Spatial distributions of secondary minerals in the Martian meteorite MIL 03346,168 determined by Raman spectroscopic imaging

Miller Range (MIL) 03346 is a nakhlite meteorite that has been extensively studied due to its unique complex secondary mineral phases and their potential implications for the hydrologic history of Mars. We conducted a set of Raman spectroscopic and Raman imaging studies of MIL 03346,168, focusing on the secondary mineral phases and their spatial distributions, with a goal to better understand the possible processes by which they were generated on Mars. This study revealed three types of calcium sulfates, a solid solution of (K, Na)‐jarosite and two groups of hydrated species with low crystallinity (HSLC) in the veins and/or mesostasis areas of the meteorite. The most abundant Ca‐sulfate is bassanite that suggests two possible paths for its direct precipitation from a Ca‐S‐H 2 O brine, either having low water activity or with incomplete development (producing bassanite with gypsum microcrystals) on Mars. The second most abundant Ca‐sulfate is soluble γ‐CaSO 4 which raises a new question on the origins of this phase in the Martian meteorite, since γ‐CaSO 4 readily hydrates in the laboratory but is apparently stable in Atacama Desert. The close spatial relationship of (K, Na)‐jarosite solid solutions with rasvumite (KFe 2 S 3 ), magnetite, HSLC, and fine‐grained low‐crystallinity alkali feldspar in mesostasis suggests a potential in situ formation of mesostasis jarosite from these Fe‐K,Na‐S‐O‐H 2 O species.