Summary

Licensing

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1. ↑ ^{a b c} Kereszturi, A., et al. "Indications of brine related local seepage phenomena on the northern hemisphere of Mars." Icarus 207.1 (2010): 149-164.
2. ↑ ^{a b} (2013). "Water and Brines on Mars: Current Evidence and Implications for MSL". Space Science Reviews 175 (1-4): 29–51. DOI:10.1007/s11214-012-9956-3. ISSN 0038-6308.
3. ↑ (2013). "Water and Brines on Mars: Current Evidence and Implications for MSL". Space Science Reviews 175 (1-4): 29–51. DOI:10.1007/s11214-012-9956-3. ISSN 0038-6308. ""Martinez et al. (2012) show that the formation of brines is consistent with the low temperatures measured by TES and THEMIS when they form (≤180 K), if the spatial resolution and optical properties of the translucent CO2 ice layer are considered. The resolution of TES is much coarser than the dimensions of the dark spots and FLF. In addition, TES and THEMIS measurements of the surface temperature are in the thermal infrared band, where CO2 ice is opaque. Since the fractional area covered by dark spots and FLF (composed of dark material above the CO2 ice layer), is much smaller than that covered by CO2 ice in TES and THEMIS pixels, they predominantly measure the low brightness temperature associated with the CO2 ice layer, not the temperature of the dark spots and FLF. As postulated by the gas venting model, shortwave solar radiation can efficiently penetrate the translucent CO2 ice layer. Thus, both the underlying surface and the dark ejecta can reach temperatures much higher than those measured by TES and THEMIS (Martinez et al. 2012). Also, subsurface melt water and ULI water can form in the shallow subsurface at temperatures as low as 180 K (see Sect. 2). Salts in contact with these types of liquid water could form liquid brines, and thus help explain the evolution of dune dark spots and FLF.""