A Review of the Phyllosilicates in Gale Crater as Detected by the CheMin Instrument on the Mars Science Laboratory, Curiosity Rover

Tu, V.; Rampe, E. B.; Bristow, T. F.; Thorpe, M. T.; Clark, J. V.; Castle, N.; Fraeman, Abigail A.; Edgar, Lauren A.; McAdam, A. C.; Bedford, C. C.; Achilles, C. N.; Blake, D. F.; Chipera, S. J.; Craig, P. I.; Marais, David J. Des; Downs, G. W.; Downs, Robert T.; Fox, V. K.; Grotzinger, J. P.; Hazen, Robert M.; Ming, D. W.; Morris, R. V.; Morrison, S. M.; Pavri, B.; Eigenbrode, J. L.; Peretyazhko, T. S.; Sarrazin, P.; Sutter, B.; Treiman, Allan H.; Vaniman, David T.; Vasavada, A. R.; Yen, A. S.; Bridges, John C.

doi:10.3390/min11080847

Cited by 31 publications

(30 citation statements)

References 144 publications

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“…For some reflections (e.g., 02 l ) the d values are nearly independent of desiccation state because their values are non‐ or weakly dependent on the interlayer spacing. Smectite‐bearing samples acquired by Curiosity and measured by CheMin within Glen Torridon were quantitatively modeled with a least squares fitting procedure (Reitveld refinement) using laboratory transmission XRD overlay patterns for fully collapsed smectites as represented in Figure 23 by SWa‐1_des and Garfield_des (Bristow et al., 2021; Rampe et al., 2020; Thorpe et al., 2022; Tu et al., 2021). Taking CRISM spectral and CheMin XRD data together, we conclude that Jura ferric‐rich smectite at unit RU_a (Jura member) is either (1) fully desiccated and the relatively weak H 2 O spectral feature at 1.92 μm results from another phase or adsorbed H 2 O or (2) is substantially desiccated and the 1.92 μm spectral feature results from residual interlayer H 2 O at concentrations not detectable by CheMin XRD.…”

Section: Spectral Identification Of Desiccated Nontronitementioning

confidence: 99%

Surface Kinetic Temperatures and Nontronite Single Scattering Albedo Spectra From Mars Reconnaissance Orbiter CRISM Hyperspectral Imaging Data Over Glen Torridon, Gale Crater, Mars

Arvidson

O’Sullivan

et al. 2022

JGR Planets

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The Mars Reconnaissance Orbiter Compact Imaging Spectrometer for Mars (CRISM) covers the spectral range from 0.362 to 3.92 μm with a midafternoon local solar time data acquisition. For equatorial to midlatitudes, depending on the season and surface materials, wavelengths longer than ∼2.65 μm exhibit spectral radiances on sensor that include sunlight and thermal‐emission related terms. We developed a radiative transfer based neural network approach to model both solar and emitted terms in which surface kinetic temperatures are retrieved for each image pixel, together with single scattering albedo spectra, over the full CRISM wavelength range. We applied the method to along‐track oversampled scene FRT00021C92 over Glen Torridon within Gale Crater, where the Curiosity rover traversed and acquired remote sensing and in‐situ data. Synergistic analysis of orbital and rover‐based data, coupled with laboratory analyses of ferric‐rich smectites, provide a self‐consistent set of results for the presence of desiccated nontronite associated with Murray formation mudstones exposed as periodic bedrock ridges located just to the south of Vera Rubin ridge. The desiccated nature is consistent with Curiosity's CheMin data, which for Glen Torridon drill samples indicate an abundance of nontronite having a collapsed structure resulting from loss of interlayer H2O.

