Coprates Chasma
Template:Infobox feature on Mars
Coprates Chasma 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]
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 meters 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.[2][3]
The bottom of the Coprates Chasma contain a large field of small pitted cones which have been interpreted as Martian equivalents of terrestrial igneous[4] or mud volcanoes.[5]
Recurrent slope lineae
Recurrent slope lineae are small dark streaks on slopes that elongate in warm seasons. They may be evidence of liquid water.[6] [7] [8]
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Wide view of part of Valles Marineris, as seen by HiRISE under HiWish program Box shows location of recurrent slope lineae that are enlarged in next image. -
Close, color view of recurrent slope lineae, as seen by HiRISE under HiWish program Arrows point to some of the recurrent slope lineae. -
Recurrent slope lineae elongate when the slopes are at their warmest. Near the equator, RSL elongate on northern slopes in the northern summer and on the southern slopes in the southern summer.
Gallery
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South rim of Coprates Chasma, image is about a kilometer wide. With enhanced IR colors, we see a portion of the very top of the south wall of the canyon, looking down onto the steep upper slopes of the canyon. -
Faults, as seen by HiRISE. Layers in the rock face may be from volcanic, lacustrine, and/or aeolian sediments deposited in Valles Marineris. -
Seasonal flows on Coprates Chasma in Valles Marineris.
References
- ^ IAU Gazetteer of Planetary Nomenclature
- ^ 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.
- ^ Harrison, K., M. Chapman. 2008. Evidence for ponding and catastrophic floods in central Valles Marineris, Mars. Icarus: 198, 351-364.
- ^ 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.
- ^ 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.
- ^ McEwen, A., et al. 2014. Recurring slope lineae in equatorial regions of Mars. Nature Geoscience 7, 53-58. doi:10.1038/ngeo2014
- ^ McEwen, A., et al. 2011. Seasonal Flows on Warm Martian Slopes. Science. 05 Aug 2011. 333, 6043,740-743. DOI: 10.1126/science.1204816
- ^ http://redplanet.asu.edu/?tag=recurring-slope-lineae
See also
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