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Images of 'Impact' found, 2,344

 
Tenoumer Impact Crater, Mauritania (photo)

PIX5973683

Tenoumer Impact Crater, Mauritania (photo)

PIX5973683

 
Impact Crater Vredefort, South Africa (photo)

PIX5973684

Impact Crater Vredefort, South Africa (photo)

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Impact Crater Wolf Creek, Australia - Area around Wolf Creek impact crater, Australia - Part of the Great Sable Desert with Wolf Creek impact crater (or Wolfe Creek, top left) in Australia, seen by Terra satellite on September 22, 2006. It would have been formed about 300,000 years ago and its diameter is 880 metres. Wolfe Creek Crater lies on the edge of the Great Sandy Desert approximately 90 km south of Halls Creek in Western Australia. Almost circular, Wolfe Creek Crater (also known as Wolf Creek Crater, top middle left) is considered the second largest crater in the world from which meteorite fragments have been collected. Because of its excellent preservation, the crater clearly shows the classic features that result from a large meteorite striking the Earth. The Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) on Nasa's Terra satellite captured this image of Wolfe Creek Crater on September 22, 2006. The Australian Outback appears mostly in varying earth ton

PIX4630615

Impact Crater Wolf Creek, Australia - Area around Wolf Creek impact crater, Australia - Part of the Great Sable Desert with Wolf Creek impact crater (or Wolfe Creek, top left) in Australia, seen by Terra satellite on September 22, 2006. It would have been formed about 300,000 years ago and its diameter is 880 metres. Wolfe Creek Crater lies on the edge of the Great Sandy Desert approximately 90 km south of Halls Creek in Western Australia. Almost circular, Wolfe Creek Crater (also known as Wolf Creek Crater, top middle left) is considered the second largest crater in the world from which meteorite fragments have been collected. Because of its excellent preservation, the crater clearly shows the classic features that result from a large meteorite striking the Earth. The Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) on Nasa's Terra satellite captured this image of Wolfe Creek Crater on September 22, 2006. The Australian Outback appears mostly in varying earth ton

PIX4630615

 
Crater Bacolor on Mars - Bacolor Crater on planet Mars - View of the impact crater Bacolor obtained by the Mars Odyssey probe. It's an impact crater about 20 km in diameter. Bacolor Crater is a magnificent impact feature about 20 kilometers (12 miles) wide. The lines on the ejecta blanket surrounding the crater rim come from a surge of superheated gas and debris flying outward in the wake of the meteorite impact that made the crater. This view combines images taken during the period from September 2002 to October 2005 by the Thermal Emission Imaging System instrument on Nasa's Mars Odyssey orbiter. The pictured location on Mars is 33 degrees north latitude, 118.6 degrees east longitude

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Crater Bacolor on Mars - Bacolor Crater on planet Mars - View of the impact crater Bacolor obtained by the Mars Odyssey probe. It's an impact crater about 20 km in diameter. Bacolor Crater is a magnificent impact feature about 20 kilometers (12 miles) wide. The lines on the ejecta blanket surrounding the crater rim come from a surge of superheated gas and debris flying outward in the wake of the meteorite impact that made the crater. This view combines images taken during the period from September 2002 to October 2005 by the Thermal Emission Imaging System instrument on Nasa's Mars Odyssey orbiter. The pictured location on Mars is 33 degrees north latitude, 118.6 degrees east longitude

PIX4616373

 
Vredefort impact crater - South Africa - Vredefort impact crater, South Africa - Vredefort impact crater in South Africa is the largest impact crater on Earth and one of the oldest. Its diameter is 300 km; it would have been formed 2 billion years ago. Image obtained from the International Space Station (ISS) on 27 June 2009. Vredefort crater is the largest impact crater on earth and one of the oldest known impact crater. Its diameter is 300 km and its age is estimated to be 2 billion years. Image taken from the international space station (ISS) on June 27, 2009

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Vredefort impact crater - South Africa - Vredefort impact crater, South Africa - Vredefort impact crater in South Africa is the largest impact crater on Earth and one of the oldest. Its diameter is 300 km; it would have been formed 2 billion years ago. Image obtained from the International Space Station (ISS) on 27 June 2009. Vredefort crater is the largest impact crater on earth and one of the oldest known impact crater. Its diameter is 300 km and its age is estimated to be 2 billion years. Image taken from the international space station (ISS) on June 27, 2009

PIX4630677

 
Pingualuit crater seen by satellite - Pingualuit crater seen by satellite - The Pingualuit crater, formerly known as the New Quebec crater, is located at the northern end of Quebec, Nunavik. It's a crater caused by the impact of a meteorite that fell about 1.4 million years ago. Visible to the left of the image, this almost perfectly circular impact crater measures about 3.4 km in diameter and houses a lake 260 metres deep. Image obtained by Landsat-7 satellite on 17 August 2002. Nasa's Landsat 7 satellite captured this image of Pingualuit Crater (a meteorite crater produced from an impact roughly 1.4 million years ago) on August 17, 2002. In this image, water appears blue, and land appears in varying shades of beige. The high latitude of the area limits vegetation, so thick, lush forests do not flourish in this region. With a diameter of 3.44 kilometers (2.14 miles), Pingualuit Crater holds a lake about 267 meters (876 feet) deep. The crater is the blue circle visible in the left part