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Section: Spectral Identification Of Desiccated Nontronitementioning

confidence: 99%

Surface Kinetic Temperatures and Nontronite Single Scattering Albedo Spectra From Mars Reconnaissance Orbiter CRISM Hyperspectral Imaging Data Over Glen Torridon, Gale Crater, Mars

Arvidson

O’Sullivan

et al. 2022

JGR Planets

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“…Mars (SAM) evolved gas analyses (EGAs) revealed the temperature of volatiles (particularly H 2 O) from minerals. 30,44 The data from Curiosity had confirmed the existence of abundant MCMs 15 and distinguished clay minerals and sulfates and oxides at several sites inside Gale Crater. 30 The 2:1 clay minerals have been identified by CheMin data with Co Kα radiation particularly in the 8−11°2θ(12−9.4 Å) (Figure 4).…”

Section: Detection Of Clay Minerals Bymentioning

confidence: 88%

“…28 The interplanar spacing d 001 = 9.6 Å has also been observed in the Highfield and Rockhall samples. 44 Generally, a single instrumental analysis cannot result in definite and convincing conclusion data on clay minerals on Mars. VNIR spectra from the Mars orbiter suggest that qualitatively there are a variety of MCMs, but their amount is uncertain.…”

Section: Detection Of Clay Minerals Bymentioning

confidence: 99%

“…Compared with the VNIR spectroscope equipped on OMEGA and CRISM, the instruments on rovers can provide more data to determine MCMs mineralogically and chemically. 44,47 The Mossbauer spectrometry is particularly sensitive to Febearing phases. The data from the Mossbauer spectrometer on the Spirit and Opportunity rovers identify Fe-bearing minerals, such as olivine, pyroxene, hematite, and magnetite and their distribution in the Gusev crater and Meridiani Planum.…”

Section: Detection Of Clay Minerals Bymentioning

confidence: 99%

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Enigmatic Issues and Widening Implications of Research on Martian Clay Minerals

Zhong

Fiore

Chen

et al. 2022

ACS Earth Space Chem.

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Clay minerals are widespread in the Martian crust. Over the last few decades, accumulating data and research into the type, crystallinity, quantity, and distribution of Martian clay minerals (MCMs) has remarkably advanced the understanding of Martian geology, paleoclimate, environment, and the question of whether water, organic matter, and life exist there. Meanwhile, some issues remain enigmatic and arguable. To date, mineralogical data from orbiters and rovers have provided information regarding the distribution, composition, age, and geological evolution of MCMs. Several models for interpreting the formation of MCMs, including weathering, hydrothermal alteration, magmatic precipitation, and diagenesis, have been proposed. Nevertheless, the exact formation mechanism of MCM, remains unclear, primarily because of the lack of sufficient information on the chemical reactions and element cycles involved in the formation of clay minerals. Examination on the type, crystallinity, quantity, and distribution of MCMs indicates that Mars possibly had a warm and wet climate during the Noachian period. Since clay minerals possess abundant −OH groups in the layered structure and can host H 2 O in the interlayer space, MCMs are thought to be potentially large water reservoirs. Studies of MCMs and their interaction with organic matter are possibly conducive to finding answers to the question of whether or not on Mars life exists as clay minerals can preserve and enrich organic matter, catalyze the formation of biotic molecules, such as RNA oligomers, ribose, and amino acids, and even contribute to the assembly of vesicles. Future missions to Mars are recommended to set studies on MCMs with the key issues above and are expecting to lead to more exciting findings.

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“…Among the abundant alteration phases that have been detected on Mars from orbit (e.g., Bibring et al, 2006; Ehlmann & Edwards, 2014; Lasue et al, 2019; Mustard, 2019), at every landing site (e.g., Bristow et al., 2018; Jolliff et al, 2019; Kounaves & Oberlin, 2019; Mittlefehldt et al, 2019; Sutter et al, 2019; Rampe et al., 2020; Tu et al, 2021), and in Martian meteorites (e.g., Bridges et al, 2019; Filiberto et al, 2014; Giesting & Filiberto, 2016; McCubbin et al, 2013; Sautter et al, 2006), hydrous minerals such as prehnite, serpentine, epidote, and zeolites—spectrally observed from orbital measurements—are indicative of low‐grade metamorphic conditions (Ehlmann et al, 2009, 2011; McSween et al, 2015; Viviano et al, 2013). Phase diagram and thermodynamic modeling studies suggest that these minerals formed at elevated temperatures (>150 °C) either along a normal geothermal gradient or as a result of impact‐ or volcanic‐induced hydrothermal systems (McSween et al, 2015; Schwenzer & Kring, 2013; Semprich et al, 2019).…”

