Astronomy:Coprates Chasma

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Coprates Chasma
Coprates Chasma THEMIS mosaic 0.5.jpg
Coprates Chasma in mosaic of THEMIS infrared images, with parts of Melas and Capri chasmata visible at upper left and lower right, respectively. Landslide deposits of enormous size are visible at left, near the junction with Melas Chasma, and at various locations from center to right. Several smaller chasmata and catenae parallel Coprates Chasma to its south.
Coordinates [ ⚑ ] : 13°24′S 61°24′W / 13.4°S 61.4°W / -13.4; -61.4
Coprates Chasma based on THEMIS data

Coprates Chasma (/ˈkɒprətz ˈkæzmə/) is a huge canyon in the Coprates quadrangle of Mars, located at 13.4° south latitude and 61.4° west longitude, part of the Valles Marineris canyon system. It is 966 km (600 mi) long and was named after a classical albedo feature name.[1] It was named from the classical Greek name for the Dez River in Persia.

Near 60° W is the deepest point of the Valles Marineris system (as well as its lowest point by elevation) at 11 km (36,000 ft) below the surrounding plateau. Eastward from here there is about a 0.03 degree upward slope before reaching the outflow channels, which means that if you filled the canyon with fluid, it would create a lake with a depth of 1 km (3,300 ft) before the fluid would overflow out onto the northern plains.[2]

Keith Harrison and Mary Chapman described strong evidence for a lake in the eastern part of Valles Marineris, especially in Coprates Chasma. It would have had an average depth of only 842 m—much smaller than the 5–10 km depth of parts of Valles Marineris. Still, its volume of 110,000 cubic miles would be comparable to Earth’s Caspian and Black Seas. The main evidence for such a lake is the presence of benches at the level that models show is where the lake level should be. Also, the low point in Eos Chasma where water would be expected to overflow is marked by fluvial features. The features look like the flow came together at a small point and carried out significant erosion.[3][4]

The bottom of the Coprates Chasma contain a large field of small pitted cones which have been interpreted as Martian equivalents of terrestrial igneous[5] or mud volcanoes.[6]

Recurrent slope lineae

Recurrent slope lineae are small dark streaks on slopes that elongate in warm seasons. They may be evidence of liquid water.[7][8][9]


See also


  1. "Planetary Names: Chasma, chasmata: Coprates Chasma on Mars" (in en).;jsessionid=DF387ED174AF21E6F11F99C4D4044B62. 
  2. Cattermole, Peter John (2001). Mars: the mystery unfolds. Oxford University Press. p. 105. ISBN 0-19-521726-8. 
  3. Harrison, K., M. Chapman. 2010. Episodic ponding and outburst flooding associated with chaotic terrains in Valles Marineris In Cabrol, N. and E. Grin (eds.). 2010. Lakes on Mars. Elsevier. NY.
  4. Harrison, K., M. Chapman. 2008. Evidence for ponding and catastrophic floods in central Valles Marineris, Mars. Icarus: 198, 351-364.
  5. Brož, Petr; Hauber, Ernst; Wray, James J.; Michael, Gregory (September 2017). "Amazonian volcanism inside Valles Marineris on Mars". Earth and Planetary Science Letters 473: 122–130. doi:10.1016/j.epsl.2017.06.003. Bibcode2017E&PSL.473..122B. 
  6. Okubo, Chris H. (May 2016). "Morphologic evidence of subsurface sediment mobilization and mud volcanism in Candor and Coprates Chasmata, Valles Marineris, Mars". Icarus 269: 23–37. doi:10.1016/j.icarus.2015.12.051. Bibcode2016Icar..269...23O. 
  7. McEwen, A., et al. 2014. Recurring slope lineae in equatorial regions of Mars. Nature Geoscience 7, 53-58. doi:10.1038/ngeo2014
  8. McEwen, A., et al. 2011. Seasonal Flows on Warm Martian Slopes. Science. 05 Aug 2011. 333, 6043,740-743. DOI: 10.1126/science.1204816
  9. "recurring slope lineae | Red Planet Report" (in en-US).