PIX4630763

Pingualuit crater seen by satellite - Pingualuit crater seen by satellite - The Pingualuit crater, formerly known as the New Quebec crater, is located at the northern end of Quebec, Nunavik. It's a crater caused by the impact of a meteorite that fell about 1.4 million years ago. Visible to the left of the image, this almost perfectly circular impact crater measures about 3.4 km in diameter and houses a lake 260 metres deep. Image obtained by Landsat-7 satellite on 17 August 2002. Nasa's Landsat 7 satellite captured this image of Pingualuit Crater (a meteorite crater produced from an impact roughly 1.4 million years ago) on August 17, 2002. In this image, water appears blue, and land appears in varying shades of beige. The high latitude of the area limits vegetation, so thick, lush forests do not flourish in this region. With a diameter of 3.44 kilometers (2.14 miles), Pingualuit Crater holds a lake about 267 meters (876 feet) deep. The crater is the blue circle visible in the left part

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Mars: craters and channels in Hephaestus Fossae - Mars: craters and channels in Hephaestus Fossae - Impact crateres and channel system in Hephaestus Fossae, a region on Mars located on the western flank of Elysium Mons. Close-up of a large impact crater measuring 20 km in diameter. The image was obtained by the Mars Express probe on December 28, 2007. 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 image shows a large impact crater measuring 20 km in diameter. It shows a blanket of ejecta with flow forms surrounding the rim

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Mars: craters and channels in Hephaestus Fossae - Mars: craters and channels in Hephaestus Fossae - Impact crateres and channel system in Hephaestus Fossae, a region on Mars located on the western flank of Elysium Mons. Close-up of a large impact crater measuring 20 km in diameter. The image was obtained by the Mars Express probe on December 28, 2007. 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 image shows a large impact crater measuring 20 km in diameter. It shows a blanket of ejecta with flow forms surrounding the rim

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Mars: craters and channels in Hephaestus Fossae - Mars: craters and channels in Hephaestus Fossae - Impact crateres and channel system in Hephaestus Fossae, a region on Mars located on the western flank of Elysium Mons. The large impact crater at the top of the picture is 20 km in diameter. The image covering an area of about 150 square km was obtained by the Mars Express probe on 28 December 2007. 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 f

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Mars: craters and channels in Hephaestus Fossae - Mars: craters and channels in Hephaestus Fossae - Impact crateres and channel system in Hephaestus Fossae, a region on Mars located on the western flank of Elysium Mons. The large impact crater at the top of the picture is 20 km in diameter. The image covering an area of about 150 square km was obtained by the Mars Express probe on 28 December 2007. 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 f

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Cratere Manicouagan - Quebec - January 2014 - The Manicouagan Impact Crater reservoir in Quebec, Canada - Cratere d'impact Manicouagan, Quebec, seen from the International Space Station (ISS) on January 2, 2014. This 100-kilometre crater formed 212 million years ago, following the fall of an asteroid on Earth. One of the Expedition 38 crew members aboard the Earth - orbiting International Space Station recorded this image which features the Manicouagan Crater and reservoir located primarily in Manicouagan Regional County Municipality in the Cote - Nord region of Quebec, Canada. Scientists believe the crater was caused by the impact of a 5 kilometer (3 mile) diameter asteroid about 215.5 million years ago (Triassic Period). The crater is a multiple - ring structure about 100 kilometers (60 miles) across, with its 70 kilometer (40 mile) diameter inner ring as its most prominent feature; it contains a 70 kilometer (40 mile) diameter annular lake, the Manicouagan Reservoir, surrounding an

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Cratere Manicouagan - Quebec - January 2014 - The Manicouagan Impact Crater reservoir in Quebec, Canada - Cratere d'impact Manicouagan, Quebec, seen from the International Space Station (ISS) on January 2, 2014. This 100-kilometre crater formed 212 million years ago, following the fall of an asteroid on Earth. One of the Expedition 38 crew members aboard the Earth - orbiting International Space Station recorded this image which features the Manicouagan Crater and reservoir located primarily in Manicouagan Regional County Municipality in the Cote - Nord region of Quebec, Canada. Scientists believe the crater was caused by the impact of a 5 kilometer (3 mile) diameter asteroid about 215.5 million years ago (Triassic Period). The crater is a multiple - ring structure about 100 kilometers (60 miles) across, with its 70 kilometer (40 mile) diameter inner ring as its most prominent feature; it contains a 70 kilometer (40 mile) diameter annular lake, the Manicouagan Reservoir, surrounding an

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Mercury seen by the Messenger probe - Mercury seen by Messenger spacecraft - Image of Mercury, obtained by the Messenger probe on October 6, 2008. The bright crater in the middle of the picture down is the Kuiper crater. The large striations north and east of the crater are observed for the first time by a space probe. Recolorised image. The spectacular image shows the departing planet taken about 90 minutes after the spacecraft's closest approach to Mercury on October 6, 2008. The bright crater just south of the center of the image is Kuiper, identified on images from the Mariner 10 mission in the 1970s. For most of the terrain east of Kuiper, toward the limb (edge) of the planet, the departing images are the first spacecraft views of that portion of Mercury's surface. A striking characteristic of this newly imaged area is the large pattern of rays that extend from the northern region of Mercury to regions south of Kuiper. This extensive ray system appears to emanate from a relatively

