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Evidence for Low-Grade Metamorphism, Hydrothermal Alteration, and Diagenesis on Mars from Phyllosilicate Mineral Assemblages

Published online by Cambridge University Press:  01 January 2024

Bethany L. Ehlmann ,
John F. Mustard ,
Roger N. Clark ,
Gregg A. Swayze  and
Scott L. Murchie
Bethany L. Ehlmann*
Affiliation:
Institut d’Astrophysique Spatiale, Université Paris-Sud 11, Orsay, 91405, France Department of Geological Sciences, Brown University, Providence, Rhode Island, 02912 USA
John F. Mustard
Affiliation:
Department of Geological Sciences, Brown University, Providence, Rhode Island, 02912 USA
Roger N. Clark
Affiliation:
US Geological Survey, Denver, Colorado, 80225 USA
Gregg A. Swayze
Affiliation:
US Geological Survey, Denver, Colorado, 80225 USA
Scott L. Murchie
Affiliation:
Johns Hopkins University Applied Physics Laboratory, Laurel, Maryland, 20723 USA
*
* E-mail address of corresponding author: ehlmann@gps.caltech.edu
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Abstract

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The enhanced spatial and spectral resolution provided by the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) on the Mars Reconnaissance Orbiter (MRO) has led to the discovery of numerous hydrated silicate minerals on Mars, particularly in the ancient, cratered crust comprising the southern highlands. Phases recently identified using visible/near-infrared spectra include: smectite, chlorite, prehnite, high-charge phyllosilicates (illite or muscovite), the zeolite analcime, opaline silica, and serpentine. Some mineral assemblages represent the products of aqueous alteration at elevated temperatures. Geologic occurrences of these mineral assemblages are described using examples from west of the Isidis basin near the Nili Fossae and with reference to differences in implied temperature, fluid composition, and starting materials during alteration. The alteration minerals are not distributed homogeneously. Rather, certain craters host distinctive alteration assemblages: (1) prehnite-chloritesilica, (2) analcime-silica-Fe,Mg-smectite-chlorite, (3) chlorite-illite (muscovite), and (4) serpentine, which furthermore has been found in bedrock units. These assemblages contrast with the prevalence of solely Fe,Mg-smectites in most phyllosilicate-bearing terrains on Mars, and they represent materials altered at depth then exposed by cratering. Of the minerals found to date, prehnite provides the clearest evidence for subsurface, hydrothermal/metamorphic alteration, as it forms only under highly restricted conditions (T = 200–400°C). Multiple mechanisms exist for forming the other individual minerals; however, the most likely formation mechanisms for the characteristic mineralogic assemblages observed are, for (1) and (2), low-grade metamorphism or hydrothermal (<400°C) circulation of fluids in basalt; for (3), transformation of trioctahedral smectites to chlorite and dioctahedral smectites to illite during diagenesis; and for (4), low-grade metamorphism or hydrothermal (<400°C) circulation of fluids in ultramafic rocks. Evidence for high-grade metamorphism at elevated pressures or temperatures >400°C has not been found.

Keywords

AnalcimeChloriteCratersDiagenesisHydrothermal AlterationIlliteInfrared SpectroscopyMarsMetamorphismMuscovitePhyllosilicatesPrehniteSerpentineSilicaZeolites
Type
Article
Information
Clays and Clay Minerals , Volume 59 , Issue 4 , August 2011 , pp. 359 - 377
Copyright
Copyright © Clay Minerals Society 2011

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