Mars
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Orcus Patera is an enigmatic elliptical depression located between the volcanoes of Elysium Mons and Olympus Mons. This well-defined depression extends approximately 380 km by 140 km in a NNE–SSW direction. It has a rim that rises up to 1800 m above the surrounding plains, while the floor of the depression lies 400–600 m below the surroundings. The straight graben that cut across its rim are clearly seen in this image. Credit: ESA/DLR/FU Berlin (G. Neukum)
 
 
Mysterious Elongated Crater
Orcus Patera is an enigmatic elliptical depression located between the volcanoes of Elysium Mons and Olympus Mons. This well-defined depression extends approximately 380 km by 140 km in a NNE–SSW direction. It has a rim that rises up to 1800 m above the surrounding plains, while the floor of the depression lies 400–600 m below the surroundings. Credit: ESA/DLR/FU Berlin (G. Neukum)
 
 
Mysterious Elongated Crater
Orcus Patera is an enigmatic elliptical depression located between the volcanoes of Elysium Mons and Olympus Mons. This well-defined depression extends approximately 380 km by 140 km in a NNE–SSW direction. It has a rim that rises up to 1800 m above the surrounding plains, while the floor of the depression lies 400–600 m below the surroundings. The term ‘patera’ is used for deep, complex or irregularly shaped volcanic craters such as the Hadriaca Patera and Tyrrhena Patera at the north-eastern margin of the Hellas impact basin. However, despite its name and the fact that it is positioned near volcanoes, the actual origin of Orcus Patera remains unclear. Credit: ESA/DLR/FU Berlin (G. Neukum)
 
 
Mysterious Elongated Crater
Deep valleys dominate this section of the Magellan Crater on Mars. They may have been created by the enormous stresses places on the planet's crust by the upsurge of the Tharsis region. Credit: ESA/DLR/FU Berlin (G. Neukum)
 
 
Rocky mounds and a plateau on Mars
Looking towards Magellan Crater across the smooth plateau and the rock mounds of the region. Credit: ESA/DLR/FU Berlin (G. Neukum)
 
 
Rocky mounds and a plateau on Mars
Meridiani Planum, at the northern edge of the southern highlands of Mars, lies between the volcanic Tharsis Region to the west and the low-lying Hellas Planitia impact basin to the south-east. Through a telescope, Meridiani Planum is a striking, dark feature, close to the martian equator. It extends 127 km by 63 km and covers an area of roughly 8000 sq km, about the size of Cyprus. This dark material probably resembles volcanic ash, which is predominantly composed of minerals such as pyroxene and olivine. Credit: ESA/DLR/FU Berlin (G. Neukum)
 
 
Volcanic ash in Meridiani Planum
Meridiani Planum, at the northern edge of the southern highlands of Mars, lies between the volcanic Tharsis Region to the west and the low-lying Hellas Planitia impact basin to the south-east. Through a telescope, Meridiani Planum is a striking, dark feature, close to the martian equator. It extends 127 km by 63 km and covers an area of roughly 8000 sq km, about the size of Cyprus. This dark material probably resembles volcanic ash, which is predominantly composed of minerals such as pyroxene and olivine. Credit: ESA/DLR/FU Berlin (G. Neukum)
 
 
Volcanic ash in Meridiani Planum
Meridiani Planum, at the northern edge of the southern highlands of Mars, lies between the volcanic Tharsis Region to the west and the low-lying Hellas Planitia impact basin to the south-east. Through a telescope, Meridiani Planum is a striking, dark feature, close to the martian equator. It extends 127 km by 63 km and covers an area of roughly 8000 sq km, about the size of Cyprus. This dark material probably resembles volcanic ash, which is predominantly composed of minerals such as pyroxene and olivine. Credit: ESA/DLR/FU Berlin (G. Neukum)
 
 
Volcanic ash in Meridiani Planum
The High Resolution Stereo Camera (HRSC) onboard the ESA spacecraft Mars Express took this image of the Phobos Grunt landing area using the HRSC nadir channel on 7 March 2010, HRSC Orbit 7915. The image resolution is 4.4m per pixel and the insert marks the proposed landing region and sites for Phobos-Grunt. Credit: ESA/DLR/FU Berlin (G. Neukum)
 
 
Phobos 7 March 2010 flyby image
The High Resolution Stereo Camera (HRSC) onboard the ESA spacecraft Mars Express took this image of Phobos using the HRSC nadir channel on 7 March 2010, HRSC Orbit 7915. This image has additionally been enhanced photometrically for better bringing features in the less illuminated part. Resolution: about 4.4 meters per pixel. Credit: ESA/DLR/FU Berlin (G. Neukum)
 
