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This article is about the crater on Mars. For the lunar crater, see Main (lunar crater).
West side of Main crater (Martian crater), as seen by CTX camera (on Mars Reconnaissance Orbiter).
Dust trails in Main crater, as seen by CTX camera (on Mars Reconnaissance Orbiter).Arrow indicates wind direction. In the spring, as the temperature rises, dry ice turns into a pressurized gas, and then blows through a weak spot and carries with it dust. If there is a wind, the dust is deposited in an elongated form as in this image.

Main is an impact crater on Mars, located in the Mare Australe quadrangle at 76.6°S latitude and 310.9°W longitude. It measures 109.0 kilometers in diameter and was named after Rev. Robert Main. The name was approved in 1973, by the International Astronomical Union (IAU) Working Group for Planetary System Nomenclature (WGPSN). [1] The floor of Main shows dark portions which are caused by pressurized carbon dioxide blowing dust in the atmosphere in the spring when the temperature goes up. Some of the dust is shaped into streaks if there is a wind. [2]

Many ideas have been advanced to explain these features. [3] [4] [5] [6] [7] [8] These features can be seen in some of the pictures below.

Close up views of these features often reveal fuzzy features that have been named "spiders."

See also

References

  1. ^ "Gazetteer of Planetary Nomenclature | Main". usgs.gov. International Astronomical Union. Retrieved 4 March 2015.
  2. ^ "Thawing 'Dry Ice' Drives Groovy Action on Mars". Jet Propulsion Laboratory.
  3. ^ Kieffer, H. H. (2000). "Mars Polar Science 2000 - Annual Punctuated CO2 Slab-ice and Jets on Mars" (PDF). Retrieved 6 September 2009. {{ cite journal}}: Cite journal requires |journal= ( help)
  4. ^ Kieffer, Hugh H. (2003). "Third Mars Polar Science Conference (2003)- Behavior of Solid CO" (PDF). Retrieved 6 September 2009. {{ cite journal}}: Cite journal requires |journal= ( help)
  5. ^ Portyankina, G., ed. (2006). "Fourth Mars Polar Science Conference - Simulations of Geyser-Type Eruptions in Cryptic Region of Martian South" (PDF). Retrieved 11 August 2009. {{ cite journal}}: Cite journal requires |journal= ( help)
  6. ^ Sz. Bérczi; et al., eds. (2004). "Lunar and Planetary Science XXXV (2004) - Stratigraphy of Special Layers – Transient Ones on Permeable Ones: Examples" (PDF). Retrieved 12 August 2009. {{ cite journal}}: Cite journal requires |journal= ( help)
  7. ^ "NASA Findings Suggest Jets Bursting From Martian Ice Cap". Jet Propulsion Laboratory. NASA. 16 August 2006. Retrieved 11 August 2009.
  8. ^ C.J. Hansen; N. Thomas; G. Portyankina; A. McEwen; T. Becker; S. Byrne; K. Herkenhoff; H. Kieffer; M. Mellon (2010). "HiRISE observations of gas sublimation-driven activity in Mars' southern polar regions: I. Erosion of the surface" (PDF). Icarus. 205 (1): 283–295. Bibcode: 2010Icar..205..283H. doi: 10.1016/j.icarus.2009.07.021. Retrieved 26 July 2010.
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