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      Evidence for Multiple Diagenetic Episodes in Ancient Fluvial‐Lacustrine Sedimentary Rocks in Gale Crater, Mars

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          Abstract

          The Curiosity rover's exploration of rocks and soils in Gale crater has provided diverse geochemical and mineralogical data sets, underscoring the complex geological history of the region. We report the crystalline, clay mineral, and amorphous phase distributions of four Gale crater rocks from an 80‐m stratigraphic interval. The mineralogy of the four samples is strongly influenced by aqueous alteration processes, including variations in water chemistries, redox, pH, and temperature. Localized hydrothermal events are evidenced by gray hematite and maturation of amorphous SiO 2 to opal‐CT. Low‐temperature diagenetic events are associated with fluctuating lake levels, evaporative events, and groundwater infiltration. Among all mudstones analyzed in Gale crater, the diversity in diagenetic processes is primarily captured by the mineralogy and X‐ray amorphous chemistry of the drilled rocks. Variations indicate a transition from magnetite to hematite and an increase in matrix‐associated sulfates suggesting intensifying influence from oxic, diagenetic fluids upsection. Furthermore, diagenetic fluid pathways are shown to be strongly affected by unconformities and sedimentary transitions, as evidenced by the intensity of alteration inferred from the mineralogy of sediments sampled adjacent to stratigraphic contacts.

          Key Points

          • CheMin‐determined mineralogy indicates pervasive low‐temperature diagenesis and localized hydrothermal alteration events at Gale crater

          • The diagenetic history of Gale crater is characterized by a diverse range in fluid chemistry, Eh, pH, and temperature

          • The distribution of SiO 2 and FeO T among crystalline and amorphous materials constrains the temperature and duration of diagenesis

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          Most cited references96

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          Global mineralogical and aqueous mars history derived from OMEGA/Mars Express data.

          Global mineralogical mapping of Mars by the Observatoire pour la Mineralogie, l'Eau, les Glaces et l'Activité (OMEGA) instrument on the European Space Agency's Mars Express spacecraft provides new information on Mars' geological and climatic history. Phyllosilicates formed by aqueous alteration very early in the planet's history (the "phyllocian" era) are found in the oldest terrains; sulfates were formed in a second era (the "theiikian" era) in an acidic environment. Beginning about 3.5 billion years ago, the last era (the "siderikian") is dominated by the formation of anhydrous ferric oxides in a slow superficial weathering, without liquid water playing a major role across the planet.
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            A habitable fluvio-lacustrine environment at Yellowknife Bay, Gale crater, Mars.

            The Curiosity rover discovered fine-grained sedimentary rocks, which are inferred to represent an ancient lake and preserve evidence of an environment that would have been suited to support a martian biosphere founded on chemolithoautotrophy. This aqueous environment was characterized by neutral pH, low salinity, and variable redox states of both iron and sulfur species. Carbon, hydrogen, oxygen, sulfur, nitrogen, and phosphorus were measured directly as key biogenic elements; by inference, phosphorus is assumed to have been available. The environment probably had a minimum duration of hundreds to tens of thousands of years. These results highlight the biological viability of fluvial-lacustrine environments in the post-Noachian history of Mars.
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              Subsurface water and clay mineral formation during the early history of Mars.

              Clay minerals, recently discovered to be widespread in Mars's Noachian terrains, indicate long-duration interaction between water and rock over 3.7 billion years ago. Analysis of how they formed should indicate what environmental conditions prevailed on early Mars. If clays formed near the surface by weathering, as is common on Earth, their presence would indicate past surface conditions warmer and wetter than at present. However, available data instead indicate substantial Martian clay formation by hydrothermal groundwater circulation and a Noachian rock record dominated by evidence of subsurface waters. Cold, arid conditions with only transient surface water may have characterized Mars's surface for over 4 billion years, since the early-Noachian period, and the longest-duration aqueous, potentially habitable environments may have been in the subsurface.
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                Author and article information

