Post by Dr. Candice Hansen and Dr. Mary Bourke,
Planetary Science Institute, Tucson, Arizona, 85705
Geography, Trinity College, Dublin, Ireland
Every year, Mars’ polar regions are covered by a seasonal layer of CO2 ice (dry ice). We are just beginning to understand the important role this volatile plays as an active agent of geomorphic change on Mars. The HiRISE camera on the Mars Reconnaissance Orbiter has been used to study sublimation activity in the spring for 3 Mars years. C hannel features often organised in radial patterns were noted and known informally as “spiders”, more formally as “araneiform terrain” (Image 1). They are tens to hundreds of m wide, with individual channels measuring several meters wide. Estimates of depth are in the order of ~ 2 m, decreasing with distance from the center of the araneform. Thin channels widen and deepen as they converge. Where they drape pre-existing topography, the channels are larger in the uphill direction suggesting they were eroded by pressurised fluid (Hansen et al, 2010).
Satellite images of Mars show dark albedo fans forming over ice in the southern hemisphere (see similar fans in Image 1). These were interpreted as having formed from plumes of dust escaping from the subsurface. Kieffer et al (2006) proposed a model to explain this process: Over the course of the winter the ice anneals into a translucent slab. In the spring sunlight penetrates through the ice. This energy, along with stored heat, warms the ground below, causing the slab of ice to sublimate from the bottom. Gas is trapped between the layer of ice and the ground. When a rupture in the ice occurs the gas flows to the vent entraining fine material from the surface. The escaping gas carries the entrained material out above the ice where it falls out downwind in fan-shaped deposits (Kieffer et al, 2006) (Image 2 and 3).
The deposition of this volatile seasonally on the surface of Mars and the energy released during sublimation make it a potentially important geomorphic agent on Mars. Recently, CO 2 sublimation was shown to trigger avalanche face flows on Mars dunes (Hansen et al, 2011).
Hansen, C., Bourke, M., Bridges, N.T., Byrne, S., Colon, C., Diniega, S., Dundas, C.M., Herkenhoff, K., Mcewen, A., Mellon, M.T., Portyankina, G., and Thomas, N., (2011): Seasonal Erosion and Restoration of Mars’ Northern Polar Dunes . Science , 331, DOI: 10.1126/science.1197636.
Hansen, C.J., Thomas, N., Portyankina, G., Mcewen, A., Becker, T., Byrne, S., Herkenhoff, K., Kieffer, H., andMellon, M., 2010: HiRISE observations of gas sublimation-driven activity in Mars’ southern polar regions: I. Erosion of the surface . Icarus, 205, 283-295.
Kieffer, H.H., Christensen, P.R., and Titus, T.N., (2006) CO 2 jets formed by sublimation beneath translucent slab ice in Mars’ seasonal south polar ice cap . Nature, 442, 793-796.
Piqueux, S., and Christensen, P.R., 2008: North and south subice gas flow and venting of the seasonal caps of Mars: A major geomorphological agent . Journal of Geophysical Research (Planets), 113, 06005.
Piqueux, S., Byrne, S., and Richardson, M.I., 2003: Sublimation of Mars’ southern seasonal CO2 ice cap and the formation of spiders . Journal of Geophysical Research (Planets), 108, 5084, doi:5010.1029/2002JE002007.
Portyankina, G., Markiewicz, W.J., Thomas, N., Hansen, C.J., andMilazzo, M., 2010: HiRISE observations of gas sublimation-driven activity in Mars’ southern polar regions: III. Models of processes involving translucent ice . Icarus, 205, 311-320.
Thomas, N., Portyankina, G., Hansen, C.J., and Pommerol, A., 2011: HiRISE observations of gas sublimation-driven activity in Mars’ southern polar regions: IV. Fluid dynamics models of CO2 jets . Icarus, 212, 66-85.
Thomas, N., Portyankina, G., Hansen, C.J., andPommerol, A., 2011: Sub-surface CO2 gas flow in Mars’ polar regions: Gas transport under constant production rate conditions. Geophysical Research Letters, 38, doi:10.1029/2011GL046797.