The imprint of atmospheric evolution in the D/H of hesperian clay minerals on Mars

P. R. Mahaffy*, C. R. Webster, J. C. Stern, A. E. Brunner, S. K. Atreya, P. G. Conrad, S. Domagal-Goldman, J. L. Eigenbrode, G. J. Flesch, L. E. Christensen, H. B. Franz, C. Freissinet, D. P. Glavin, J. P. Grotzinger, J. H. Jones, L. A. Leshin, C. Malespin, A. C. McAdam, D. W. Ming, R. Navarro-GonzalezP. B. Niles, T. Owen, A. A. Pavlov, A. Steele, M. G. Trainer, K. H. Williford, J. J. Wray, Penny King

*Corresponding author for this work

    Research output: Contribution to journalArticlepeer-review

    119 Citations (Scopus)

    Abstract

    The deuterium-to-hydrogen (D/H) ratio in strongly bound water or hydroxyl groups in ancient martian clays retains the imprint of the water of formation of these minerals. Curiosity's Sample Analysis at Mars (SAM) experiment measured thermally evolved water and hydrogen gas released between 550° and 950°C from samples of Hesperian-era Gale crater smectite to determine this isotope ratio. The D/H value is 3.0 (±0.2) times the ratio in standard mean ocean water. The D/H ratio in this ∼3-billion-year-old mudstone, which is half that of the present martian atmosphere but substantially higher than that expected in very early Mars, indicates an extended history of hydrogen escape and desiccation of the planet.

    Original languageEnglish
    Pages (from-to)412-414
    Number of pages3
    JournalScience
    Volume347
    Issue number6220
    DOIs
    Publication statusPublished - 23 Jan 2015

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