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. 2017 Apr 17;375(2094):20150390. doi: 10.1098/rsta.2015.0390

Figure 3.

Figure 3.

(ae) D/H ratio (δD) versus water content in Martian igneous minerals. High-impact shock pressures, mantle source enrichment and crustal assimilation can add D-rich atmospheric hydrogen to igneous minerals, meaning the majority do not have D/H ratios representative of the Martian mantle (δD < 275‰, orange envelope). See the electronic supplementary material for data and references.