Stability of hydrous minerals on the martian surface

By D. Bish, J. Carey, D. Vaniman, S. Chipera. 2003

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Hydration state of the Martian surface as seen by Mars Express OMEGA: 2. H2O content of the surface (2007, background): “…for instance, then experimental data estimating the amount of water these minerals can store under current Mars pressure and temperature conditions [Bish et al., 2003; Fialips et al., 2005] can be used to determine the relative proportions of dust and nontronite that are required to fit our…”
Mineralogy and evolution of the surface of Mars: A review (2007, background): “Zeolites, which are hydrated silicates, are invoked as possible reservoirs of water on the surface of Mars (Bish et al., 2003; Fialips et al., 2005; Tokano and Bish, 2005).”
Global distribution of near-surface hydrogen on Mars (2004, background): “One possible explanation is that these deposits contain hydrated minerals [Feldman et al., 2002b; Bish et al., 2003a ], possibly in the form of clays, zeolites, hydrous sulfates, hydrous carbonates, hydrous chlorides, and/or other more complex hydrous salts.”
Stability and exchange of subsurface ice on Mars (2005, background): “Adsorption is assumed to be rapid compared to temperature variations [Zent and Quinn, 1997; Bish et al., 2003].”