Section: Introductionmentioning

confidence: 99%

Constraints on the formation of carbonates and low‐grade metamorphic phases in the Martian crust as a function of H₂O‐CO₂ fluids

Semprich

Filiberto

Treiman

et al. 2021

Meteorit & Planetary Scien

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Low-grade metamorphic hydrous minerals and carbonates occur in various settings on Mars and in Martian meteorites. We present constraints on the stability of prehnite, zeolites, serpentine, and carbonates by modeling the influence of H 2 O-CO 2 fluids during low-grade metamorphism in the Martian crust using compositions of a Martian basalt and an ultramafic cumulate. In basaltic compositions with 5 wt% fluid, our models predict prehnite in less oxidized, CO 2 -poor conditions (≤0.44 mol kg À1 CO 2 ) on warmer geotherms of 20 °C km À1 . At fluid-saturated conditions, epidote and laumontite are replaced by quartz, calcite, chlorite, and muscovite. In ultramafic compositions with 5 wt% fluid, antigorite (serpentine) is stable at CO 2 -poor conditions of ≤0.33 mol kg À1 , while talc forms at 0.05-0.56 mol kg À1 CO 2 . At fluid-saturated conditions, antigorite is replaced by talc and chlorite, and at higher X(CO 2 ) by magnesite and quartz. Our models therefore suggest that prehnite, zeolites, and serpentine have formed in a CO 2 -poor environment on Mars implying that fluids during their formation either did not contain high amounts of CO 2 or had degassed CO 2 . Carbonates and potentially talc would have formed in the presence of a CO 2 -bearing fluid and therefore at different alteration stages than for prehnite, zeolites, and serpentine either in the same hydrothermal event during which the fluid composition changed gradually due to cooling and precipitation or by separate and successive alteration events with fluids of different compositions.

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A Review of the Phyllosilicates in Gale Crater as Detected by the CheMin Instrument on the Mars Science Laboratory, Curiosity Rover

Cited by 31 publications

References 144 publications

Surface Kinetic Temperatures and Nontronite Single Scattering Albedo Spectra From Mars Reconnaissance Orbiter CRISM Hyperspectral Imaging Data Over Glen Torridon, Gale Crater, Mars

Surface Kinetic Temperatures and Nontronite Single Scattering Albedo Spectra From Mars Reconnaissance Orbiter CRISM Hyperspectral Imaging Data Over Glen Torridon, Gale Crater, Mars

Enigmatic Issues and Widening Implications of Research on Martian Clay Minerals

Constraints on the formation of carbonates and low‐grade metamorphic phases in the Martian crust as a function of H₂O‐CO₂ fluids

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A Review of the Phyllosilicates in Gale Crater as Detected by the CheMin Instrument on the Mars Science Laboratory, Curiosity Rover

Cited by 31 publications

References 144 publications

Surface Kinetic Temperatures and Nontronite Single Scattering Albedo Spectra From Mars Reconnaissance Orbiter CRISM Hyperspectral Imaging Data Over Glen Torridon, Gale Crater, Mars

Surface Kinetic Temperatures and Nontronite Single Scattering Albedo Spectra From Mars Reconnaissance Orbiter CRISM Hyperspectral Imaging Data Over Glen Torridon, Gale Crater, Mars

Enigmatic Issues and Widening Implications of Research on Martian Clay Minerals

Constraints on the formation of carbonates and low‐grade metamorphic phases in the Martian crust as a function of H2O‐CO2 fluids

Contact Info

Product

Resources

About

Constraints on the formation of carbonates and low‐grade metamorphic phases in the Martian crust as a function of H₂O‐CO₂ fluids