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On the in situ aqueous alteration of soils on Mars |
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| Authors: | Ronald Amundson Stephanie Ewing Brad Sutter Oliver Chadwick Michelle Walvoord |
| Institution: | a Division of Ecosystem Sciences, 137 Mulford Hall, University of California, Berkeley, CA 94720, USA b Department of Earth and Planetary Science, McCone Hall, University of California, Berkeley, CA 94720, USA c Jacobs NASA/Johnson Space Center, MC JE23, 2224 Bay Area Blvd., Houston, TX 77058, USA d Department of Geography, University of California, Santa Barbara, CA 93106, USA e Space Sciences Laboratory, 7 Gauss Way, University of California, Berkeley, CA 94720, USA f U.S. Geological Survey, Denver Federal Center, Box 25046, MS-413, Lakewood, CO 80225-0046, USA g NASA-Ames Research Center, Building 245, Room 212, MS 245-3, Moffett Field, CA 94035, USA |
| Abstract: | Early (>3 Gy) wetter climate conditions on Mars have been proposed, and it is thus likely that pedogenic processes have occurred there at some point in the past. Soil and rock chemistry of the Martian landing sites were evaluated to test the hypothesis that in situ aqueous alteration and downward movement of solutes have been among the processes that have transformed these portions of the Mars regolith. A geochemical mass balance shows that Martian soils at three landing sites have lost significant quantities of major rock-forming elements and have gained elements that are likely present as soluble ions. The loss of elements is interpreted to have occurred during an earlier stage(s) of weathering that may have been accompanied by the downward transport of weathering products, and the salts are interpreted to be emplaced later in a drier Mars history. Chemical differences exist among the sites, indicating regional differences in soil composition. Shallow soil profile excavations at Gusev crater are consistent with late stage downward migration of salts, implying the presence of small amounts of liquid water even in relatively recent Martian history. While the mechanisms for chemical weathering and salt additions on Mars remain unclear, the soil chemistry appears to record a decline in leaching efficiency. A deep sedimentary exposure at Endurance crater contains complex depth profiles of SO4, Cl, and Br, trends generally consistent with downward aqueous transport accompanied by drying. While no model for the origin of Martian soils can be fully constrained with the currently available data, a pedogenic origin is consistent with observed Martian geology and geochemistry, and provides a testable hypothesis that can be evaluated with present and future data from the Mars surface. |
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