Stability and exchange of subsurface ice on Mars

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Thermal contraction crack polygons on Mars: Classification, distribution, and climate implications from HiRISE observations (2009, background): “ice reservoirs: deconvolving primary atmospheric deposition that forms massive ice deposits, from cyclical vapor diffusion, that generates pore-ice deposits remains an active area of inquiry [Mustard et al., 2001; Head et al., 2003; Schorghofer and Aharonson, 2005; Kostama et al., 2006; Schorghofer,”
Widespread excess ice in Arcadia Planitia, Mars (2015, background): “EXCESS ICE IN ARCADIA PLANITIA, MARS 6571 which show a match between today’s ice distribution and current climate model predictions [Mellon et al., 2004; Schorghofer and Aharonson, 2005].”
The Modern Near-Surface Martian Climate: A Review of In-situ Meteorological Data from Viking to Curiosity (2017, background): “At equatorial and low latitudes, brine formation by the melting of ice is unlikely because water ice is not thermodynamically stable in the shallow subsurface at these latitudes (Mellon and Jakosky 1993; Mellon et al. 2004; Schorghofer and Aharonson 2005).”