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Mercury seen by the Messenger probe - Mercury seen by Messenger spacecraft - Image of Mercury, obtained by the Messenger probe on October 6, 2008. The bright crater in the middle of the picture down is the Kuiper crater. The large striations north and east of the crater are observed for the first time by a space probe. Recolorised image. The spectacular image shows the departing planet taken about 90 minutes after the spacecraft's closest approach to Mercury on October 6, 2008. The bright crater just south of the center of the image is Kuiper, identified on images from the Mariner 10 mission in the 1970s. For most of the terrain east of Kuiper, toward the limb (edge) of the planet, the departing images are the first spacecraft views of that portion of Mercury's surface. A striking characteristic of this newly imaged area is the large pattern of rays that extend from the northern region of Mercury to regions south of Kuiper. This extensive ray system appears to emanate from a relatively

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Asteroide Ida seen by Galileo probe - Asteroid Ida seen by Galileo spacecraft - Mosaic of five images obtained by the Galileo probe on 28 August 1993 between 3000 and 3800 km from the asteroid. This view of the asteroid 243 Ida is a mosaic of five image frames acquired by the Galileo spacecraft's solid-state imaging system at ranges of 3,057 to 3,821 kilometers (1,900 to 2,375 miles) on August 28, 1993. Ida is the second asteroid ever encountered by a spacecraft. It appears to be about 52 kilometers (32 miles) in length, more than twice as large as Gaspra, the first asteroid observed by Galileo in October 1991

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Asteroide Ida seen by Galileo probe - Asteroid Ida seen by Galileo spacecraft - Mosaic of five images obtained by the Galileo probe on 28 August 1993 between 3000 and 3800 km from the asteroid. This view of the asteroid 243 Ida is a mosaic of five image frames acquired by the Galileo spacecraft's solid-state imaging system at ranges of 3,057 to 3,821 kilometers (1,900 to 2,375 miles) on August 28, 1993. Ida is the second asteroid ever encountered by a spacecraft. It appears to be about 52 kilometers (32 miles) in length, more than twice as large as Gaspra, the first asteroid observed by Galileo in October 1991

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March: chaotic terrain between Kasei Valles and Sacra Fossae - Mars: Chaotic terrain between Kasei Valles and Sacra Fossae - Region bordering Kasei Valles and Sacra Fossae. To the north, the large impact crater is 35 km in diameter. The image covering an area of 225 km by 95 km was obtained by the Mars Express probe. Mars Express flew over the boundary between Kasei Valles and Sacra Fossae and imaged the region, acquiring spectacular views of the chaotic terrain in the area. The images are centred at 12* N/285* E and have a ground resolution of about 21 m/pixel. They cover 225 x 95 km or 21.375 sq km, an area roughly half the size of the Netherlands. The image shows an old 35 km - diameter impact crater in the north. The crater's southwestern rim is eroded strongly, mostly by flowing water. The source of the water was located in Etus Chasma, which lies about 850 km to the southwest. The crater floor and the northwestern part are remarkably flat, formed by sediments and basaltic lava fl

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March: chaotic terrain between Kasei Valles and Sacra Fossae - Mars: Chaotic terrain between Kasei Valles and Sacra Fossae - Region bordering Kasei Valles and Sacra Fossae. To the north, the large impact crater is 35 km in diameter. The image covering an area of 225 km by 95 km was obtained by the Mars Express probe. Mars Express flew over the boundary between Kasei Valles and Sacra Fossae and imaged the region, acquiring spectacular views of the chaotic terrain in the area. The images are centred at 12* N/285* E and have a ground resolution of about 21 m/pixel. They cover 225 x 95 km or 21.375 sq km, an area roughly half the size of the Netherlands. The image shows an old 35 km - diameter impact crater in the north. The crater's southwestern rim is eroded strongly, mostly by flowing water. The source of the water was located in Etus Chasma, which lies about 850 km to the southwest. The crater floor and the northwestern part are remarkably flat, formed by sediments and basaltic lava fl

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Moon: Cratere Clavius - Moon: Clavius Crater: Image obtained on August 24, 2016, a day before the last quarter of the moon

Sebastian Voltmer

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Moon: Cratere Clavius - Moon: Clavius Crater: Image obtained on August 24, 2016, a day before the last quarter of the moon

Sebastian Voltmer

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Moon: Aristarchus crater - Moon: Aristarchus crater - Apollo 15 - The Aristarchus crater and the Schroeter valley. Image obtained from the Apollo 15 control module. An oblique view of Schroeter's Valley and the crater Aristarchus, as photographed by the Apollo 15 Command and Service Module (CSM) in lunar orbit. The large, bright - appearing crater to the left of the head of meandering Schroeter's Valley is Aristarchus, the center of which is located at 48 degrees west longitude and 214 degrees north latitude. The crater Aristarchus approximately 35 kilometers (about 21.75 statute miles) in diameter. The head of Schroeter's Valley, a sinuous rille in the Aristarchus Plateau in the Ocean of Storms, is called Cobra Head. Herodotus the crater just above and to the right of Cobra Head in upper center

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Moon: Aristarchus crater - Moon: Aristarchus crater - Apollo 15 - The Aristarchus crater and the Schroeter valley. Image obtained from the Apollo 15 control module. An oblique view of Schroeter's Valley and the crater Aristarchus, as photographed by the Apollo 15 Command and Service Module (CSM) in lunar orbit. The large, bright - appearing crater to the left of the head of meandering Schroeter's Valley is Aristarchus, the center of which is located at 48 degrees west longitude and 214 degrees north latitude. The crater Aristarchus approximately 35 kilometers (about 21.75 statute miles) in diameter. The head of Schroeter's Valley, a sinuous rille in the Aristarchus Plateau in the Ocean of Storms, is called Cobra Head. Herodotus the crater just above and to the right of Cobra Head in upper center

