Glaciers on Mars
Glaciers , loosely defined as patches of currently or recently flowing ice, are thought to be present across large but restricted areas of the modern Martian surface, and are inferred to have been more widely distributed at times in the past. [1] [2] Lobate convex features on the surface known as viscous flow features and lobate debris aprons , which show the characteristics of non-Newtonian flow , are now almost unanimously regarded as true glaciers. [1] [3] [4] [5] [6] [7] [8] [9] [10]
Page Revisions
| Year | Metadata | Sections | Top Words | First Paragraph |
| 2018 |
257220 characters 14 sections 81 paragraphs 69 images 690 internal links 97 external links |
glacier 0.383 hiwish 0.327 glaciers 0.326 ismenius 0.268 hirise 0.236 lacus 0.232 fill 0.204 ice 0.185 program 0.176 lineated 0.174 tongue 0.151 valley 0.146 lobate 0.125 location 0.113 debris 0.112 |
Glaciers , loosely defined as patches of currently or recently flowing ice, are thought to be present across large but restricted areas of the modern Martian surface, and are inferred to have been more widely distributed at times in the past. [1] [2] Lobate convex features on the surface known as viscous flow features and lobate debris aprons , which show the characteristics of non-Newtonian flow , are now almost unanimously regarded as true glaciers. [1] [3] [4] [5] [6] [7] [8] [9] [10] |
|
| 2017 |
206770 characters 12 sections 79 paragraphs 71 images 221 internal links 79 external links |
3. Concentric crater fill, lineated valley fill, and lobate debris aprons |
glacier 0.375 hiwish 0.329 glaciers 0.328 ismenius 0.269 hirise 0.237 lacus 0.233 fill 0.205 ice 0.186 program 0.177 lineated 0.175 tongue 0.151 valley 0.147 lobate 0.126 location 0.114 debris 0.113 |
Glaciers , loosely defined as patches of currently or recently flowing ice, are thought to be present across large but restricted areas of the modern Martian surface, and are inferred to have been more widely distributed at times in the past. [1] [2] Lobate convex features on the surface known as viscous flow features and lobate debris aprons , which show the characteristics of non-Newtonian flow , are now almost unanimously regarded as true glaciers. [1] [3] [4] [5] [6] [7] [8] [9] [10] However, a variety of other features on the surface have also been interpreted as directly linked to flowing ice, such as fretted terrain , [1] [11] lineated valley fill , [7] [9] concentric crater fill , [3] [12] and arcuate ridges. [10] A variety of surface textures seen in imagery of the midlatitudes and polar regions are also thought to be linked to sublimation of glacial ice. [12] [13] |
| 2016 |
157979 characters 11 sections 69 paragraphs 62 images 211 internal links 33 external links |
3. Concentric crater fill, lineated valley fill, and lobate debris aprons |
glacier 0.368 glaciers 0.359 hiwish 0.309 ismenius 0.271 lacus 0.235 hirise 0.226 fill 0.194 ice 0.184 program 0.167 tongue 0.166 lineated 0.153 lobate 0.138 debris 0.117 location 0.107 brain 0.107 |
Glaciers , loosely defined as patches of currently or recently flowing ice, are thought to be present across large but restricted areas of the modern Martian surface, and are inferred to have been more widely distributed at times in the past. [1] [2] Lobate convex features on the surface known as viscous flow features and lobate debris aprons , which show the characteristics of non-Newtonian flow , are now almost unanimously regarded as true glaciers. [1] [3] [4] [5] [6] [7] [8] [9] [10] However, a variety of other features on the surface have also been interpreted as directly linked to flowing ice, such as fretted terrain , [1] [11] lineated valley fill , [7] [9] concentric crater fill , [3] [12] and arcuate ridges. [10] A variety of surface textures seen in imagery of the midlatitudes and polar regions are also thought to be linked to sublimation of glacial ice. [12] [13] |
| 2015 |
134667 characters 10 sections 51 paragraphs 41 images 180 internal links 33 external links |
3. Concentric crater fill, Lineated valley fill, and Lobate debris aprons |
glaciers 0.416 glacier 0.342 ismenius 0.230 hiwish 0.224 ice 0.223 lacus 0.199 fill 0.199 hirise 0.176 lobate 0.168 debris 0.142 lineated 0.140 lda 0.138 brain 0.130 program 0.123 aprons 0.123 |
Glaciers , loosely defined as patches of currently or recently flowing ice, are thought to be present across large but restricted areas of the modern Martian surface, and are inferred to have been more widely distributed at times in the past. [1] [2] Lobate convex features on the surface known as viscous flow features and lobate debris aprons , which show the characteristics of non-Newtonian flow , are now almost unanimously regarded as true glaciers. [1] [3] [4] [5] [6] [7] [8] [9] [10] However, a variety of other features on the surface have also been interpreted as directly linked to flowing ice, such as fretted terrain , [1] [11] lineated valley fill , [7] [9] concentric crater fill , [3] [12] and arcuate ridges. [10] A variety of surface textures seen in imagery of the midlatitudes and polar regions are also thought to be linked to sublimation of glacial ice. [12] [13] |
