Landform due to the sublimation of any ice at the surface or in the subsurface.
A type of thermokarst landforms.
Pits can exist from the millimeter scale to the kilometer scale. Depend on depth and thickness of ice and temperature variations of the ground.
Residual lags. They are depleted in ice, resulting from sublimation loss. They are underlied by ice-rich material.
Landforms produced by differential sublimation due to albedo differences. Low-albedo material is heated and experiences more intensive sublimation than high-albedo regions that are cooler and preserve ice, leaving a dark lag deposit that will protect the underlying dark ice. Volatiles removed from dark regions are redeposited onto clean ice as frost. This process enhances albedo contrast between dirty and clean ice (Prockter et al. 1998; Mangold 2011). This process characteristically occurs on icy...
KeywordsPorosity Dioxide Dust Depression Mercury
- Blewett DT, Chabot NL, Denevi BW, Ernst CM, Head JW, Izenberg NR, Murchie SL, Solomon SC, Nittler LR, McCoy TJ, Xiao Z, Baker DMH, Fassett CI, Braden SE, Oberst J, Scholten F, Preusker F, Hurwitz DM (2011) Hollows on Mercury: MESSENGER evidence for geologically recent volatile-related activity. Science 333:1856CrossRefGoogle Scholar
- Hansen CJ, Byrne S, Portyankina G, Bourke M et al (2012) Observations of the northern seasonal polar cap on Mars: I. Spring sublimation activity and processes. Icarus http://dx.doi.org/10.1016/j.icarus.2012.09.024
- Hartmann WK, Raper O (1974) The new mars: The discoveries of mariner 9, NASA SP-337Google Scholar
- Lefort A, Russell PS, Thomas N, McEwen AS, Dundas CM, Kirk RL (2009) Observations of periglacial landforms in Utopia Planitia with the High Resolution Imaging Science Experiment (HiRISE). J Geophys Res 114, E04005. doi:10.1029/2008JE003264Google Scholar
- Levy JS, Head JW, Marchant DR (2011) Gullies, polygons and mantles in Martian permafrost environments: cold desert landforms and sedimentary processes during recent Martian geological history, Special publications 354. Geological Society, London, pp 167–182. doi:10.1144/SP354.10Google Scholar