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Carbon sequestration on Mars: Reply

Edwards, Christopher S. and Ehlmann, Bethany L. (2016) Carbon sequestration on Mars: Reply. Geology, 44 (6). e389. ISSN 0091-7613. doi:10.1130/G37984Y.1.

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Martian atmospheric pressure has important implications for the past and present habitability of the planet, including the timing and causes of environmental change. The ancient Martian surface is strewn with evidence for early water bound in minerals (e.g., Ehlmann and Edwards, 2014) and recorded in surface features such as large catastrophically created outflow channels (e.g., Carr, 1979), valley networks (Hynek et al., 2010; Irwin et al., 2005), and crater lakes (e.g., Fassett and Head, 2008). Using orbital spectral data sets coupled with geologic maps and a set of numerical spectral analysis models, Edwards and Ehlmann (2015) constrained the amount of atmospheric sequestration in early Martian rocks and found that the majority of this sequestration occurred prior to the formation of the early Hesperian/late Noachian valley networks (Fassett and Head, 2011; Hynek et al., 2010), thus implying the atmosphere was already thin by the time these surface-water-related features were formed.

Item Type:Article
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URLURL TypeDescription ItemOriginal Article
Ehlmann, Bethany L.0000-0002-2745-3240
Additional Information:© 2016 Geological Society of America. First Published on May 23, 2016.
Issue or Number:6
Record Number:CaltechAUTHORS:20160708-110916082
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Official Citation:Carbon sequestration on Mars: REPLY Christopher S. Edwards, Bethany L. Ehlmann Geology Jun 2016, 44 (6) e389; DOI: 10.1130/G37984Y.1
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:68923
Deposited By: Tony Diaz
Deposited On:08 Jul 2016 23:34
Last Modified:11 Nov 2021 04:06

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