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

Schwenzer, S. P.; Bridges, J. C.; Wiens, R. C.; Conrad, Pamela G.; Kelley, Simon P.; Léveillé, Richard; Mangold, N.; Martín‐Torres, Javier; McAdam, A. C.; Newsom, H. E.; Zorzano, María Paz; Rapin, W.; Spray, John G.; Treiman, Allan H.; Westall, Francès; Fairén, Alberto González; Meslin, Pierre‐Yves

doi:10.1111/maps.12668

Cited by 61 publications

(88 citation statements)

References 119 publications

(195 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Their formation requires enrichment of dissolved species—by freezing or evaporation—in fractures of the rock. Because this work focuses on the clay formation, detailed modeling of the last stage is beyond the scope of this work and discussed elsewhere [ Schwenzer et al ., , and in preparation].…”

Section: Discussionmentioning

confidence: 99%

Diagenesis and clay mineral formation at Gale Crater, Mars

et al. 2015

Self Cite

View full text Add to dashboard Cite

The Mars Science Laboratory rover Curiosity found host rocks of basaltic composition and alteration assemblages containing clay minerals at Yellowknife Bay, Gale Crater. On the basis of the observed host rock and alteration minerals, we present results of equilibrium thermochemical modeling of the Sheepbed mudstones of Yellowknife Bay in order to constrain the formation conditions of its secondary mineral assemblage. Building on conclusions from sedimentary observations by the Mars Science Laboratory team, we assume diagenetic, in situ alteration. The modeling shows that the mineral assemblage formed by the reaction of a CO2-poor and oxidizing, dilute aqueous solution (Gale Portage Water) in an open system with the Fe-rich basaltic-composition sedimentary rocks at 10–50°C and water/rock ratio (mass of rock reacted with the starting fluid) of 100–1000, pH of ∽7.5–12. Model alteration assemblages predominantly contain phyllosilicates (Fe-smectite, chlorite), the bulk composition of a mixture of which is close to that of saponite inferred from Chemistry and Mineralogy data and to that of saponite observed in the nakhlite Martian meteorites and terrestrial analogues. To match the observed clay mineral chemistry, inhomogeneous dissolution dominated by the amorphous phase and olivine is required. We therefore deduce a dissolving composition of approximately 70% amorphous material, with 20% olivine, and 10% whole rock component.

show abstract

Section: Discussionmentioning

confidence: 99%

Diagenesis and clay mineral formation at Gale Crater, Mars

et al. 2015

Self Cite

View full text Add to dashboard Cite

show abstract

“…; Schwenzer et al. ). More than 50% of detected Martian clay minerals and the majority of zeolite detections are associated with impact structures (Carter et al.…”

Section: Introductionmentioning

confidence: 97%

Experimental hydrothermal alteration of basaltic glass with relevance to Mars

Sætre

Hellevang

Riu

et al. 2018

Meteorit & Planetary Scien

View full text Add to dashboard Cite

Phyllosilicates, carbonates, zeolites, and sulfates on Mars give clues about the planet's past environmental conditions, but little is known about the specific conditions in which these minerals formed within the crust and at the surface. The aim of the present study was to gain increased understanding on the formation of secondary phases by hydrothermal alteration of basaltic glass. The reaction processes were studied under varying conditions (temperature, pCO2, water:rock ratio, and fluid composition) with relevance to aqueous hydrothermal alteration in fully and partly saturated Martian basalt deposits. Analyses made on reaction products using X‐ray diffraction (XRD) and scanning electron microscope (SEM) were compared with near infrared spectroscopy (NIR) to establish relative detectability and spectral signatures. This study demonstrates that comparable alteration minerals (phyllosilicates, carbonates, zeolites) form from vapor condensing on mineral surfaces in unsaturated sediments and not only in fully water‐saturated sediments. In certain environments where water vapor might be present, it can alter the basaltic bedrock to a suite of authigenic phases similar to those observed on the Martian surface. For the detection of the secondary phases, XRD and SEM‐EDS were found to be superior to NIR for detecting and characterizing zeolites. The discrepancy in detectability of zeolites between NIR and XRD/SEM‐EDS might indicate that zeolites on Mars are more abundant than previously thought.

show abstract

“…A number of thermochemical studies predicted the formation of alteration minerals from basaltic and ultramafic protoliths, predominantly in hydrothermal or diagenetic contexts (Bridges & Schwenzer, ; Filiberto & Schwenzer, ; Griffith & Shock, ; Schwenzer et al, ; Schwenzer & Kring, , ; Zolotov & Mironenko, ), but focused on temperatures below 300 °C, relatively high water to rock ratios, and pressures equivalent to less than 10 km in crustal depth. Petrogenetic grids for terrestrial mafic and ultramafic rocks have been used to help recognize low‐grade metamorphic assemblages (Ehlmann et al, ; Viviano et al, ) and for plotting Martian whole‐rock compositions (McSween et al, ).…”

Section: Introductionmentioning

confidence: 99%

Phase Equilibria Modeling of Low‐Grade Metamorphic Martian Rocks

et al. 2019

Self Cite

View full text Add to dashboard Cite

Hydrous phases have been identified to be a significant component of Martian mineralogy. Particularly, prehnite, zeolites, and serpentine are evidence for low‐grade metamorphic reactions at elevated temperatures in mafic and ultramafic protoliths. Their presence suggests that at least part of the Martian crust is sufficiently hydrated for low‐grade metamorphic reactions to occur. A detailed analysis of changes in mineralogy with variations in fluid content and composition along possible Martian geotherms can contribute to determine the conditions required for subsurface hydrous alteration, fluid availability, and rock properties in the Martian crust. In this study, we use phase equilibria models to explore low‐grade metamorphic reactions covering a pressure‐temperature range of 0–0.5 GPa and 150–450 °C for several Martian protolith compositions and varying fluid content. Our models replicate the detected low‐grade metamorphic/hydrothermal mineral phases like prehnite, chlorite, analcime, unspecified zeolites, and serpentine. Our results also suggest that actinolite should be a part of lower‐grade metamorphic assemblages, but actinolite may not be detected in reflectance spectra for several reasons. By gradually increasing the water content in the modeled whole‐rock composition, we can estimate the amount of water required to precipitate low‐grade metamorphic phases. Mineralogical constraints do not necessarily require an elevated geothermal gradient for the formation of prehnite. However, restricted crater excavation depths even for large impact craters are not likely sampling prehnite along colder gradients, suggesting either a geotherm of ~20 °C/km in the Noachian or an additional heat source such as hydrothermal or magmatic activity.

show abstract

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

Cited by 61 publications

References 119 publications

Diagenesis and clay mineral formation at Gale Crater, Mars

Diagenesis and clay mineral formation at Gale Crater, Mars

Experimental hydrothermal alteration of basaltic glass with relevance to Mars

Phase Equilibria Modeling of Low‐Grade Metamorphic Martian Rocks

Contact Info

Product

Resources

About