                Contributors
                cherie.n.achilles@nasa.gov
                Journal
                J Geophys Res Planets
                J Geophys Res Planets
                10.1002/(ISSN)2169-9100
                JGRE
                Journal of Geophysical Research. Planets
                John Wiley and Sons Inc. (Hoboken )
                2169-9097
                2169-9100
                13 August 2020
                August 2020
                : 125
                : 8 ( doiID: 10.1002/jgre.v125.8 )
                : e2019JE006295
                Affiliations
                [ 1 ] NASA Goddard Space Flight Center Greenbelt MD USA
                [ 2 ] NASA Johnson Space Center Houston TX USA
                [ 3 ] Department of Geosciences University of Arizona Tucson AZ USA
                [ 4 ] NASA Ames Research Center Moffett Field CA USA
                [ 5 ] Planetary Science Institute Tucson AZ USA
                [ 6 ] Jet Propulsion Laboratory California Institute of Technology Pasadena CA USA
                [ 7 ] Jacobs at NASA Johnson Space Center Houston TX USA
                [ 8 ] Department of Earth and Planetary Sciences University of Tennessee, Knoxville Knoxville TN USA
                [ 9 ] Department of Earth Sciences University of New Brunswick Fredericton New Brunswick Canada
                [ 10 ] Department of Physics University of Guelph Guelph Ontario Canada
                [ 11 ] Carnegie Institute for Science Washington DC USA
                [ 12 ] Lunar and Planetary Institute Houston TX USA
                [ 13 ] School of Earth and Space Exploration Arizona State University Tempe AZ USA
                [ 14 ] Chesapeake Energy Oklahoma City OK USA
                [ 15 ] Division of Geological and Planetary Sciences California Institute of Technology Pasadena CA USA
                [ 16 ] SETI Institute Mountain View CA USA
                Author notes
                [*] [* ] Correspondence to:

                C. N. Achilles,

                cherie.n.achilles@ 123456nasa.gov

                Author information
                https://orcid.org/0000-0001-9185-6768
                https://orcid.org/0000-0002-6999-0028
                https://orcid.org/0000-0002-8380-7728
                https://orcid.org/0000-0001-6725-0555
                https://orcid.org/0000-0003-0567-8876
                https://orcid.org/0000-0003-1413-4002
                https://orcid.org/0000-0001-7661-2626
                https://orcid.org/0000-0003-2410-0412
                https://orcid.org/0000-0001-9120-2991
                https://orcid.org/0000-0002-3036-170X
                https://orcid.org/0000-0002-2626-1132
                https://orcid.org/0000-0001-5818-9123
                https://orcid.org/0000-0002-5444-952X
                https://orcid.org/0000-0001-7928-834X
                https://orcid.org/0000-0002-1712-8057
                https://orcid.org/0000-0002-8073-2839
                https://orcid.org/0000-0002-9767-4153
                https://orcid.org/0000-0003-4163-8644
                https://orcid.org/0000-0003-4080-4997
                https://orcid.org/0000-0002-1235-9016
                https://orcid.org/0000-0002-6827-5831
                https://orcid.org/0000-0001-5533-6490
                Article
                JGRE21422 2019JE006295
                10.1029/2019JE006295
                7507756
                32999799
                26a63e49-f298-4745-bb63-68c53d0eb901
                ©2020. The Authors.

                This is an open access article under the terms of the http://creativecommons.org/licenses/by/4.0/ License, which permits use, distribution and reproduction in any medium, provided the original work is properly cited.

                History
                : 02 December 2019
                : 17 June 2020
                : 22 June 2020
                Page count
                Figures: 10, Tables: 2, Pages: 20, Words: 9448
                Funding
                Funded by: National Aeronautics and Space Administration (NASA) , open-funder-registry 10.13039/100000104;
                Award ID: NNX16AL41H
                Categories
                Mineralogy and Petrology
                Planetary Mineralogy and Petrology
                Planetary Sciences: Solid Surface Planets
                Composition
                Research Article
                Research Articles
                Custom metadata
                2.0
                August 2020
                Converter:WILEY_ML3GV2_TO_JATSPMC version:5.9.1 mode:remove_FC converted:22.09.2020

                mineralogy,diagenesis,mars,xrd
                mineralogy, diagenesis, mars, xrd

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