Outflow channels
Outflow channels are extremely long, wide swathes of scoured ground on Mars , commonly containing the streamlined remnants of pre-existing topography and other linear erosive features indicating sculpting by fluids moving downslope. [1] Channels extend many hundreds of kilometers in length and are typically greater than one kilometer in width; the largest valley ( Kasei Vallis ) is around 3,500 km (2,200 mi) long, greater than 400 km (250 mi) wide and exceeds 2.5 km (1.6 mi) in depth cut into the surrounding plains. These features tend to appear fully sized at fractures in the Martian surface, either from chaos terrains or from canyon systems or other tectonically controlled, deep graben , though there are exceptions. Besides their exceptional size, the channels are also characterized by low sinuosities and high width:depth ratios compared both to other Martian valley features and to terrestrial river channels. Crater counts indicate that most of the channels were cut since the early Hesperian , [2] though the age of the features is variable between different regions of Mars. Some outflow channels in the Amazonis and Elysium Planitiae regions have yielded ages of only tens of million years, extremely young by the standards of Martian topographic features. [3]
Page Revisions
| Year | Metadata | Sections | Top Words | First Paragraph |
| 2018 |
122612 characters 12 sections 12 paragraphs 13 images 742 internal links 3 external links |
channels 0.502 outflow 0.377 floods 0.137 amazonis 0.121 elysium 0.120 drainage 0.114 tend 0.110 graben 0.109 terrestrial 0.106 cut 0.105 chryse 0.103 channel 0.101 planitiae 0.100 argued 0.094 flow 0.093 |
Outflow channels are extremely long, wide swathes of scoured ground on Mars , commonly containing the streamlined remnants of pre-existing topography and other linear erosive features indicating sculpting by fluids moving downslope. [1] Channels extend many hundreds of kilometers in length and are typically greater than one kilometer in width; the largest valley ( Kasei Vallis ) is around 3,500 km (2,200 mi) long, greater than 400 km (250 mi) wide and exceeds 2.5 km (1.6 mi) in depth cut into the surrounding plains. These features tend to appear fully sized at fractures in the Martian surface, either from chaos terrains or from canyon systems or other tectonically controlled, deep graben , though there are exceptions. Besides their exceptional size, the channels are also characterized by low sinuosities and high width:depth ratios compared both to other Martian valley features and to terrestrial river channels. Crater counts indicate that most of the channels were cut since the early Hesperian , [2] though the age of the features is variable between different regions of Mars. Some outflow channels in the Amazonis and Elysium Planitiae regions have yielded ages of only tens of million years, extremely young by the standards of Martian topographic features. [3] |
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| 2017 |
122470 characters 12 sections 12 paragraphs 13 images 742 internal links 3 external links |
channels 0.502 outflow 0.377 floods 0.137 amazonis 0.121 elysium 0.120 drainage 0.114 tend 0.110 graben 0.109 terrestrial 0.106 cut 0.105 chryse 0.103 channel 0.101 planitiae 0.100 argued 0.094 flow 0.093 |
Outflow channels are extremely long, wide swathes of scoured ground on Mars , commonly containing the streamlined remnants of pre-existing topography and other linear erosive features indicating sculpting by fluids moving downslope. [1] Channels extend many hundreds of kilometers in length and are typically greater than one kilometer in width; the largest valley ( Kasei Vallis ) is around 3,500 km (2,200 mi) long, greater than 400 km (250 mi) wide and exceeds 2.5 km (1.6 mi) in depth cut into the surrounding plains. These features tend to appear fully sized at fractures in the Martian surface, either from chaos terrains or from canyon systems or other tectonically controlled, deep graben , though there are exceptions. Besides their exceptional size, the channels are also characterized by low sinuosities and high width:depth ratios compared both to other Martian valley features and to terrestrial river channels. Crater counts indicate that most of the channels were cut since the early Hesperian , [2] though the age of the features is variable between different regions of Mars. Some outflow channels in the Amazonis and Elysium Planitiae regions have yielded ages of only tens of million years, extremely young by the standards of Martian topographic features. [3] |
