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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 long and was named after a classical albedo feature name.〔(IAU Gazetteer of Planetary Nomenclature )〕 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.〔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.〕 ==Gallery== File:Top of Coprates Chasma.jpg|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. Image:Corprates Chasma Fault.JPG|Faults, as seen by HiRISE. Layers in the rock face may be from volcanic, lacustrine, and/or aeolian sediments deposited in Valles Marineris. Image:PIA19805-SeasonalFlows-CopratesChasma-VallesMarineris-20150721.jpg|Seasonal flows on Coprates Chasma in Valles Marineris. 抄文引用元・出典: フリー百科事典『 ウィキペディア（Wikipedia）』 ■ウィキペディアで「Coprates Chasma」の詳細全文を読む スポンサード リンク
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