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Moon: grooves and mountain, April 1972 (photo)

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Moon: grooves and mountain, April 1972 (photo)

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Mars - Artist's View - Mars - Artwork - A view from north of Mars' equato

Steven Hobbs

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Mars - Artist's View - Mars - Artwork - A view from north of Mars' equato

Steven Hobbs

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Tethys, Saturn satellite, seen by the Cassini probe - Saturn's moon Tethys seen by Cassini spacecraft: The Tethys satellite photographed by the Cassini probe on 11 April 2015 has a distance of 53,000 km from the satellite. Tethys is about 1070 km in diameter. - This enhancement-color mosaic of Saturn's icy moon Tethys shows a range of features on the moon's trailing hemisphere. Tethys is tidally locked to Saturn, so the trailing hemisphere is the side of the moon that always faces opposite its direction of motion as it orbits the planet - Images taken using clear, green, infrared and ultraviolet spectral filters were combined to create the view, which highlights subtle color differences across Tethys' surface at wavelengths not visible to human eyes. The moon's surface is fairly uniform in natural color - The color of the surface changes conspicuously across the disk, from yellowish hues to nearly white. These broad color changes are affected by a number of external processes. First, S

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Tethys, Saturn satellite, seen by the Cassini probe - Saturn's moon Tethys seen by Cassini spacecraft: The Tethys satellite photographed by the Cassini probe on 11 April 2015 has a distance of 53,000 km from the satellite. Tethys is about 1070 km in diameter. - This enhancement-color mosaic of Saturn's icy moon Tethys shows a range of features on the moon's trailing hemisphere. Tethys is tidally locked to Saturn, so the trailing hemisphere is the side of the moon that always faces opposite its direction of motion as it orbits the planet - Images taken using clear, green, infrared and ultraviolet spectral filters were combined to create the view, which highlights subtle color differences across Tethys' surface at wavelengths not visible to human eyes. The moon's surface is fairly uniform in natural color - The color of the surface changes conspicuously across the disk, from yellowish hues to nearly white. These broad color changes are affected by a number of external processes. First, S

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Europe - Jupiter Satellite - View of the surface of the Europe satellite obtained from images made by the Galileo probe in 1995 and 1998. Jupiter's icy moon Europa looms large in this newly - reprocessed color view, made from images taken by Nasa's Galileo spacecraft in the late 1990s. This is the color view of Europa from Galileo that shows the largest portion of the moon's surface at the highest resolution. To create this new version, the images were assembled into a realistic color view of the surface that approximates how Europa would appear to the human eye. The scene shows the stunning diversity of Europa's surface geology. Long, linear cracks and ridges crisscross the surface, interrupted by regions of disrupted terrain where the surface ice crust has been broken up and re - frozen into new patterns. Color variations across the surface are associated with differences in geologic feature type and location. For example, areas that appear blue or white contain relatively pure water

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Europe - Jupiter Satellite - View of the surface of the Europe satellite obtained from images made by the Galileo probe in 1995 and 1998. Jupiter's icy moon Europa looms large in this newly - reprocessed color view, made from images taken by Nasa's Galileo spacecraft in the late 1990s. This is the color view of Europa from Galileo that shows the largest portion of the moon's surface at the highest resolution. To create this new version, the images were assembled into a realistic color view of the surface that approximates how Europa would appear to the human eye. The scene shows the stunning diversity of Europa's surface geology. Long, linear cracks and ridges crisscross the surface, interrupted by regions of disrupted terrain where the surface ice crust has been broken up and re - frozen into new patterns. Color variations across the surface are associated with differences in geologic feature type and location. For example, areas that appear blue or white contain relatively pure water

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Mars: craters and channels in Hephaestus Fossae - Mars: craters and channels in Hephaestus Fossae - Impact crateres and channel system in Hephaestus Fossae, a region on Mars located on the western flank of Elysium Mons. The large impact crater on the left of the image measures 20 km in diameter. The image covering an area of about 150 square km was obtained by the Mars Express probe on 28 December 2007. 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 measuri

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Mars: craters and channels in Hephaestus Fossae - Mars: craters and channels in Hephaestus Fossae - Impact crateres and channel system in Hephaestus Fossae, a region on Mars located on the western flank of Elysium Mons. The large impact crater on the left of the image measures 20 km in diameter. The image covering an area of about 150 square km was obtained by the Mars Express probe on 28 December 2007. 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 measuri

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Asteroide Ida seen by Galileo probe - Asteroid Ida seen by Galileo spacecraft - Mosaic of five images obtained by the Galileo probe on 28 August 1993 between 3000 and 3800 km from the asteroid. Recolorised image. This false-color view of the asteroid 243 Ida is a mosaic of five image frames acquired by the Galileo spacecraft's solid-state imaging system at ranges of 3,057 to 3,821 kilometers (1,900 to 2,375 miles) on August 28, 1993. Ida is the second asteroid ever encountered by a spacecraft. It appears to be about 52 kilometers (32 miles) in length, more than twice as large as Gaspra, the first asteroid observed by Galileo in October 1991

