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- D. T. Vaniman
- Planetary Science Institute, Tucson, AZ 85719, USA.
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- D. L. Bish
- Department of Geological Sciences, Indiana University, Bloomington, IN 47405, USA.
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- D. W. Ming
- NASA Johnson Space Center, Houston, TX 77058, USA.
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- T. F. Bristow
- NASA Ames Research Center, Moffett Field, CA 94035, USA.
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- R. V. Morris
- NASA Johnson Space Center, Houston, TX 77058, USA.
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- D. F. Blake
- NASA Ames Research Center, Moffett Field, CA 94035, USA.
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- S. J. Chipera
- Chesapeake Energy, Oklahoma City, OK 73154, USA.
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- S. M. Morrison
- Department of Geosciences, University of Arizona, Tucson, AZ 85721, USA.
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- A. H. Treiman
- Lunar and Planetary Institute, Houston, TX 77058, USA.
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- E. B. Rampe
- NASA Johnson Space Center, Houston, TX 77058, USA.
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- M. Rice
- Division of Geologic and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA.
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- C. N. Achilles
- ESCG/UTC Aerospace Systems, Houston, TX 77058, USA.
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- J. P. Grotzinger
- Division of Geologic and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA.
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- S. M. McLennan
- Department of Geosciences, State University of New York, Stony Brook, NY 11794, USA.
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- J. Williams
- Institute of Meteoritics, University of New Mexico, Albuquerque, NM 87131, USA.
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- J. F. Bell
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287, USA.
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- H. E. Newsom
- Institute of Meteoritics, University of New Mexico, Albuquerque, NM 87131, USA.
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- R. T. Downs
- Department of Geosciences, University of Arizona, Tucson, AZ 85721, USA.
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- S. Maurice
- Institut de Recherche en Astrophysique et Planétologie (IRAP), Universite de Toulouse/CNRS, Toulouse 31400, France.
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- P. Sarrazin
- SETI Institute, Mountain View, CA 94043, USA.
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- A. S. Yen
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA.
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- J. M. Morookian
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA.
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- J. D. Farmer
- School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287, USA.
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- K. Stack
- Division of Geologic and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA.
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- R. E. Milliken
- Department of Geological Sciences, Brown University, Providence, RI 02912, USA.
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- B. L. Ehlmann
- Division of Geologic and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA.
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- D. Y. Sumner
- Department of Earth and Planetary Sciences, University of California, Davis, CA 95616, USA.
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- G. Berger
- Institut de Recherche en Astrophysique et Planétologie (IRAP), Universite de Toulouse/CNRS, Toulouse 31400, France.
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- J. A. Crisp
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA.
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- J. A. Hurowitz
- Department of Geosciences, State University of New York, Stony Brook, NY 11794, USA.
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- R. Anderson
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA.
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- D. J. Des Marais
- NASA Ames Research Center, Moffett Field, CA 94035, USA.
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- E. M. Stolper
- Division of Geologic and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA.
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- K. S. Edgett
- Malin Space Science Systems, San Diego, CA 92121, USA.
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- S. Gupta
- Department of Earth Science and Engineering, Imperial College London, London SW7 2AZ, UK.
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- N. Spanovich
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA.
抄録
<jats:p> Sedimentary rocks at Yellowknife Bay (Gale crater) on Mars include mudstone sampled by the Curiosity rover. The samples, John Klein and Cumberland, contain detrital basaltic minerals, calcium sulfates, iron oxide or hydroxides, iron sulfides, amorphous material, and trioctahedral smectites. The John Klein smectite has basal spacing of ~10 angstroms, indicating little interlayer hydration. The Cumberland smectite has basal spacing at both ~13.2 and ~10 angstroms. The larger spacing suggests a partially chloritized interlayer or interlayer magnesium or calcium facilitating H <jats:sub>2</jats:sub> O retention. Basaltic minerals in the mudstone are similar to those in nearby eolian deposits. However, the mudstone has far less Fe-forsterite, possibly lost with formation of smectite plus magnetite. Late Noachian/Early Hesperian or younger age indicates that clay mineral formation on Mars extended beyond Noachian time. </jats:p>
収録刊行物
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- Science
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Science 343 (6169), 1243480-, 2014-01-24
American Association for the Advancement of Science (AAAS)