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| 2016 |
60700 characters 12 sections 12 paragraphs 13 images 211 internal links 3 external links |
channels 0.502 outflow 0.377 floods 0.137 amazonis 0.121 elysium 0.120 drainage 0.114 tend 0.110 graben 0.109 terrestrial 0.106 cut 0.105 chryse 0.103 channel 0.101 planitiae 0.100 argued 0.094 flow 0.093 |
Outflow channels are extremely long, wide swathes of scoured ground on Mars , commonly containing the streamlined remnants of pre-existing topography and other linear erosive features indicating sculpting by fluids moving downslope. [1] Channels extend many hundreds of kilometers in length and are typically greater than one kilometer in width; the largest valley ( Kasei Vallis ) is around 3,500 km (2,200 mi) long, greater than 400 km (250 mi) wide and exceeds 2.5 km (1.6 mi) in depth cut into the surrounding plains. These features tend to appear fully sized at fractures in the Martian surface, either from chaos terrains or from canyon systems or other tectonically controlled, deep graben , though there are exceptions. Besides their exceptional size, the channels are also characterized by low sinuosities and high width:depth ratios compared both to other Martian valley features and to terrestrial river channels. Crater counts indicate that most of the channels were cut since the early Hesperian , [2] though the age of the features is variable between different regions of Mars. Some outflow channels in the Amazonis and Elysium Planitiae regions have yielded ages of only tens of million years, extremely young by the standards of Martian topographic features. [3] |
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| 2015 |
60929 characters 12 sections 12 paragraphs 13 images 212 internal links 3 external links |
channels 0.502 outflow 0.377 floods 0.137 amazonis 0.121 elysium 0.120 drainage 0.114 tend 0.110 graben 0.109 terrestrial 0.106 cut 0.105 chryse 0.103 channel 0.101 planitiae 0.100 argued 0.094 flow 0.093 |
Outflow channels are extremely long, wide swathes of scoured ground on Mars , commonly containing the streamlined remnants of pre-existing topography and other linear erosive features indicating sculpting by fluids moving downslope. [1] Channels extend many hundreds of kilometers in length and are typically greater than one kilometer in width; the largest valley ( Kasei Vallis ) is around 3,500 km (2,200 mi) long, greater than 400 km (250 mi) wide and exceeds 2.5 km (1.6 mi) in depth cut into the surrounding plains. These features tend to appear fully sized at fractures in the Martian surface, either from chaos terrains or from canyon systems or other tectonically controlled, deep graben , though there are exceptions. Besides their exceptional size, the channels are also characterized by low sinuosities and high width:depth ratios compared both to other Martian valley features and to terrestrial river channels. Crater counts indicate that most of the channels were cut since the early Hesperian , [2] though the age of the features is variable between different regions of Mars. Some outflow channels in the Amazonis and Elysium Planitiae regions have yielded ages of only tens of million years, extremely young by the standards of Martian topographic features. [3] |
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| 2013 |
60048 characters 11 sections 12 paragraphs 13 images 213 internal links 2 external links |
channels 0.495 outflow 0.359 floods 0.140 amazonis 0.124 elysium 0.123 drainage 0.116 tend 0.112 graben 0.112 terrestrial 0.109 cut 0.107 chryse 0.105 channel 0.104 planitiae 0.102 argued 0.097 flow 0.096 |
Outflow channels are extremely long, wide swathes of scoured ground on Mars , commonly containing the streamlined remnants of pre-existing topography and other linear erosive features indicating sculpting by fluids moving downslope. [1] Channels extend many hundreds of kilometers in length and are typically greater than one kilometer in width; the largest valley ( Kasei Vallis ) is around 3,500 km (2,200 mi) long, greater than 400 km (250 mi) wide and exceeds 2.5 km (1.6 mi) in depth cut into the surrounding plains. These features tend to appear fully sized at fractures in the Martian surface, either from chaos terrains or from canyon systems or other tectonically controlled, deep graben , though there are exceptions. Besides their exceptional size, the channels are also characterized by low sinuosities and high width:depth ratios compared both to other Martian valley features and to terrestrial river channels. Crater counts indicate that most of the channels were cut since the early Hesperian , [2] though the age of the features is variable between different regions of Mars. Some outflow channels in the Amazonis and Elysium Planitiae regions have yielded ages of only tens of million years, extremely young by the standards of Martian topographic features. [3] |
