Formation of manganese oxides on early Mars due to active halogen cycling

Mitra, K.; Moreland, E. L.; Ledingham, Greg; Catalano, Jeffrey G.

doi:10.1038/s41561-022-01094-y

Cited by 7 publications

(8 citation statements)

References 66 publications

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“…A fascinating yet unresolved aspect of mineral precipitation relates to the observation of manganese‐rich nodules and fracture fillings in Gale and Endeavor craters (Arvidson et al., 2016; Berger et al., 2022; Lanza et al., 2016; Mitra et al., 2022)—deposits reminiscent of the primary precipitation of Mn oxides and hydroxides in terrestrial sediments (Freitas et al., 2013; Post, 1999).…”

Section: Systematic Survey Of Paragenetic Modesmentioning

confidence: 99%

“…Note that in this restricted context oxidation reactions involving multiple chemical changes, such as the oxidation of iron sulfides to iron oxides, are included under diagenetic processes. The oxides and hydroxides of two metal elements, Fe and Mn (Bowles et al., 2011), are frequently invoked in discussions of near‐surface redox reactions on Mars (Berger et al., 2022; King & McSween, 2005; Mitra et al., 2022).…”

Section: Systematic Survey Of Paragenetic Modesmentioning

confidence: 99%

“…Though no specific Mn minerals have been definitively identified, manganese phases have been inferred from locally enhanced concentrations (Arvidson et al., 2016; Berger et al., 2022; Lanza et al., 2016; Mitra et al., 2022).…”

Section: Systematic Survey Of Paragenetic Modesmentioning

confidence: 99%

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On the Diversity and Formation Modes of Martian Minerals

et al. 2023

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A systematic survey of 161 known and postulated minerals originating on Mars points to 20 different mineral‐forming processes (paragenetic modes), which are a subset of formation modes observed on Earth. The earliest martian minerals, as on Earth, were primary phases from mafic igneous rocks and their ultramafic cumulates. Subsequent primary igneous minerals were associated with products of limited fractional crystallization, including alkaline and quartz‐normative lithologies. Significant mineral diversification occurred via precipitation of primary phases from aqueous and atmospheric fluids, including authigenesis, hydrothermal and cryogenic precipitation, and evaporites, including freeze drying during eras of low atmospheric pressures. In particular, hydrothermal mineral formation associated with both volcanic fluids and sustained hydrothermal activity in impact fracture zones may have triggered significant mineral diversification, though as yet undocumented. At least 65 such primary minerals have been identified by flown missions to Mars and from martian meteorites. A host of secondary martian minerals were produced by near‐surface processes related to water/rock interactions, including hydration/dehydration, oxidation/reduction, serpentinization, metasomatism, and a variety of diagenetic alterations. Additional mineral diversity resulted from metamorphic events, including thermal and shock metamorphism, lightning, and bolide impacts. However, several dominant sources of mineral diversity on Earth, including: (1) extensive fluid/rock interactions and element concentration associated with plate tectonics; (2) high‐pressure regional metamorphism associated with plate tectonics; and (3) biologically mediated mineralization—are not known to be in play on Mars. Consequently, we estimate the total mineral diversity of Mars to be an order of magnitude smaller than on Earth.

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Section: Systematic Survey Of Paragenetic Modesmentioning

confidence: 99%

Section: Systematic Survey Of Paragenetic Modesmentioning

confidence: 99%

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On the Diversity and Formation Modes of Martian Minerals

et al. 2023

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“…Unlike Mn 2+/3+ -precipitates, Mn 4+ minerals are difficult to form on the Martian subsurface. Mitra et al (2023) suggest that the oxyhalogen species, chlorate and bromate in the Martian subsurface act as reactive oxidants to form Mn 4+ minerals. Although neither chlorate nor bromate is detected in the Mn-precipitates and other alteration products of Y 000802, these oxidants dissolved in groundwater may have induced the formation of Mn 4+ minerals.…”

Section: Acidic Oxidizing Environment After Alkaline Reducing Environ...mentioning

confidence: 99%

“…There is no doubt that the jarosite was formed before Y 000802 entered the Earth's atmosphere. The formation of jarosite, which requires the oxidation of Fe 2+ , is also thought to have occurred at this time when Y 000802 was exposed to an oxidizing environment by subsurface water enriched in strong oxidants (Mitra et al, 2023;Rampe et al, 2017), although we cannot exclude the possibility that some jarosite formed on Earth. A small amount of phosphorus is contained in the Mn-precipitates and Fe-rich portions (Table 2).…”

Section: Acidic Oxidizing Environment After Alkaline Reducing Environ...mentioning

confidence: 99%

Mn‐Precipitates Found in a Martian Crustal Rock

Nakamura,

Miyahara,

Suga

et al. 2023

JGR Planets

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Alteration minerals in one of the Martian meteorite nakhlites, Yamato (Y) 000802, were studied to understand the alteration process and conditions. Mn‐precipitates are discovered between altered plagioclase grains in Y 000802. Mn‐precipitates consist of hausmannite (), manganite (γ‐Mn3+OOH), rhodochrosite (Mn2+CO3), and a trace amount of Mn4+O2 mineral. Jarosite ) is also found. Mn2+ dissolved from olivine contributes to the formation of Mn‐precipitates. A weakly acidic‐neutral fluid containing a trace amount of altered the olivine, and Mn2+ was dissolved into the fluid. The fluid also reacted with plagioclase and probably induced dealkalization of plagioclase, causing a local strong alkaline environment. Plagioclase was altered to ferroan saponite‐nontronite + amorphous SiO2 under alkaline conditions. Simultaneously, Mn2+/3+‐precipitates were formed from the Mn2+‐containing fluid in the interstices between the altered plagioclase grains under the strong alkaline reducing environment. These alterations occurred in the deep part of the nakhlite body, where they are isolated from Martian subsurface water, including strong oxidants. The formation of Mn2+/3+‐precipitates may have been triggered by the melting of permafrost caused by an impact event around ∼633 Ma. Later, the nakhlite body was probably excavated by another impact, making it susceptible to water including strong oxidants. Pyrrhotite was dissolved and a highly acidic oxidizing fluid was formed, which would induce the formation of jarosite and the Mn4+O2 mineral between ∼633 Ma and ∼11 Ma.

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