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Asteroide Ida seen by Galileo probe - Asteroid Ida seen by Galileo spacecraft - Mosaic of five images obtained by the Galileo probe on 28 August 1993 between 3000 and 3800 km from the asteroid. Recolorised image. This false-color view of the asteroid 243 Ida is a mosaic of five image frames acquired by the Galileo spacecraft's solid-state imaging system at ranges of 3,057 to 3,821 kilometers (1,900 to 2,375 miles) on August 28, 1993. Ida is the second asteroid ever encountered by a spacecraft. It appears to be about 52 kilometers (32 miles) in length, more than twice as large as Gaspra, the first asteroid observed by Galileo in October 1991

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Cratere Erlanger sur la Lune - Erlanger crater near Moon north pole - Erlanger cratere is located 90 km from the north pole of the Moon. The bottom of this 10 km-diameter crater rarely receives the sun's rays. In this image obtained on August 8, 2009 by the LRO probe (Lunar Reconnaissance Orbiter), only the edges of the crater are illuminated by the Sun. Bed view of Erlanger, crater 10 km (6 miles) across just 90 km (50 miles) from the Moon's north pole. The Sun is perpetually on the horizon as seen from the crater, and only the raised rim is ever lit. In this shot almost the entire circle of the rim can be seen, poking into the sunlight. The crater has steep walls, and the bottom almost never sees sunlight. Image taken by the Lunar Reconnaissance Orbiter's (LRO) instrument on august 8 2009

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Cratere Erlanger sur la Lune - Erlanger crater near Moon north pole - Erlanger cratere is located 90 km from the north pole of the Moon. The bottom of this 10 km-diameter crater rarely receives the sun's rays. In this image obtained on August 8, 2009 by the LRO probe (Lunar Reconnaissance Orbiter), only the edges of the crater are illuminated by the Sun. Bed view of Erlanger, crater 10 km (6 miles) across just 90 km (50 miles) from the Moon's north pole. The Sun is perpetually on the horizon as seen from the crater, and only the raised rim is ever lit. In this shot almost the entire circle of the rim can be seen, poking into the sunlight. The crater has steep walls, and the bottom almost never sees sunlight. Image taken by the Lunar Reconnaissance Orbiter's (LRO) instrument on august 8 2009

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The disappearance of dinosaurs - Artist view - Tertiary dawn - Artist view - Artist view of the impact of the asteroid responsible for the disappearance of dinosaurs, about 65 million years ago. The last seconds before the asteroid impact that ended the age of dinosaurs

S. Numazawa

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The disappearance of dinosaurs - Artist view - Tertiary dawn - Artist view - Artist view of the impact of the asteroid responsible for the disappearance of dinosaurs, about 65 million years ago. The last seconds before the asteroid impact that ended the age of dinosaurs

S. Numazawa

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Mars: crateres and canals in Hephaestus Fossae - Impact crateres and channel system in Hephaestus Fossae, a region on Mars located on the western flank of Elysium Mons. The large impact crater on the left is 20 km in diameter. The image covering an area of about 150 square km was obtained by the Mars Express probe on 28 December 2007. 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. This image covering an area of approximately 150 km exhibits a large impact crater measuring 20 kilometers in diameter. 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

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Mars: crateres and canals in Hephaestus Fossae - Impact crateres and channel system in Hephaestus Fossae, a region on Mars located on the western flank of Elysium Mons. The large impact crater on the left is 20 km in diameter. The image covering an area of about 150 square km was obtained by the Mars Express probe on 28 December 2007. 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. This image covering an area of approximately 150 km exhibits a large impact crater measuring 20 kilometers in diameter. 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

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March: chaotic terrain between Kasei Valles and Sacra Fossae - Mars: Chaotic terrain between Kasei Valles and Sacra Fossae - Region bordering Kasei Valles and Sacra Fossae. The large impact crater is 35 km in diameter. The image covering an area of 225 km by 95 km was obtained by the Mars Express probe. Mars Express flew over the boundary between Kasei Valles and Sacra Fossae and imaged the region, acquiring spectacular views of the chaotic terrain in the area. The images are centred at 12* N/285* E and have a ground resolution of about 21 m/pixel. They cover 225 x 95 km or 21.375 sq km, an area roughly half the size of the Netherlands. The image shows an old 35 km - diameter impact crater in the north. The crater's southwestern rim is eroded strongly, mostly by flowing water. The source of the water was located in Echo Chasma, which lies about 850 km to the southwest

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March: chaotic terrain between Kasei Valles and Sacra Fossae - Mars: Chaotic terrain between Kasei Valles and Sacra Fossae - Region bordering Kasei Valles and Sacra Fossae. The large impact crater is 35 km in diameter. The image covering an area of 225 km by 95 km was obtained by the Mars Express probe. Mars Express flew over the boundary between Kasei Valles and Sacra Fossae and imaged the region, acquiring spectacular views of the chaotic terrain in the area. The images are centred at 12* N/285* E and have a ground resolution of about 21 m/pixel. They cover 225 x 95 km or 21.375 sq km, an area roughly half the size of the Netherlands. The image shows an old 35 km - diameter impact crater in the north. The crater's southwestern rim is eroded strongly, mostly by flowing water. The source of the water was located in Echo Chasma, which lies about 850 km to the southwest

