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. 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 of carbon dioxide ice lying on top of water ice. 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.
Halo features
Bright transient halo features around the carbon dioxide pits were found during the southern hemisphere's summer, during Mars year 28. However, this was the only time these features have ever been seen. The data to understand these halos were taken from the MRO Context Camera, the HiRISE camera, and the MOC. The halo features were only visible during the solar longitudes of 279 degrees and 331 degrees. The halo's appearance correlates to the global dust storm that began earlier in the same Martian year. The lifetime of the halos was broken into trimesters; the first was 285–295 degrees Ls, the second was 295–305 degrees Ls, and the final was counted at 305–340 degrees Ls. The average width of the high albedo area around the Swiss cheese features changes throughout its lifetime. In the first trimester the width was calculated to be 12.14 ± 1.44 meters wide, the second trimester was 32.96 ± 4.02 meters wide, and in the final trimester the average width was 55.48 ± 6.98 meters. The Hapke's reflectance theory was used to calculate the brightness of the features. During the first trimester, the halos were 4 +/-.3% brighter than the non-halo areas. Then in the second trimester the halos became more prominent at 7 +/-.7% brighter. Toward the end of their life they were the brightest recorded at 8 +/-.6% brighter than the surrounding topography. The halos are brighter than the surrounding region due to the impurities in the ice. The global dust storm filled the CO2 ice with sand and increased the grain size of the ice crystals.
