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Formation of Carbonates in Martian Meteorite ALH 84001: Cool Water Near the Surface of Mars

Formation of Carbonates in Martian Meteorite ALH 84001: Cool Water Near the Surface of Mars. ALH 84001 igneous age ( Ieft side of gray box) and carbonate age (right) fall in the period of active aqueous processes on Mars.

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Formation of Carbonates in Martian Meteorite ALH 84001: Cool Water Near the Surface of Mars

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  1. Formation of Carbonates in Martian Meteorite ALH 84001:Cool Water Near the Surface of Mars ALH 84001 igneous age (Ieft side of gray box) and carbonate age (right) fall in the period of active aqueous processes on Mars. Secondary carbonates in ancient orthopyroxenite ALH 84001 record key information about the environment of their formation. Ehlmann et al. (2011)

  2. Clumped Isotope Thermometry Experimental data like these and thermodynamic principles allow us to correlate 47 with temperature. The mean value of ALH 84001 implies 18°C (±4) Isotopologues of CO2 differ in how much 12C, 13C, 16O, 17O, and 18O they contain. Mass 47 is useful because it contains both 13C and 18O, which have a temperture-dependent preference for residing in the same molecule. The parameter 47 derives from the abundance ratios of masses 47 and 44, compared to the value expected if the isotopes are randomly distributed among the isotopologues.

  3. Evaporating Fluids, Precipitating Carbonates Physical Model: Fractured near-surface of Mars is saturated at some depth with water. Evaporation causes carbonates to form. Little connection with the atmosphere, so evaporation causes correlated changes in 13C and  18O.

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