Quantification of Carbonates, Oxychlorines, and Chlorine Generated by Heterogeneous Electrochemistry Induced by Martian Dust Activity

Wang, A.; Jackson, Andrew W.; Sturchio, Neil C.; Houghton, Jennifer; Yan, Chuck Y. C.; Olsen, Kevin; Qu, Quincy H. K.

doi:10.1029/2022gl102127

Cited by 7 publications

(11 citation statements)

References 41 publications

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“…One type of formation processes involves a relatively recent formation at low water chemical activity and possibly low temperature by rapid olivine carbonation and/or catalysis by heterogeneous electrochemistry (Garenne, 2013; Kelemen, 2020; Shaheen et al., 2010; Wang et al., 2022). Such processes rely on gas‐surface interactions and should form carbonates preferentially in the first few micrometers to tens of micrometers at the surface.…”

Section: Discussionmentioning

confidence: 99%

Carbonate Detection With SuperCam in Igneous Rocks on the Floor of Jezero Crater, Mars

Clavé

Benzerara²,

Meslin

et al. 2023

JGR Planets

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Perseverance explored two geological units on the floor of Jezero Crater over the first 420 Martian days of the Mars2020 mission. These units, the Máaz and Séítah formations, are interpreted to be igneous in origin, with traces of alteration. We report the detection of carbonate phases along the rover traverse based on laser-induced breakdown spectroscopy (LIBS), infrared reflectance spectroscopy (IRS), and time-resolved Raman (TRR) spectroscopy by the SuperCam instrument. Carbonates are identified through direct detection of vibrational modes of CO 3 functional groups (IRS and TRR), major oxides content, and ratios of C and O signal intensities (LIBS). In Séítah, the carbonates are consistent with magnesite-siderite solid solutions (Mg# of 0.42-0.70) with low calcium contents (<5 wt.% CaO). They are detected together with olivine in IRS and TRR spectra. LIBS and IRS also indicate a spatial association of the carbonates with clays. Carbonates in Máaz are detected in fewer points, as: (a) siderite (Mg# as low as 0.03); (b) carbonate-containing coatings, enriched in Mg (Mg# ∼0.82) and spatially associated with different salts. Overall, using conservative criteria, carbonate detections are rare in LIBS (∼30/2,000 points), IRS (∼15/2,000 points), and TRR (1/150 points) data. This is best explained by (a) a low carbonate content overall, (b) small carbonate grains mixed with other phases, (c) intrinsic complexity of in situ measurements. This is consistent with orbital observations of Jezero crater, and similar to compositions of carbonates previously reported in Martian meteorites. This suggests a limited carbonation of Jezero rocks by locally equilibrated fluids. Plain Language SummaryCarbonates are mineral phases that generally form by alteration of primary, magmatic minerals. This alteration process may occur under a variety of environmental conditions, which affect the resulting carbonate phase: its abundance, composition, spatial distribution and the mineral phases it is associated with. Consequently, carbonates keep track of the environmental conditions under which they formed, and in particular, the amount of CO 2 and liquid water involved in their formation. Understanding the history of both water and CO 2 on Mars is critical to better understand the evolution of the red planet and its atmosphere, but also the origin of the water on Earth, and possibly the origin of life. Since the beginning of the Mars2020 mission in Jezero Crater, the SuperCam instrument has analyzed more than 200 rocks of the crater CLAVÉ ET AL.

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Section: Discussionmentioning

confidence: 99%

Carbonate Detection With SuperCam in Igneous Rocks on the Floor of Jezero Crater, Mars

Clavé

Benzerara²,

Meslin

et al. 2023

JGR Planets

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“…Research on in situ plasma and UV spectra monitored during ESD revealed that CO 2 + , CO + , O I , and O 3 are generated in dry CO 2 during the ESD process. The chemical reactions were inferred as follows: (M = Mg or K. Cl I marks the first excited state of the Cl atom, and M* marks the excited cation) normale − + normalM − Cl → Cl normalI + normalM * Cl normalI + ( O I , O II , O 3 ) + normalM * → normalM − ClO 3 MClO 3 + ( O I , O II , O 3 ) → normalM − ClO 4 …”

Section: Resultsmentioning

confidence: 99%

Section: Resultsmentioning

confidence: 99%

Oxychloride Generation by Electrostatic Discharge (ESD) of Martian Dust and Detection by Infrared Spectroscopy

Wang

et al. 2023

ACS Earth Space Chem.

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Stable oxychlorides, mainly composed of ClO4 –, ClO3 –, or their mixture, are significantly enriched on the Martian surface (up to ∼0.5%) compared to Earth. ClO4 – and ClO3 – have different physicochemical properties and biological activities. They are also important candidates for in situ resource utilization (ISRU) and even the food sources of potential Martian lives. Therefore, it is of great scientific significance to determine the species of oxychlorides, especially the ratio of ClO4 –/ClO3 – on the Martian surface, not only for Martian environmental evolution and life search but also for Martian resource development. In this study, first, a simulation of oxychloride generation by electrostatic discharge (ESD) of the Martian dust storm was performed under simulated Martian conditions. Second, the spectral features of the Fourier transform infrared attenuated total reflection (FTIR-ATR) spectra and liquid transmission (FTIR-TR) spectra of ClO4 – and ClO3 – were characterized, and a quantitative model between their IR spectra and their concentrations was built. Finally, the concentration of ClO4 – and ClO3 – in the ESD reaction product under various reaction times and the ratio of ClO4 –/ClO3 – was detected and analyzed. Our results provide valuable information for the study of the origin of the mechanism, the scientific estimation of the abundance and the species of oxychlorides on the Martian surface, and even the feasibility of ISRU on the Martian surface.

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“…Under most circumstances, the present atmosphere of Mars is too tenuous to support lightning. However, electrostatic emissions that affect chemical changes, for example, in the chlorine cycle, have been observed to be associated with recent martian dust storm activity (Ruf et al., 2009; Wang et al., 2023). However, severe lightning storms may have been associated with episodes of explosive volcanism, which are thought to have generated extensive, dynamic eruptive ash clouds (Brož & Hauber, 2012, 2013; Brož et al., 2021; Halevy & Head, 2014; L. Wilson & Head, 1994).…”

Section: Systematic Survey Of Paragenetic Modesmentioning

confidence: 99%

“…(2009); 124 = Wang et al. (2023); 125 = L. Wilson and Head (1994); 126 = Brož et al. (2021); 127 = Tomioka and Miyahara (2017); 128 = Tschauner (2019); 129 = El Goresy et al.…”

Section: Introductionmentioning

confidence: 99%

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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Quantification of Carbonates, Oxychlorines, and Chlorine Generated by Heterogeneous Electrochemistry Induced by Martian Dust Activity

Cited by 7 publications

References 41 publications

Carbonate Detection With SuperCam in Igneous Rocks on the Floor of Jezero Crater, Mars

Carbonate Detection With SuperCam in Igneous Rocks on the Floor of Jezero Crater, Mars

Oxychloride Generation by Electrostatic Discharge (ESD) of Martian Dust and Detection by Infrared Spectroscopy

On the Diversity and Formation Modes of Martian Minerals

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