Elemental Composition of the Martian Crust

McSween, H. Y.; Taylor, G. J.; Wyatt, M. B.

doi:10.1126/science.1165871

Cited by 392 publications

(284 citation statements)

References 29 publications

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“…Herd et al 2002;Wadhwa 2008). Nevertheless, in the case of Mars, the composition of basaltic SNC meteorites, from which such reducing conditions are inferred, differs from that of old surface basalts found in the Gusev crater that require a more oxidized source instead (McSween et al 2009). An explanation for this discrepancy is that meteorites and surface rocks formed from melting and crystallization of the same source but under different f O 2 conditions (Tuff et al 2013).…”

Section: Outgassing Of Comentioning

confidence: 96%

The habitability of a stagnant-lid Earth

Tosi

Godolt

Stracke

et al. 2017

A&A

126

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Context. Plate tectonics is considered a fundamental component for the habitability of the Earth. Yet whether it is a recurrent feature of terrestrial bodies orbiting other stars or unique to the Earth is unknown. The stagnant lid may rather be the most common tectonic expression on such bodies. Aims. To understand whether a stagnant-lid planet can be habitable, i.e. host liquid water at its surface, we model the thermal evolution of the mantle, volcanic outgassing of H 2 O and CO 2 , and resulting climate of an Earth-like planet lacking plate tectonics. Methods. We used a 1D model of parameterized convection to simulate the evolution of melt generation and the build-up of an atmosphere of H 2 O and CO 2 over 4.5 Gyr. We then employed a 1D radiative-convective atmosphere model to calculate the global mean atmospheric temperature and the boundaries of the habitable zone (HZ).Results. The evolution of the interior is characterized by the initial production of a large amount of partial melt accompanied by a rapid outgassing of H 2 O and CO 2 . The maximal partial pressure of H 2 O is limited to a few tens of bars by the high solubility of water in basaltic melts. The low solubility of CO 2 instead causes most of the carbon to be outgassed, with partial pressures that vary from 1 bar or less if reducing conditions are assumed for the mantle to 100-200 bar for oxidizing conditions. At 1 au, the obtained temperatures generally allow for liquid water on the surface nearly over the entire evolution. While the outer edge of the HZ is mostly influenced by the amount of outgassed CO 2 , the inner edge presents a more complex behaviour that is dependent on the partial pressures of both gases. Conclusions. At 1 au, the stagnant-lid planet considered would be regarded as habitable. The width of the HZ at the end of the evolution, albeit influenced by the amount of outgassed CO 2 , can vary in a non-monotonic way depending on the extent of the outgassed H 2 O reservoir. Our results suggest that stagnant-lid planets can be habitable over geological timescales and that joint modelling of interior evolution, volcanic outgassing, and accompanying climate is necessary to robustly characterize planetary habitability.

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Section: Outgassing Of Comentioning

confidence: 96%

The habitability of a stagnant-lid Earth

Tosi

Godolt

Stracke

et al. 2017

A&A

126

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“…The composition of Martian basalts was obtained from global remote sensing observations [ Hamilton and Christensen , 1997; Bandfield et al ., 2000; McSween et al ., 2009]. Although shergottites and in situ chemical data (MER and MSL) are available, those likely represent local assemblages.…”

Section: Geochemical Settingmentioning

confidence: 99%

“…And second, because equilibrium models do not take into account the role of reactive surface area in determining the differences on crystallization pathways from small‐to‐large sediment particle sizes (kinetic models are needed to accomplish this objective). To help solve this problem, we have applied a reactive‐transport approach to model the formation of mineral sequences known to exist on Mars, as described from lander and orbiter data [e.g., Hamilton and Christensen , 1997; Bandfield et al ., 2000; Mustard et al ., 2008; McSween et al ., 2009; Ehlmann et al ., 2011; Vaniman et al ., 2014; Rampe et al ., 2017; Hurowitz et al ., 2017], considering open system conditions both at the atmosphere‐water and water‐rock interfaces and implementing a kinetic approach for the dissolution and precipitation of solid phases. We present a suite of models representing aqueous environments in systems under an early Mars atmosphere, to analyze the role of (i) the reactive surface area of primary minerals; (ii) the reactive transport processes through the basalt interface; and (iii) the cation adsorption by the surface of clays.…”