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| 2012 |
59296 characters 11 sections 12 paragraphs 12 images 214 internal links 2 external links |
channels 0.495 outflow 0.359 floods 0.140 amazonis 0.124 elysium 0.123 drainage 0.116 tend 0.112 graben 0.112 terrestrial 0.109 cut 0.107 chryse 0.105 channel 0.104 planitiae 0.102 argued 0.097 flow 0.096 |
Outflow channels are the extremely long, wide swathes of scoured ground on Mars , commonly containing the streamlined remnants of pre-existing topography and other linear erosive features indicating sculpting by fluids moving downslope. [1] Channels extend many hundreds of kilometers in length and are typically greater than one kilometer in width; the largest valley ( Kasei Vallis ) is around 3500 km long, greater than 400 km wide and exceeds 2.5 km in depth cut into the surrounding plains. These features tend to appear fully sized at fractures in the Martian surface, either from chaos terrains or from canyon systems or other tectonically controlled, deep graben , though there are exceptions. Besides their exceptional size, the channels are also characterized by low sinuosities and high width:depth ratios compared both to other Martian valley features and to terrestrial river channels. Crater counts indicate that most of the channels were cut since the early Hesperian , [2] though the age of the features is variable between different regions of Mars. Some outflow channels in the Amazonis and Elysium Planitiae regions have yielded ages of only tens of million years, extremely young by the standards of Martian topographic features. [3] |
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| 2011 |
59222 characters 11 sections 12 paragraphs 12 images 213 internal links 1 external links |
channels 0.495 outflow 0.359 floods 0.140 amazonis 0.124 elysium 0.123 drainage 0.116 tend 0.112 graben 0.112 terrestrial 0.109 cut 0.107 chryse 0.105 channel 0.104 planitiae 0.102 argued 0.097 flow 0.096 |
Outflow channels is the term used to describe extremely long, wide swathes of scoured ground on Mars , commonly containing the streamlined remnants of pre-existing topography and other linear erosive features indicating sculpting by fluids moving downslope [1] . Channels extend many hundreds of kilometers in length and are typically greater than one kilometer in width; the largest valley ( Kasei Vallis ) is around 3500 km long, greater than 400 km wide and exceeds 2.5 km in depth cut into the surrounding plains. These features tend to appear fully sized at fractures in the Martian surface, either from chaos terrains or from canyon systems or other tectonically controlled, deep graben , though there are exceptions. Besides their exceptional size, the channels are also characterized by low sinuosities and high width:depth ratios compared both to other Martian valley features and to terrestrial river channels. Crater counts indicate that most of the channels were cut since the early Hesperian [2] , though the age of the features is variable between different regions of Mars. Some outflow channels in the Amazonis and Elysium Planitiae regions have yielded ages of only tens of million years, extremely young by the standards of Martian topographic features [3] . |
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| 2010 |
16062 characters 2 sections 3 paragraphs 11 images 18 internal links 1 external links |
outflow 0.600 channels 0.414 fluid 0.319 length 0.282 thousands 0.271 channel 0.226 flow 0.208 systems 0.184 largest 0.173 kilometers 0.163 formed 0.123 large 0.084 surface 0.076 mars 0.021 |
The outflow channels of Mars are large channel systems that formed by fluid flow from the sub-surface . The largest outflow channels are thousands of kilometers in length. |
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| 2009 |
14883 characters 2 sections 1 paragraphs 10 images 15 internal links 1 external links |
outflow 0.600 channels 0.414 fluid 0.319 length 0.282 thousands 0.271 channel 0.226 flow 0.208 systems 0.184 largest 0.173 kilometers 0.163 formed 0.123 large 0.084 surface 0.076 mars 0.021 |
The outflow channels of Mars are large channel systems that formed by fluid flow from the sub-surface . The largest outflow channels are thousands of kilometers in length. |