Swiss cheese features

Pits in south polar ice cap, taken in consecutive southern hemisphere summers, the first of which was in 1999, the second in 2001. Mars Global Surveyor, NASA

Swiss cheese features (SCFs) are curious pits in the south polar ice cap of Mars (Mare Australe quadrangle) named from their similarity to the holes in Swiss cheese. They were first seen in 2000 using Mars Orbiter Camera imagery.^[1] They are typically a few hundred meters across and 8 metres deep, with a flat base and steep sides. They tend to have similar bean-like shapes with a cusp pointing towards the south pole, indicating that insolation is involved in their formation. The angle of the Sun probably contributes to their roundness. Near the Martian summer solstice, the Sun can remain continuously just above the horizon; as a result the walls of a round depression will receive more intense sunlight, and sublimate much more rapidly than the floor. The walls sublimate and recede, while the floor remains the same.^[2]^[3]
As the seasonal frost disappears, the pit walls appear to darken considerably relative to the surrounding terrain. The SCFs have been observed to grow in size, year by year, at an average rate of 1 to 3 meters, suggesting that they are formed in a thin layer (8m) of carbon dioxide ice lying on top of water ice.^[4]^[5] Later research with HiRISE showed that the pits are in a 1-10 meter thick layer of dry ice that is sitting on a much larger water ice cap. Pits have been observed to begin with small areas along faint fractures. The circular pits have steep walls that work to focus sunlight, thereby increasing erosion. For a pit to develop, a steep wall of about 10 cm and a length of over 5 meters is necessary.^[6]

Swiss cheese-like ice formations as seen by Mars Global Surveyor.

Swiss cheese-like ice formations as seen by Mars Global Surveyor showing layers.

Close-up of Swiss cheese terrain, as seen by Mars Global Surveyor.

References[edit]

^ Thomas, P. C.; et al. (2000). "North-south geological differences between the residual polar caps on Mars". Nature. 404 (6774): 161–4. Bibcode:2000Natur.404..161T. doi:10.1038/35004528. PMID 10724162.

^ Hartmann, W. 2003. A Traveler's Guide to Mars. Workman Publishing. NY NY.

^ Mangold, N. 2011. Ice sublimation as a geomorphic process: A planetary perspective. Geomorphology. 126:1-17.

^ Byrne, S.; Ingersoll, A. P. (2002). "A Sublimation Model for the Formation of the Martian Polar Swiss-cheese Features". American Astronomical Society. American Astronomical Society. 34: 837. Bibcode:2002DPS....34.0301B.

^ "HiRISE - South Pole Residual Cap Swiss-Cheese Terrain Monitoring (PSP_005095_0935)". hirise.lpl.arizona.edu. Archived from the original on 2015-02-12.

^ Buhler, Peter, Andrew Ingersoll, Bethany Ehlmann, Caleb Fassett, James Head. 2017. How the martian residual south polar cap develops quasi-circular and heart-shaped pits, troughs, and moats. Icarus: 286, 69-9.

[1] Thomas, P. C.; et al. (2000). "North-south geological differences between the residual polar caps on Mars". Nature. 404 (6774): 161–4. Bibcode:2000Natur.404..161T. doi:10.1038/35004528. PMID 10724162.

[2] Hartmann, W. 2003. A Traveler's Guide to Mars. Workman Publishing. NY NY.

[3] Mangold, N. 2011. Ice sublimation as a geomorphic process: A planetary perspective. Geomorphology. 126:1-17.

[4] Byrne, S.; Ingersoll, A. P. (2002). "A Sublimation Model for the Formation of the Martian Polar Swiss-cheese Features". American Astronomical Society. American Astronomical Society. 34: 837. Bibcode:2002DPS....34.0301B.

[5] "HiRISE - South Pole Residual Cap Swiss-Cheese Terrain Monitoring (PSP_005095_0935)". hirise.lpl.arizona.edu. Archived from the original on 2015-02-12.

[6] Buhler, Peter, Andrew Ingersoll, Bethany Ehlmann, Caleb Fassett, James Head. 2017. How the martian residual south polar cap develops quasi-circular and heart-shaped pits, troughs, and moats. Icarus: 286, 69-9.

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