Evaporation of ice in planetary atmospheres: Ice-covered rivers on mars

The State and Future of Mars Polar Science and Exploration

“…It has been suggested that subglacial discharges may have also contributed to the formation of the major polar reentrants, including Chasma Boreale in the north and Chasma Australe in the south, as well as a number of similar, but smaller features found along the periphery of both caps (Wallace and Sagan 1979, Clifford 1987, Benito et al 1997, Fishbaugh and Head 1999b, Anguita et al 2000. These broad, linear, and deeply incised depressions may have originated from a jokulhlaup, the catastrophic discharge of a large subglacial reservoir of basal meltwater.…”

Martian drainage densities

“…Although many alternatives were initially proposed, a broad consensus has emerged that the valleys have formed, like terrestrial river valleys, by the slow erosion of running water [see Carr, 1981;Baker, 1982]. Discussion of the valleys has generally focused not on their origin by slow erosion but on the relative roles of runoff and groundwater sapping [e.g., Sharp and Malin, 1975;Pieri, 1980], whether warm and wet conditions were required for their formation [e.g., Wallace and Sagan, 1979;Squyres, 1989;Squyres and Kasting, 1994], and what their broad climatic implications might be [e.g., Pollack, 1979;Pollack et al, 1987]. The basic assumption that they formed by slow erosion of running water has rarely been questioned.…”

Paleohydrology of Eberswalde crater, Mars

“…This discrepancy between empirical and theoretical results has motivated investigations of higher-thanexpected solar luminosity, obliquity variations, more effective greenhouse gases, carbon dioxide clouds, albedo differences, and release of volatiles by impacts or volcanism as possible ways of warming the planet (e.g., Baker et al, 1991;Whitmire et al, 1995;Sagan and Chyba, 1997;Segura et al, 2002;Colaprete and Toon, 2003;Segura et al, 2008Segura et al, , 2012Mischna et al, 2013;Ramirez et al, 2014). Other investigators have examined ways to erode valleys under cold conditions, including ice flow, stream flow under an ice cover, or generation of meltwater by surface (impact ejecta) or subsurface (geothermal) heat sources (e.g., Wallace and Sagan, 1979;Carr, 1983;Brakenridge et al, 1985;Wilhelms and Baldwin, 1989;Brakenridge, 1990;Gulick and Baker, 1990;Carr, 1995;Goldspiel and Squyres, 2000;Harrison and Grimm, 2002;Carr and Head, 2003;Mangold et al, 2012a). Quantitative constraints on the Martian paleoclimate based on landform morphometry would have considerable value in guiding these modeling efforts.…”