Section: Introductionmentioning

confidence: 99%

Mineral paragenesis on Mars: The roles of reactive surface area and diffusion

et al. 2017

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Geochemical models of secondary mineral precipitation on Mars generally assume semiopen systems (open to the atmosphere but closed at the water‐sediment interface) and equilibrium conditions. However, in natural multicomponent systems, the reactive surface area of primary minerals controls the dissolution rate and affects the precipitation sequences of secondary phases, and simultaneously, the transport of dissolved species may occur through the atmosphere‐water and water‐sediment interfaces. Here we present a suite of geochemical models designed to analyze the formation of secondary minerals in basaltic sediments on Mars, evaluating the role of (i) reactive surface areas and (ii) the transport of ions through a basalt sediment column. We consider fully open conditions, both to the atmosphere and to the sediment, and a kinetic approach for mineral dissolution and precipitation. Our models consider a geochemical scenario constituted by a basin (i.e., a shallow lake) where supersaturation is generated by evaporation/cooling and the starting point is a solution in equilibrium with basaltic sediments. Our results show that cation removal by diffusion, along with the input of atmospheric volatiles and the influence of the reactive surface area of primary minerals, plays a central role in the evolution of the secondary mineral sequences formed. We conclude that precipitation of evaporites finds more restrictions in basaltic sediments of small grain size than in basaltic sediments of greater grain size.

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“…Since the surface of Mars is largely volcanic (McSween et al, 2009), evidence for hydrothermal activity lies in the alteration products and element mobility patterns produced when hydrothermal fluids interact with volcanic materials. Geochemical and mineralogical evidence can help distinguish hydrothermal from ambient temperature fluid-rock interaction, which can help reconstruct potentially habitable environments.…”

Section: Background: Mars Hydrothermal Alterationmentioning

confidence: 99%

Lassen Volcanic Fumaroles and Hot Springs: Analog for Mars

McHenry

Gerard

Walters

2014

Proc. Wisc. Space Conf.

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We are conducting a pilot study on the hydrothermal alteration of lavas at Lassen Volcanic National Park as an analog for potential hydrothermal deposits on Mars. Lassen has hot springs and fumaroles that have altered its lavas into silica, sulfates, and phyllosilicates, all mineral types also identified on Mars. Hydrothermal environments were likely common on Mars (due to evidence of early aqueous and a long record of volcanic activity), and such environments could have remained habitable long after the surface cooled and desiccated. However, some hydrothermal environments are more habitable than others, and being able to distinguish between the deposits of hostile acid-sulfate fumarole and more accommodating near-neutral hot spring environments can provide clues to habitability. Lassen hydrothermal environments produce silica by both acid-sulfate leaching and precipitation from neutral hydrothermal waters, both of which have been suggested as potential origins for deposits in Columbia Hills of Gusev Crater on Mars. ObjectivesThe objectives of this study are to:1. Determine the mineralogical and geochemical patterns of lava alteration associated with acid-sulfate leaching at Lassen hot springs and fumaroles, and contrast them with the patterns associated with more neutral, Cl-rich hydrothermal fluids at fumaroles and hot springs within Lassen park. 2. Compare these results to the mineralogy and geochemistry of hydrothermal deposits observed in the Columbia Hills of Gusev Crater, and determine if either scenario is more consistent with the observations. 3. Determine what mineralogical and geochemical evidence for hydrothermal alteration is most likely to be preserved in the rock record by analyzing samples from the hydrothermally altered lavas of Pleistocene Brokeoff Volcano (in Lassen park) and comparing them to samples from the active fields.

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Elemental Composition of the Martian Crust

Cited by 392 publications

References 29 publications

The habitability of a stagnant-lid Earth

The habitability of a stagnant-lid Earth

Mineral paragenesis on Mars: The roles of reactive surface area and diffusion

Lassen Volcanic Fumaroles and Hot Springs: Analog for Mars

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