 
Phobos 7 March 2010 flyby image
Kasei Valles and Sacra Fossae, in perspective. Credit: ESA/DLR/FU Berlin (G. Neukum)
 
 
Kasei Valles and Sacra Fossae
Kasei Valles and Sacra Fossae, in perspective. Credit: ESA/DLR/FU Berlin (G. Neukum)
 
 
Kasei Valles and Sacra Fossae
Daedalia Planum is a sparsely cratered, untextured plain that lies to the south-east of Arsia Mons, one of the largest volcanoes on Mars. It is 350 km in diameter and rises 14 km. The plain is dominated by numerous lava flows of varying ages. The images are centred at 21°S/ 243°E. They cover about 150 x 75 km or 11 250 sq km, an area roughly the size of Jamaica, and have a ground resolution of about 17m/ pixel. Credit: ESA/DLR/FU Berlin (G. Neukum)
 
 
Daedalia Planum in perspective
Daedalia Planum is a sparsely cratered, untextured plain that lies to the south-east of Arsia Mons, one of the largest volcanoes on Mars. It is 350 km in diameter and rises 14 km. The plain is dominated by numerous lava flows of varying ages. The images are centred at 21°S/ 243°E. They cover about 150 x 75 km or 11 250 sq km, an area roughly the size of Jamaica, and have a ground resolution of about 17m/ pixel. Credit: ESA/DLR/FU Berlin (G. Neukum)
 
 
Daedalia Planum in perspective
Daedalia Planum is a sparsely cratered, untextured plain that lies to the south-east of Arsia Mons, one of the largest volcanoes on Mars. It is 350 km in diameter and rises 14 km. The plain is dominated by numerous lava flows of varying ages. The images are centred at 21°S/ 243°E. They cover about 150 x 75 km or 11 250 sq km, an area roughly the size of Jamaica, and have a ground resolution of about 17m/ pixel. Credit: ESA/DLR/FU Berlin (G. Neukum)
 
 
Daedalia Planum in perspective
Daedalia Planum is a sparsely cratered, untextured plain that lies to the south-east of Arsia Mons, one of the largest volcanoes on Mars. It is 350 km in diameter and rises 14 km. The plain is dominated by numerous lava flows of varying ages. The images are centred at 21°S/ 243°E. They cover about 150 x 75 km or 11 250 sq km, an area roughly the size of Jamaica, and have a ground resolution of about 17m/pixel. Credit: ESA/DLR/FU Berlin (G. Neukum)
 
 
Lava flows in Daedalia Planum
Mars Express image of a region close to Ma'adim Vallis, one of the largest canyons on Mars. After Valles Marineris, Ma'adim Vallis is one of the largest canyons on Mars. The imaged region lies south-east of Ma'adim Vallis; the pictures are centred at about 29°S and 182°E and have a ground resolution of 15 m/pixel. Ma'adim Vallis is located between the volcanic region of Tharsis, which harbours four volcanoes, including the largest in the Solar System, and the Hellas Planitia impact basin. The canyon, 20 km wide and 2 km deep, originates in the southern highlands close to the 'dichotomy boundary' and ends in Gusev crater. The dichotomy boundary is a narrow region separating the cratered highlands, located mostly in the southern hemisphere of Mars, from the northern hemisphere's lowland plains. The images cover 138 x 70 km, roughly the size of Cyprus. A sharp boundary is visible in the centre, dividing dark material to the west and light material to the east. Scientists suspect that this feature is most likely the edge of a basaltic lava flow. Wrinkle ridges are clearly visible on the surface of the lava flow. They were most likely formed by compressive forces. To the north is a crater, almost 20 km in size. It is partially filled with lava, which shows that it must have formed before the lava set in. The smaller, 7 km crater at the southern edge of the larger crater must have formed later because it has an ejecta blanket that may have formed from material rich in water-ice ejected during impact. Credits: ESA/DLR/FU Berlin (G. Neukum)
 
 
Close to Ma'adim Vallis, perspective view
Mars Express image of a region close to Ma'adim Vallis, one of the largest canyons on Mars. After Valles Marineris, Ma'adim Vallis is one of the largest canyons on Mars. The imaged region lies south-east of Ma'adim Vallis; the pictures are centred at about 29°S and 182°E and have a ground resolution of 15 m/pixel. Ma'adim Vallis is located between the volcanic region of Tharsis, which harbours four volcanoes, including the largest in the Solar System, and the Hellas Planitia impact basin. The canyon, 20 km wide and 2 km deep, originates in the southern highlands close to the 'dichotomy boundary' and ends in Gusev crater. The dichotomy boundary is a narrow region separating the cratered highlands, located mostly in the southern hemisphere of Mars, from the northern hemisphere's lowland plains. The images cover 138 x 70 km, roughly the size of Cyprus. A sharp boundary is visible in the centre, dividing dark material to the west and light material to the east. Scientists suspect that this feature is most likely the edge of a basaltic lava flow. Credit: ESA/DLR/FU Berlin (G. Neukum)
 