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Cratere Manicouagan - Quebec - March 2008 - The Manicouagan Impact Crater reservoir in Quebec, Canada - Cratere d'impact Manicouagan, Quebec, seen from the International Space Station (ISS) in March 2008. This 100-kilometre crater formed 212 million years ago, following the fall of an asteroid on Earth. The reservoir, a large annular lake, marks the site of an impact crater 60 miles (100 kilometers) wide. Formed almost 212 million years ago when a large meteorite hit Earth, the crater has been worn down by many advances and retreats of glaciers and other processes of erosion. Seen here from the International Space Station (ISS) in March 2008

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Cratere Manicouagan - Quebec - March 2008 - The Manicouagan Impact Crater reservoir in Quebec, Canada - Cratere d'impact Manicouagan, Quebec, seen from the International Space Station (ISS) in March 2008. This 100-kilometre crater formed 212 million years ago, following the fall of an asteroid on Earth. The reservoir, a large annular lake, marks the site of an impact crater 60 miles (100 kilometers) wide. Formed almost 212 million years ago when a large meteorite hit Earth, the crater has been worn down by many advances and retreats of glaciers and other processes of erosion. Seen here from the International Space Station (ISS) in March 2008

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Traces of flow on Mars - Mars: gullies on impact crater wall - Gullies along a wall of an impact crater (Hale crater). These ravines are thought to indicate the presence of liquid water in the Martian basement. Image obtained by the Mars Reconnaissance Orbiter probe on August 3, 2009. Gullies, on Earth, are usually formed through the action of liquid water. Whether gullies form under today's cold dry conditions on Mars is a major question that planetary scientists are trying to answer. The gullies pictured here in Hale crater are great examples of what a typical Martian gully looks like. Wide V - shaped channels running downhill (from top to bottom) where the material that carved the gully flowed. At the bottom of the channel this material empties out onto a fan - shaped mound. Several gullies are visible here and the fans from each gully overlap one other in complicated ways. Image taken on August 3, 2009 by the HIRISE camera on Nasa's Mars Reconnaissance Orbiter

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Traces of flow on Mars - Mars: gullies on impact crater wall - Gullies along a wall of an impact crater (Hale crater). These ravines are thought to indicate the presence of liquid water in the Martian basement. Image obtained by the Mars Reconnaissance Orbiter probe on August 3, 2009. Gullies, on Earth, are usually formed through the action of liquid water. Whether gullies form under today's cold dry conditions on Mars is a major question that planetary scientists are trying to answer. The gullies pictured here in Hale crater are great examples of what a typical Martian gully looks like. Wide V - shaped channels running downhill (from top to bottom) where the material that carved the gully flowed. At the bottom of the channel this material empties out onto a fan - shaped mound. Several gullies are visible here and the fans from each gully overlap one other in complicated ways. Image taken on August 3, 2009 by the HIRISE camera on Nasa's Mars Reconnaissance Orbiter

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Moon: King crater - Moon: King crater - The King impact crater on the hidden face of the Moon. This crater is about 75 km in diameter and 4 km in depth. Image obtained in April 1972 from the control module of Apollo 16. An oblique view of King Crater on the lunar farside, as photographed from the Apollo 16 spacecraft in lunar orbit. Note the interesting mountainous feature inside the crater. The coordinates of the center of King Crater are 120.5 degrees east longitude and 5.5 degrees north latitude. The two “” fingers”” of the central highlands in King Crater point towards the north - northwest. While astronauts John W. Young, commander; and Charles M. Duke Jr., lunar module pilot; descended in the Apollo 16 Lunar Module (LM) “” Orion””” to explore the Descartes highlands landing site on the moon, astronaut Thomas K. Mattingly II, command module pilot, remained with the Command and Service Modules (CSM) “” Casper””” in lunar orbit. April 1972

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Moon: King crater - Moon: King crater - The King impact crater on the hidden face of the Moon. This crater is about 75 km in diameter and 4 km in depth. Image obtained in April 1972 from the control module of Apollo 16. An oblique view of King Crater on the lunar farside, as photographed from the Apollo 16 spacecraft in lunar orbit. Note the interesting mountainous feature inside the crater. The coordinates of the center of King Crater are 120.5 degrees east longitude and 5.5 degrees north latitude. The two “” fingers”” of the central highlands in King Crater point towards the north - northwest. While astronauts John W. Young, commander; and Charles M. Duke Jr., lunar module pilot; descended in the Apollo 16 Lunar Module (LM) “” Orion””” to explore the Descartes highlands landing site on the moon, astronaut Thomas K. Mattingly II, command module pilot, remained with the Command and Service Modules (CSM) “” Casper””” in lunar orbit. April 1972

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Sunrise on the crater Tycho - Tycho Crater Sunrise - Sunrise on the central peak of the crater Tycho on the Moon. This crater is about 82 km in diameter and its central peak rises at 2 km above sea level. Image obtained on June 10, 2011 by the LRO (Lunar Reconnaissance Orbiter) probe. On 10 June 2011 the LRO spacecraft slewed 65* to the west, allowing the LROC NACs to capture this dramatic sunrise view of Tycho crater. A very popular target with amateur astronomers, Tycho is located at 43.37* S, 348.68* E, and is ~ 82 km (51 miles) in diameter. The summit of the central peak is 2 km (6562 ft) above the crater floor, and the crater floor is about 4700 m (15,420 ft) below the rim. Many “” clasts”” ranging in size from 10 meters to 100s of meters are exposed in the central peak slopes