| 2014 |
108352 characters 8 sections 38 paragraphs 29 images 177 internal links 18 external links |
3. Concentric crater fill, Lineated valley fill, and Lobate debris aprons 4. Tongue-shaped glaciers and glaciers on volcanoes |
glacier 0.427 glaciers 0.346 ismenius 0.233 ice 0.224 lacus 0.202 fill 0.202 hiwish 0.190 hirise 0.161 lobate 0.129 tilt 0.125 aprons 0.119 glacial 0.117 lineated 0.116 debris 0.115 tongue 0.115 |
Glaciers , loosely defined as patches of currently or recently flowing ice, are thought to be present across large but restricted areas of the modern Martian surface, and are inferred to have been more widely distributed at times in the past. [1] [2] Lobate convex features on the surface known as viscous flow features and lobate debris aprons , which show the characteristics of non-Newtonian flow , are now almost unanimously regarded as true glaciers. [1] [3] [4] [5] [6] [7] [8] [9] [10] However, a variety of other features on the surface have also been interpreted as directly linked to flowing ice, such as fretted terrain , [1] [11] lineated valley fill , [7] [9] concentric crater fill , [3] [12] and arcuate ridges. [10] A variety of surface textures seen in imagery of the midlatitudes and polar regions are also thought to be linked to sublimation of glacial ice. [12] [13] |
| 2013 |
108306 characters 8 sections 38 paragraphs 30 images 176 internal links 18 external links |
3. Concentric crater fill, Lineated valley fill, and Lobate debris aprons 4. Tongue-shaped glaciers and glaciers on volcanoes |
glacier 0.427 glaciers 0.346 ismenius 0.233 ice 0.224 lacus 0.202 fill 0.202 hiwish 0.190 hirise 0.161 lobate 0.129 tilt 0.125 aprons 0.119 glacial 0.117 lineated 0.117 debris 0.115 tongue 0.115 |
Glaciers , loosely defined as patches of currently or recently flowing ice, are thought to be present across large but restricted areas of the modern Martian surface, and are inferred to have been more widely distributed at times in the past. [1] [2] Lobate convex features on the surface known as viscous flow features and lobate debris aprons , which show the characteristics of non-Newtonian flow , are now almost unanimously regarded as true glaciers. [1] [3] [4] [5] [6] [7] [8] [9] [10] However, a variety of other features on the surface have also been interpreted as directly linked to flowing ice, such as fretted terrain , [1] [11] lineated valley fill , [7] [9] concentric crater fill , [3] [12] and arcuate ridges. [10] A variety of surface textures seen in imagery of the midlatitudes and polar regions are also thought to be linked to sublimation of glacial ice. [12] [13] |
| 2012 |
92608 characters 7 sections 29 paragraphs 24 images 176 internal links 32 external links |
1. Water source for future colonists 4. Concentric crater fill, Lineated valley fill, and Lobate debris aprons |
glaciers 0.370 glacier 0.369 ismenius 0.261 lacus 0.226 ice 0.192 hiwish 0.192 hirise 0.184 tongue 0.152 mensae 0.143 debris 0.138 hellas 0.131 dirt 0.130 kettles 0.129 ridges 0.122 location 0.121 |
Glaciers formed much of the observable surface in large areas of Mars. Most of the area in high latitudes, especially the Ismenius Lacus quadrangle , is believed to still contain enormous amounts of water ice. [1] [2] Recent evidence has led many planetary scientists to believe that water ice still exists in the form of glaciers that are covered with a thin layer of insulating rock. [3] [4] [5] [6] [7] [8] In March 2010, scientists released the results of a radar study of an area called Deuteronilus Mensae that found widespread evidence of ice lying beneath a few meters of rock debris. [9] [10] Glaciers are believed to be associated with Fretted terrain , [11] many volcanoes, [12] [13] and even some craters. [14] |
| 2011 |
92464 characters 7 sections 29 paragraphs 24 images 176 internal links 32 external links |
1. Water source for future colonists 4. Concentric crater fill, Lineated valley fill, and Lobate debris aprons |
glaciers 0.370 glacier 0.369 ismenius 0.261 lacus 0.226 ice 0.192 hiwish 0.192 hirise 0.184 tongue 0.152 mensae 0.143 debris 0.138 hellas 0.131 dirt 0.130 kettles 0.129 ridges 0.122 location 0.121 |
Glaciers formed much of the observable surface in large areas of Mars. Most of the area in high latitudes, especially the Ismenius Lacus quadrangle , is believed to still contain enormous amounts of water ice. [1] [2] Recent evidence has led many planetary scientists to believe that water ice still exists in the form of glaciers that are covered with a thin layer of insulating rock. [3] [4] [5] [6] [7] [8] In March 2010, scientists released the results of a radar study of an area called Deuteronilus Mensae that found widespread evidence of ice lying beneath a few meters of rock debris. [9] [10] Glaciers are believed to be associated with Fretted terrain , [11] many volcanoes, [12] [13] and even some craters. [14] |