 
Close to Ma'adim Vallis, perspective view
Mars Express image of a region close to Ma'adim Vallis, one of the largest canyons on Mars. After Valles Marineris, Ma'adim Vallis is one of the largest canyons on Mars. The imaged region lies south-east of Ma'adim Vallis; the pictures are centred at about 29°S and 182°E and have a ground resolution of 15 m/pixel. Ma'adim Vallis is located between the volcanic region of Tharsis, which harbours four volcanoes, including the largest in the Solar System, and the Hellas Planitia impact basin. The canyon, 20 km wide and 2 km deep, originates in the southern highlands close to the 'dichotomy boundary' and ends in Gusev crater. The dichotomy boundary is a narrow region separating the cratered highlands, located mostly in the southern hemisphere of Mars, from the northern hemisphere's lowland plains. The images cover 138 x 70 km, roughly the size of Cyprus. A sharp boundary is visible in the centre, dividing dark material to the west and light material to the east. Scientists suspect that this feature is most likely the edge of a basaltic lava flow. Wrinkle ridges are clearly visible on the surface of the lava flow. They were most likely formed by compressive forces. To the north is a crater, almost 20 km in size. It is partially filled with lava, which shows that it must have formed before the lava set in. The smaller, 7 km crater at the southern edge of the larger crater must have formed later because it has an ejecta blanket that may have formed from material rich in water-ice ejected during impact. A linear feature, more than 200 km long, divides the image almost in the centre. It is most likely a trough associated with the uprising of the Tharsis volcanic region in the north-east. The uprising may have created a lot of stress in the crust which was released when the fracture zones formed, creating the trough. Credit: ESA/DLR/FU Berlin (G. Neukum)
 
 
Close to Ma'adim Vallis, perspective view
Mars Express image of a region close to Ma'adim Vallis, one of the largest canyons on Mars. After Valles Marineris, Ma'adim Vallis is one of the largest canyons on Mars. The imaged region lies south-east of Ma'adim Vallis; the pictures are centred at about 29°S and 182°E and have a ground resolution of 15 m/pixel. Ma'adim Vallis is located between the volcanic region of Tharsis, which harbours four volcanoes, including the largest in the Solar System, and the Hellas Planitia impact basin. The canyon, 20 km wide and 2 km deep, originates in the southern highlands close to the 'dichotomy boundary' and ends in Gusev crater. The dichotomy boundary is a narrow region separating the cratered highlands, located mostly in the southern hemisphere of Mars, from the northern hemisphere's lowland plains. Credit: ESA/DLR/FU Berlin (G. Neukum)
 
 
Close to Ma'adim Vallis
This image of Hephaestus Fossae was obtained by ESA's Mars Express orbiter on 28 December 2007. The region is dotted with craters and channel systems and lies at about 21° North and 126° East on the Red Planet. Named after the Greek god of fire, Hephaestus Fossae extends for more than 600 km on the western flank of Elysium Mons in the Utopia Planitia region. The surface is mostly smooth, and is covered by several small impact craters measuring 800 to 2800 m in diameter. Smaller craters are scattered across the entire region. A larger impact crater measuring 20 km in diameter is a prominent feature. Covering an area of approximately 150 sq km, this crater could harbour cities such as Bonn or Kiel. In contrast to the smaller craters, it shows a blanket of ejecta with flow forms surrounding the rim. The large craters were formed when loose, soft material was ejected due to impact, and the smaller ones formed due to secondary impacts, when consolidated material was ejected in a ballistic path and impacted the original crater at varying distances. Most martian water exists in the form of subsurface ice. The presence of a blanket of ejecta and outflow channels around the crater suggest that the primary impact may have penetrated the surface enough to melt a buried frozen water reservoir. Credits: ESA/DLR/FU Berlin (G. Neukum)
 
 
Hephaestus Fossae Perspective View
This image of Hephaestus Fossae was obtained by ESA's Mars Express orbiter on 28 December 2007. The region is dotted with craters and channel systems and lies at about 21° North and 126° East on the Red Planet. Named after the Greek god of fire, Hephaestus Fossae extends for more than 600 km on the western flank of Elysium Mons in the Utopia Planitia region. The surface is mostly smooth, and is covered by several small impact craters measuring 800 to 2800 m in diameter. Smaller craters are scattered across the entire region. The left side of the image shows a large impact crater measuring 20 km in diameter. Covering an area of approximately 150 sq km, a crater of this size on Earth could harbour cities such as Bonn or Kiel. In contrast to the smaller craters, it shows a blanket of ejecta with flow forms surrounding the rim. Credits: ESA/DLR/FU Berlin (G. Neukum)
 
