The imprint of atmospheric evolution in the D/H of Hesperian clay minerals on Mars
- Creators
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Mahaffy, P. R.
- Webster, C. R.
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Stern, J. C.
- Brunner, A. E.
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Atreya, S. K.
- Conrad, P. G.
- Domagal-Goldman, S.
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Eigenbrode, J. L.
- Flesch, G. J.
- Christensen, L. E.
- Franz, H. B.
- Freissinet, C.
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Glavin, D. P.
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Grotzinger, J. P.
- Jones, J. H.
- Leshin, L. A.
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Malespin, C.
- McAdam, A. C.
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Ming, D. W.
- Navarro-González, R.
- Niles, P. B.
- Owen, T.
- Pavlov, A. A.
- Steele, A.
- Trainer, M. G.
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Williford, K. H.
- Wray, J. J.
- MSL Science Team
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°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.
Attached Files
Supplemental Material - Mahaffy-SM.pdf
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Additional details
- Eprint ID
- 52528
- DOI
- 10.1126/science.1260291
- Resolver ID
- CaltechAUTHORS:20141210-083740627
- NASA
- Created
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2014-12-16Created from EPrint's datestamp field
- Updated
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2021-11-10Created from EPrint's last_modified field
- Caltech groups
- Division of Geological and Planetary Sciences (GPS)