Alteration minerals, fluids, and gases on early Mars: Predictions from 1‐D flow geochemical modeling of mineral assemblages in meteorite <scp>ALH</scp> 84001

Daswani, Mohit Melwani; Schwenzer, S. P.; Reed, Mark H.; Wright, I. P.; Grady, M. M.

doi:10.1111/maps.12713

Cited by 30 publications

(30 citation statements)

References 165 publications

(176 reference statements)

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“…In addition, we compare our results to data for ALH 84001 from Melwani Daswani et al. (), who reacted bulk ALH 84001 host rock in a 1D flow model. Total dissolved solids range from 1.3 × 10 −2 to 4.4 × 10 −2 mole L −1 between W/R 1000 and 100.…”

Section: Discussionmentioning

confidence: 81%

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Fluids during diagenesis and sulfate vein formation in sediments at Gale crater, Mars

Schwenzer

Bridges

Wiens

et al. 2016

Meteorit & Planetary Scien

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Abstract-We model the fluids involved in the alteration processes recorded in the Sheepbed Member mudstones of Yellowknife Bay (YKB), Gale crater, Mars, as revealed by the Mars Science Laboratory Curiosity rover investigations. We compare the Gale crater waters with fluids modeled for shergottites, nakhlites, and the ancient meteorite ALH 84001, as well as rocks analyzed by the Mars Exploration rovers, and with terrestrial ground and surface waters. The aqueous solution present during sediment alteration associated with phyllosilicate formation at Gale was high in Na, K, and Si; had low Mg, Fe, and Al concentrations-relative to terrestrial groundwaters such as the Deccan Traps and other modeled Mars fluids; and had near neutral to alkaline pH. Ca and S species were present in the 10 À3 to 10 À2 concentration range. A fluid local to Gale crater strata produced the alteration products observed by Curiosity and subsequent evaporation of this groundwatertype fluid formed impure sulfate-and silica-rich deposits-veins or horizons. In a second, separate stage of alteration, partial dissolution of this sulfate-rich layer in Yellowknife Bay, or beyond, led to the pure sulfate veins observed in YKB. This scenario is analogous to similar processes identified at a terrestrial site in Triassic sediments with gypsum veins of the Mercia Mudstone Group in Watchet Bay, UK.

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Section: Discussionmentioning

confidence: 81%

“…) and the composition of the clays (e.g., Bridges and Schwenzer ; Melwani Daswani et al. ) indicate that the system was not in contact with the Martian atmosphere at the time of vein formation, and therefore, carbonate precipitation does not need to be considered here.…”

Section: Discussionmentioning

confidence: 99%

Fluids during diagenesis and sulfate vein formation in sediments at Gale crater, Mars

Schwenzer

Bridges

Wiens

et al. 2016

Meteorit & Planetary Scien

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“…; Melwani Daswani et al. ) to the current seasonal changes in the polar caps. The atmosphere of Mars was measured for the first time by the Viking lander (Chamberlain et al.…”

Section: Objective 4: Constrain the Inventory Of Martian Volatiles Asmentioning

confidence: 99%

“…; Melwani Daswani et al. ). Moreover, they were ejected at different times from Mars than the shergottites, which could be important if the atmospheric composition changes on the time scale of millions of years (the time between ejection events) or shorter (Swindle et al.…”

Section: Objective 4: Constrain the Inventory Of Martian Volatiles Asmentioning

confidence: 99%

The potential science and engineering value of samples delivered to Earth by Mars sample return

