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Laboratory simulations of Mars aqueous geochemistry |
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| Authors: | Mark A Bullock Jeffrey M Moore |
| Institution: | a Southwest Research Institute, Department of Space Studies, 1050 Walnut St., Suite 426, Boulder, CO 80302, USA b NASA Ames Research Center, Space Sciences Division, M/S 245-3, Moffett Field, CA 94035, USA c Laboratory for Atmospheric and Space Physics, Campus Box 0392, University of Colorado, Boulder, CO 80309-0392, USA |
| Abstract: | We report on laboratory experiments in which we allowed an SNC-derived mineral mix to react with pure water under a simulated Mars atmosphere for 7 months. These experiments were performed at one bar and at three different temperatures in order to simulate the subsurface conditions that most likely exist where liquid water and rock interact on Mars today. The dominant cations dissolved in the solutions we produced, which may be characterized as dilute brines, are Ca2+, Mg2+, Al3+, and Na+, while the major anions are dissolved C, F−, SO2−4 and Cl−. Typical solution pH was in the range of 4.2-6.0. Abundance patterns of elements in our synthetic sulfate-chloride brines are distinctly unlike those of terrestrial ocean water or continental waters, however, they are quite similar to those measured in the martian fines at the Mars Pathfinder and Viking 1 and 2 Landing sites. This suggests that salts present in the martian regolith may have formed over time as a result of the interaction of surface or subsurface liquid water with basalts in the presence of a martian atmosphere similar in composition to that of today. If most of the mobile surface layer was formed during the Noachian when erosion rates were much higher than at present, and if this layer is homogeneous in salt composition, the total amount of salt in the martian fines is approximately the same as in the Earth's oceans. The minimum quantity of circulating water necessary to deposit this amount of salt is approximately equivalent to a global layer 625 m deep. |
| Keywords: | Mars surface Mineralogy Regoliths |
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