Hydrothermal and pedogenic carbonates constrain liquid water on Mars

Mathematics – Logic

Scientific paper

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[5415] Planetary Sciences: Solid Surface Planets / Erosion And Weathering

Scientific paper

Recent observations document the presence of carbonates in rock outcrops [1, 2] as well as soils [3] on Mars. The presence of carbonates on Mars has implications not only for the history of carbon dioxide on that planet, but also allows constraints to be placed on aqueous solutions on the martian surface. Here, to constrain interactions of liquid water with carbonates on Mars, we examine dissolution and precipitation rates of carbonate minerals as a function of composition, and perform thermodynamic and reactive transport modeling. Mineral dissolution rates of carbonates suggest that mineral persistences may follow the order calcite < dolomite < rhodochrosite < siderite < magnesite [4-6]. Mineral precipitation rates suggest that at low temperatures, mineral precipitation may follow the order calcite > siderite > rhodochrosite > magnesite [7-9]. Thermodynamic modeling using Geochemist's Workbench [10] suggests that siderite may be the most stable carbonate phase under Mars-relevant conditions. Reactive transport modeling using CrunchFlow [11-14] allows predictions of mineralogical profiles through carbonate rocks reacted with aqueous solutions on Mars. Therefore, observations of carbonates on Mars may allow greater constraints to be placed on the history of water on Mars.

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