 
Hephaestus Fossae Perspective View
This image of Hephaestus Fossae was obtained by ESA's Mars Express orbiter on 28 December 2007. The region is dotted with craters and channel systems and lies at about 21° North and 126° East on the Red Planet. Named after the Greek god of fire, Hephaestus Fossae extends for more than 600 km on the western flank of Elysium Mons in the Utopia Planitia region. The surface is mostly smooth, and is covered by several small impact craters measuring 800 to 2800 m in diameter. Smaller craters are scattered across the entire region. The left side of the image shows a large impact crater measuring 20 km in diameter. Covering an area of approximately 150 sq km, a crater of this size on Earth could harbour cities such as Bonn or Kiel. In contrast to the smaller craters, it shows a blanket of ejecta with flow forms surrounding the rim. Credits: ESA/DLR/FU Berlin (G. Neukum)
 
 
Hephaestus Fossae Perspective View
This image, taken by the Mars Express High Resolution Stereo Camera, shows the region of Ariadnes Colles on the Red Planet. The image data was acquired on 16 April 2007 in the region of Ariadnes Colles that lies at about 34° south and 172° east. The ground resolution is about 13 m/pixel. Credits: ESA/DLR/FU Berlin (G. Neukum)
 
 
Ariadnes Colles, perspective view
This image, taken by the Mars Express High Resolution Stereo Camera, shows the region of Ariadnes Colles on the Red Planet. The image data was acquired on 16 April 2007 in the region of Ariadnes Colles that lies at about 34° south and 172° east. The ground resolution is about 13 m/pixel. Credits: ESA/DLR/FU Berlin (G. Neukum)
 
 
Ariadnes Colles, nadir view
ESA's Mars Express orbiter imaged the snow-laden region of Rupes Tenuis on the martian north pole on 29 July 2008. Rupes Tenuis is located at the southern edge of the martian north polar cap, approximately 5500 km northeast of the Tharsis volcanic region. The images are at about 81° north and 297° east and have a ground resolution of approximately 41 m/pixel. They cover an area of about 44 000 km2, almost as large as the Netherlands. Credits: ESA/DLR/FU Berlin (G. Neukum)
 
 
Rupes Tenuis perspective view
ESA's Mars Express orbiter imaged the snow-laden region of Rupes Tenuis on the martian north pole on 29 July 2008. Rupes Tenuis is located at the southern edge of the martian north polar cap, approximately 5500 km northeast of the Tharsis volcanic region. The images are at about 81° north and 297° east and have a ground resolution of approximately 41 m/pixel. They cover an area of about 44 000 km2, almost as large as the Netherlands. Credits: ESA/DLR/FU Berlin (G. Neukum)
 
 
Rupes Tenuis nadir view
Crommelin Crater on Mars, an area where Light Toned Deposits, or LTD, are known to be present. An analysis of data and images from Mars Express suggests that several LTD, some of the least understood structures on Mars, were formed when large amounts of groundwater burst on to the surface. Scientists propose that groundwater had a greater role in shaping the martian surface than previously believed, and may have sheltered primitive life forms as the planet started drying up. This is a mosaic composed of nadir images taken by the High Resolution Stereo Camera on board ESA’s Mars Express spacecraft. Credit: ESA/DLR/FU Berlin (G. Neukum)
 
 
Crommelin Crater
Iani Chaos on Mars, an area where Light Toned Deposits, or LTD, are known to be present. An analysis of data and images from Mars Express suggests that several LTD, some of the least understood structures on Mars, were formed when large amounts of groundwater burst on to the surface. Scientists propose that groundwater had a greater role in shaping the martian surface than previously believed, and may have sheltered primitive life forms as the planet started drying up. This image was obtained with the High Resolution Stereo Camera on board ESA’s Mars Express spacecraft. Credit: ESA/DLR/FU Berlin (G. Neukum)
 
 
Iani Chaos
The High Resolution Stereo Camera on board ESA's Mars Express imaged the Eumenides Dorsum mountains on the Red Planet. Eumenides Dorsum is located in to the west of the Tharsis Region, and forms part of the Medusae-Fossae Region, at approximately 2° south and 206° east. The images, taken on 26 December 2007, have a ground resolution of about 13 m/pixel and cover an area of about 12 000 square km. Credit: ESA/DLR/FU Berlin (G. Neukum)
 
 
Perspective view of Euminedes Dorsum
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