1. Preservation Potentials of Siderite in Low‐Temperature Brines Relevant to Mars.
- Author
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Chen, Bohao, Yu, Xiao‐Wen, Zhao, Yu‐Yan Sara, Zhou, Di‐Sheng, Qu, Shuai‐Yi, Zhao, Jiannan, Qi, Chao, Li, Xiongyao, and Liu, Jianzhong
- Subjects
ATMOSPHERIC carbon dioxide ,GALE Crater (Mars) ,MARTIAN surface ,SIDERITE ,LOW temperatures ,GOETHITE - Abstract
The scarce carbonate record on the Martian surface is one of the fundamental unsolved issues for paleoclimate and environmental evolution. Whether carbonates first formed and then dissolved due to a transition in global environments or whether Mg–Fe carbonates never extensively formed due to geochemical kinetics thresholds remains unknown. In this study, we experimentally examined the preservation potential of siderite in Mars‐relevant fluids, including ultrapure water, H2O2, NaClO4, NaClO3, NaCl, Na2SO4, NaHCO3, and Na2SiO3 solutions, at 277 K. The effects of the water/rock ratio at WR10 and WR100 on dissolution rates were also investigated. We found that siderite dissolution and subsequent oxidation and hydrolysis of leached Fe did not substantially acidify the solutions. The siderite dissolved relatively rapidly in the chloride and chlorate solutions and slowly in the silica or bicarbonate solutions. In a circum‐neutral to slightly alkaline aqueous environment with oxidative species, the mobility of leached Fe was limited, leading to the formation of goethite or lepidocrocite, which clustered on the siderite surface. The longest lifetime of 1‐mm siderite grains was found in the Na2SiO3 solution at WR100, which was estimated to range from 198 ka to 198 Ma. Water‐limited, silica‐rich, and oxidative aqueous environments benefit siderite preservation on the Martian surface. Our results support that the lack of voluminous siderite on Mars may be primarily due to the inhibition of its formation rather than alteration and dissolution after its presence, consistent with the recent detection of Mg–Fe carbonate at Gale Crater and Jezero Crater. Plain Language Summary: Despite the predominant carbon dioxide atmosphere, the distribution of carbonate outcrops on Mars detected to date is very limited. The discrepancy between the CO2‐dominant atmosphere and scarce carbonate records is one of the key issues for understanding the paleoclimate and environmental evolution of Mars. We experimentally investigated the preservation potential of siderite in eight Mars‐relevant fluids under water‐limited versus water‐abundant scenarios at 277 K. We found that water‐limited conditions, silica‐rich environments, and the presence of oxidants in aqueous environments generally benefit siderite preservation. The longest lifetime of 1‐mm siderite grains is present in silica‐rich solutions, estimated to range from 198 ka to 198 Ma. In a neutral to alkaline aqueous environment with oxidative species, the mobility of leached iron is limited, and the Fe precipitates are mainly in the form of goethite or lepidocrocite, accumulating on the siderite surface. Martian aqueous environments can efficiently preserve siderite. Therefore, the lack of voluminous siderite on Mars may be because siderite was never extensively formed rather than altered and dissolved after its presence. Key Points: Siderite dissolves relatively fast in chloride‐ and chlorate‐fluids and slowly in silica‐ and bicarbonate‐fluidsWater‐limited, silica‐rich, and oxidative aqueous environments favor siderite preservation on the Martian surfaceThe scarcity of voluminous siderite on Mars may be due to the inhibition of its formation rather than its dissolution after its presence [ABSTRACT FROM AUTHOR]
- Published
- 2024
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