Beaty¹,

Grady²,

McSween³

et al. 2019

Meteorit & Planetary Scien

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Executive Summary Return of samples from the surface of Mars has been a goal of the international Mars science community for many years. Affirmation by NASA and ESA of the importance of Mars exploration led the agencies to establish the international MSR Objectives and Samples Team (iMOST). The purpose of the team is to re‐evaluate and update the sample‐related science and engineering objectives of a Mars Sample Return (MSR) campaign. The iMOST team has also undertaken to define the measurements and the types of samples that can best address the objectives. Seven objectives have been defined for MSR, traceable through two decades of previously published international priorities. The first two objectives are further divided into sub‐objectives. Within the main part of the report, the importance to science and/or engineering of each objective is described, critical measurements that would address the objectives are specified, and the kinds of samples that would be most likely to carry key information are identified. These seven objectives provide a framework for demonstrating how the first set of returned Martian samples would impact future Martian science and exploration. They also have implications for how analogous investigations might be conducted for samples returned by future missions from other solar system bodies, especially those that may harbor biologically relevant or sensitive material, such as Ocean Worlds (Europa, Enceladus, Titan) and others. Summary of Objectives and Sub‐Objectives for MSR Identified by iMOST This objective is divided into five sub‐objectives that would apply at different landing sites. 1.1 Characterize the essential stratigraphic, sedimentologic, and facies variations of a sequence of Martian sedimentary rocks. 1.2 Understand an ancient Martian hydrothermal system through study of its mineralization products and morphological expression. 1.3 Understand the rocks and minerals representative of a deep subsurface groundwater environment. 1.4 Understand water/rock/atmosphere interactions at the Martian surface and how they have changed with time. 1.5 Determine the petrogenesis of Martian igneous rocks in time and space. This objective has three sub‐objectives: 2.1 Assess and characterize carbon, including possible organic and pre‐biotic chemistry. 2.2 Assay for the presence of biosignatures of past life at sites that hosted habitable environments and could have preserved any biosignatures. 2.3 Assess the possibility that any life forms detected are alive, or were recently alive. Summary of iMOST Findings Several specific findings were identified during the iMOST study. While they are not explicit recommendations, we suggest that they should serve as guidelines for future decision making regarding planning of potential future MSR missions. The samples to be collected by the Mars 2020 (M‐2020) rover will be of sufficient size and quality to address and solve a wide variety of scientific questions. Samples, by definition, are a statistical representation of a larger entity...

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“…The code solves equations of chemical equilibria for aqueous species and minerals constrained by thermodynamic data, mass balance, mass action, and energy balance equations in its database; aqueous solutions are represented with an extended DebyeHückel model (Reed 1982;Spycher and Reed, 1988;Reed 1998;). We have applied CHIM-XPT to a wide variety of post-magmatic, impact-generated and sedimentary alteration systems of mafic host rock compositions (e.g., Schwenzer and Kring, 2009;Bridges and Schwenzer, 2012;Schwenzer et al, 2012;Filiberto and Schwenzer, 2013;Schwenzer and Kring, 2013;Bridges et al, 2015;Melwani Daswani et al, 2016;Schwenzer et al, 2016;), including modelling towards the observed carbonate-phyllosilicate alteration succession in the nakhlite Martian meteorites (Bridges and Schwenzer, 2012).…”

Section: Geochemical Modelingmentioning

confidence: 99%

Serpentinite with and without brucite: A reaction pathway analysis of a natural serpentinite in the Josephine ophiolite, California

Sonzogni

Treiman

Schwenzer

2017

Journal of Mineralogical and Petrological Sciences

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A partially serpentinized peridotite from the Josephine ophiolite has been studied in detail in order to characterize the chemical processes of its serpentinization. The original rock was harzburgite, and its olivine and orthopyroxene are partially replaced by veins and patches of lizardite serpentine and magnetite; brucite and talc are completely absent from the serpentinite, regardless of whether the precursor mineral was olivine or pyroxene. Petrographic and mineral-chemical data suggest at least two phases of serpentinization. Incipient serpentinization produced lizardite and magnetite veinlets, from preferential dissolution of orthopyroxene, and/or infiltration of a silica-rich fluid. No talc or brucite was produced, which suggests this serpentinization happened in a chemically open system. Later serpentinization was from a fluid closer to Fe-Mg-Si chemical equilibrium with the harzburgite, which should in theory favor formation of a brucite-bearing serpentinite. Brucite is absent from late serpentine veins, but they have some porosity which could represent former brucite that was dissolved out or was reacted out after serpentinization. Isocon modeling suggests that Si, Fe, and K were added during serpentinization and that Ca was lost; i.e., the serpentinization was not isochemical (except for H 2 O). Results of petrographic observations, thermodynamic modeling, and mass balance calculations were used to constrain the reactions for global serpentinization of the studied sample. These reactions indicate that water with a concentration of H 2 up to two times that of deep sea vent fluids may have been produced during the serpentinization of the Josephine peridotite, which could then have been a potential host for significant biomass.

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Alteration minerals, fluids, and gases on early Mars: Predictions from 1‐D flow geochemical modeling of mineral assemblages in meteorite ALH 84001

Cited by 30 publications

References 165 publications

Fluids during diagenesis and sulfate vein formation in sediments at Gale crater, Mars

Fluids during diagenesis and sulfate vein formation in sediments at Gale crater, Mars

The potential science and engineering value of samples delivered to Earth by Mars sample return

Serpentinite with and without brucite: A reaction pathway analysis of a natural serpentinite in the Josephine ophiolite, California

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