The imprint of atmospheric evolution in the D/H of Hesperian clay minerals on Mars
- Mahaffy, P. R.
- Webster, C. R.
- Stern, J. C.
- Brunner, A. E.
- Atreya, S. K.
- Conrad, P. G.
- Domagal-Goldman, S.
- Eigenbrode, J. L.
- Flesch, G. J.
- Christensen, L. E.
- Franz, H. B.
- Freissinet, C.
- Glavin, D.P.
- Grotzinger, J. P.
- Jones, J. H.
- Leshin, L. A.
- Malespin, C.
- McAdam, A.C.
- Ming, D. W.
- Navarro-Gonzalez, R.
- Niles, P. B.
- Owen, T.
- Pavlov, A. A.
- Steele, A.
- Trainer, M. G.
- Williford, K. H.
- Wray, J. J. and the MSL Science Team
- DLR Collaborator (MSL Science Team), Reitz G.
Publication date
January 2014
DOI Publisher
American Association for the Advancement of Science (AAAS) ISSN
0036-8075 Citation count (estimate)
44Abstract
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°C 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 (SMOW). The D/H ratio in this ~3 billion year old mudstone that 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
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