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Sunrise on the crater Tycho - Tycho Crater Sunrise - Sunrise on the central peak of the crater Tycho on the Moon. This crater is about 82 km in diameter and its central peak rises at 2 km above sea level. Image obtained on June 10, 2011 by the LRO (Lunar Reconnaissance Orbiter) probe. On 10 June 2011 the LRO spacecraft slewed 65* to the west, allowing the LROC NACs to capture this dramatic sunrise view of Tycho crater. A very popular target with amateur astronomers, Tycho is located at 43.37* S, 348.68* E, and is ~ 82 km (51 miles) in diameter. The summit of the central peak is 2 km (6562 ft) above the crater floor, and the crater floor is about 4700 m (15,420 ft) below the rim. Many “” clasts”” ranging in size from 10 meters to 100s of meters are exposed in the central peak slopes

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Moon: Moscow Sea and crateres - Moon: Mare Moscoviense and craters - Part of the hidden face of the Moon with the Moscow Sea on the right. Image obtained during the Apollo 13 mission, April 1970. This oblique view of the lunar farside was photographed from the Apollo 13 spacecraft as it passed around the moon on its hazardous journey home. The large conspicuous mare area is Mare Moscoviense which is located at 146 degrees east longitude and 25 degrees north latitude. The large crater at the horizon is International Astronomical Union Crater No. 221. This view is looking northeast from the spacecraft

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Moon: Moscow Sea and crateres - Moon: Mare Moscoviense and craters - Part of the hidden face of the Moon with the Moscow Sea on the right. Image obtained during the Apollo 13 mission, April 1970. This oblique view of the lunar farside was photographed from the Apollo 13 spacecraft as it passed around the moon on its hazardous journey home. The large conspicuous mare area is Mare Moscoviense which is located at 146 degrees east longitude and 25 degrees north latitude. The large crater at the horizon is International Astronomical Union Crater No. 221. This view is looking northeast from the spacecraft

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March: Chaotic terrain between Kasei Valles and Sacra Fossae - Mars: Chaotic terrain between Kasei Valles and Sacra Fossae - Region bordering Kasei Valles (top) and Sacra Fossae (bottom). Kasei Valles is one of the largest Martian canal systems. The large impact crater on the right is 35 km in diameter. The image covering an area of 225 km by 95 km was obtained by the Mars Express probe. Mars Express flew over the boundary between Kasei Valles and Sacra Fossae and imaged the region, acquiring spectacular views of the chaotic terrain in the area. The images are centred at 12* N/285* E and have a ground resolution of about 21 m/pixel. They cover 225 x 95 km or 21.375 sq km, an area roughly half the size of the Netherlands. The upper portion of the image swath shows the eastern margin of Kasei Valles and the western margin of the Lunae Planum plateau and the adjoining Sacra Fossae. Kasei Valles is one of the largest outflow channels on Mars, spanning 3000 km, from the Chryse Planitia basi

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March: Chaotic terrain between Kasei Valles and Sacra Fossae - Mars: Chaotic terrain between Kasei Valles and Sacra Fossae - Region bordering Kasei Valles (top) and Sacra Fossae (bottom). Kasei Valles is one of the largest Martian canal systems. The large impact crater on the right is 35 km in diameter. The image covering an area of 225 km by 95 km was obtained by the Mars Express probe. Mars Express flew over the boundary between Kasei Valles and Sacra Fossae and imaged the region, acquiring spectacular views of the chaotic terrain in the area. The images are centred at 12* N/285* E and have a ground resolution of about 21 m/pixel. They cover 225 x 95 km or 21.375 sq km, an area roughly half the size of the Netherlands. The upper portion of the image swath shows the eastern margin of Kasei Valles and the western margin of the Lunae Planum plateau and the adjoining Sacra Fossae. Kasei Valles is one of the largest outflow channels on Mars, spanning 3000 km, from the Chryse Planitia basi

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Rhea, satellite of Saturn, seen by Cassini - Saturn's moon Rhea seen by Cassini - Mosaic of images obtained by the Cassini probe in March 2015. Rhea is the second largest satellite in Saturn (1528 km in diameter). After a couple of years in high - inclination orbits that limited its ability to encounter Saturn's moons, Nasa's Cassini spacecraft returned to Saturn's equatorial plane in March 2015.Image taken using clear, green, infrared and ultraviolet spectral filters were combined to create these enhanced color views, which offer an expanded range of the colors visible to human eyes in order to highlight subtle color differences across Rhea's surface. The moon's surface is fairly uniform in natural color.This view at right is centered at 9 degrees north latitude, 254 degrees west longitude. Resolution in this mosaic is 300 meters (984 feet) per pixel. The image was acquired at a distance that ranged from about 36,000 to 32.100 miles (57,900 to 51,700 kilometers) from Rhea

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Rhea, satellite of Saturn, seen by Cassini - Saturn's moon Rhea seen by Cassini - Mosaic of images obtained by the Cassini probe in March 2015. Rhea is the second largest satellite in Saturn (1528 km in diameter). After a couple of years in high - inclination orbits that limited its ability to encounter Saturn's moons, Nasa's Cassini spacecraft returned to Saturn's equatorial plane in March 2015.Image taken using clear, green, infrared and ultraviolet spectral filters were combined to create these enhanced color views, which offer an expanded range of the colors visible to human eyes in order to highlight subtle color differences across Rhea's surface. The moon's surface is fairly uniform in natural color.This view at right is centered at 9 degrees north latitude, 254 degrees west longitude. Resolution in this mosaic is 300 meters (984 feet) per pixel. The image was acquired at a distance that ranged from about 36,000 to 32.100 miles (57,900 to 51,700 kilometers) from Rhea

