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Evidence for Partially Chloritized Smectite in Gale Crater, Mars, and Implications for DiagenesisPhyllosilicates are an important mineral group found in ancient (~3.5-4.1 Gyr old) martian terrains because they are a marker of water-rock interactions and can help constrain aqueous conditions (e.g., pH, salinity, temperature) and, thus, identify habitable environments. Orbital visible/short-wave infrared (VSWIR) data demonstrate that smectite is the most abundant type of phyllosilicate on Mars, followed by chlorite [e.g., 1]. The geologic settings in which phyllosilicates are found provide important clues into their formation. Smectite has been identified in abundances of up to ~30 wt.% in early Hesperian-aged fluvial-lacustrine sedimentary rocks in Gale crater using the CheMin X-ray diffractometer on the Mars Science Laboratory Curiosity rover [e.g., 2-6]. CheMin XRD patterns and evolved water measured by the Sample Analysis at Mars (SAM) instrument suite show the structure of smectite changes from trioctahedral Fe(II)-bearing smectite at the base of the section to dioctahedral nontronite and montmorillonite ~400 m up section in the Glen Torridon valley where orbital VSWIR show evidence of Fe/Mg smectite. Most of the smectite identified by CheMin is collapsed (i.e., lacking substantial interlayer H2O) based on basal spacings at 10 Å. Fe(II) saponite found in two drill targets at the base of the section in Yellowknife Bay, however, suggest the smectite is expanded. The XRD pattern of the “Cumberland” drill target has a peak at 13.5 Å, whereas the “John Klein” drill target has a peak at 10 Å and a shoulder extending to higher d-spacings (Fig. 1) [2]. A possible explanation for this expanded structure is partial chloritization of the interlayer site caused by the precipitation of small domains of brucite-like sheets [e.g., 7,8]. Here, we synthesize smectite with different degrees of chloritization and analyze the products via XRD, evolved gas analysis (EGA), and VSWIR to determine whether chloritized smectite on Mars can be recognized with these techniques.
Document ID
20240000623
Acquisition Source
Johnson Space Center
Document Type
Conference Paper
Authors
E B Rampe
(Johnson Space Center Houston, United States)
V M Tu
(Jacobs (United States) Dallas, Texas, United States)
T F Bristow
(Ames Research Center Mountain View, United States)
B L Ehlmann
(California Institute of Technology Pasadena, United States)
R V Morris
(Johnson Space Center Houston, United States)
J V Clark
(GeoControl Systems (United States) Houston, Texas, United States)
S Perry
(California Department of Water Resources )
V Cruz
(Jacobs (United States) Dallas, Texas, United States)
B Rasmussen
(California Institute of Technology Pasadena, United States)
D W Ming
(Johnson Space Center Houston, United States)
P D Archer
(Jacobs (United States) Dallas, Texas, United States)
Date Acquired
January 16, 2024
Subject Category
Lunar and Planetary Science and Exploration
Meeting Information
Meeting: 55th Lunar and Planetary Science Conference (LPSC)
Location: The Woodlands, TX
Country: US
Start Date: March 11, 2024
End Date: March 15, 2024
Sponsors: Lunar and Planetary Institute
Funding Number(s)
WBS: 811073.02.52.01.11
Distribution Limits
Public
Copyright
Portions of document may include copyright protected material.
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