2 in the atmosphere collapsed to form poorly consolidated carbonate patinas on rock surfaces and in open fractures.