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Tethys, Saturn satellite, seen by the Cassini probe - Saturn's moon Tethys seen by Cassini spacecraft: The Tethys satellite photographed by the Cassini probe on 11 April 2015 has a distance of 53,000 km from the satellite. Tethys is about 1070 km in diameter. - This enhancement-color mosaic of Saturn's icy moon Tethys shows a range of features on the moon's trailing hemisphere. Tethys is tidally locked to Saturn, so the trailing hemisphere is the side of the moon that always faces opposite its direction of motion as it orbits the planet - Images taken using clear, green, infrared and ultraviolet spectral filters were combined to create the view, which highlights subtle color differences across Tethys' surface at wavelengths not visible to human eyes. The moon's surface is fairly uniform in natural color - The color of the surface changes conspicuously across the disk, from yellowish hues to nearly white. These broad color changes are affected by a number of external processes. First, S

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Tethys, Saturn satellite, seen by the Cassini probe - Saturn's moon Tethys seen by Cassini spacecraft: The Tethys satellite photographed by the Cassini probe on 11 April 2015 has a distance of 53,000 km from the satellite. Tethys is about 1070 km in diameter. - This enhancement-color mosaic of Saturn's icy moon Tethys shows a range of features on the moon's trailing hemisphere. Tethys is tidally locked to Saturn, so the trailing hemisphere is the side of the moon that always faces opposite its direction of motion as it orbits the planet - Images taken using clear, green, infrared and ultraviolet spectral filters were combined to create the view, which highlights subtle color differences across Tethys' surface at wavelengths not visible to human eyes. The moon's surface is fairly uniform in natural color - The color of the surface changes conspicuously across the disk, from yellowish hues to nearly white. These broad color changes are affected by a number of external processes. First, S

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Jupiter seen from his satellite Ganymede - Illustration - Ridges, grooves, and craters on Ganymede - Artist's view of the surface of Ganymede, Jupiter's largest satellite. An impact crater about 15 km in diameter differs from the striated surface of the satellite. In the sky are represented Jupiter, the Europe satellite on the top right, and Io on the left of Jupiter. Jupiter's largest satellite Ganymede has a varying surface, some of which is characterized by rumpled bundles of ridges and grooves that run for hundreds of miles over a frozen surface of water - ice. They probably formed long ago when tectonic forces pulled apart Ganymede's upper crust; similar sets of faults occur in rift zones on Earth, as in eastern Africa. Subsequent meteoritic impacts have peppered - - and broken in places - - the continuity of the running formations. In this image an impact crater about 10 miles in diameter dominates a scene otherwise defined by a dozen long ridges. In the middle of the crater is a

Walter B Myers

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Jupiter seen from his satellite Ganymede - Illustration - Ridges, grooves, and craters on Ganymede - Artist's view of the surface of Ganymede, Jupiter's largest satellite. An impact crater about 15 km in diameter differs from the striated surface of the satellite. In the sky are represented Jupiter, the Europe satellite on the top right, and Io on the left of Jupiter. Jupiter's largest satellite Ganymede has a varying surface, some of which is characterized by rumpled bundles of ridges and grooves that run for hundreds of miles over a frozen surface of water - ice. They probably formed long ago when tectonic forces pulled apart Ganymede's upper crust; similar sets of faults occur in rift zones on Earth, as in eastern Africa. Subsequent meteoritic impacts have peppered - - and broken in places - - the continuity of the running formations. In this image an impact crater about 10 miles in diameter dominates a scene otherwise defined by a dozen long ridges. In the middle of the crater is a

Walter B Myers

PIX4575196

 
Tethys, Saturn satellite, seen by the Cassini probe - Saturn's moon Tethys seen by Cassini spacecraft - The Tethys satellite photographed by the Cassini probe on August 30, 2007 at a distance of 97,000 km. Tethys is about 1070 km in diameter. At the top left of the picture is the gigantic impact crater Odysseus, which measures 450 km in diameter. The vast expanse of the crater Odysseus spreads out below Cassini in this mosaic view of Saturn's moon Tethys. The crater (450 kilometers or 280 miles across) is a remarkably well - preserved example of an ancient multi - ringed impact basin: the outer ring is defined by steep, cliff - like walls that descend to generally broad internal terraces. The inner ring is formed by a prominent, crown - shaped, 140 - kilometer (88 - mile) diameter circular band of icy mountains. Multi - ring basins are seen on rocky bodies as well as icy ones. The complex internal structure and multi - ringed nature of these very large basins are believed to arise from

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Tethys, Saturn satellite, seen by the Cassini probe - Saturn's moon Tethys seen by Cassini spacecraft - The Tethys satellite photographed by the Cassini probe on August 30, 2007 at a distance of 97,000 km. Tethys is about 1070 km in diameter. At the top left of the picture is the gigantic impact crater Odysseus, which measures 450 km in diameter. The vast expanse of the crater Odysseus spreads out below Cassini in this mosaic view of Saturn's moon Tethys. The crater (450 kilometers or 280 miles across) is a remarkably well - preserved example of an ancient multi - ringed impact basin: the outer ring is defined by steep, cliff - like walls that descend to generally broad internal terraces. The inner ring is formed by a prominent, crown - shaped, 140 - kilometer (88 - mile) diameter circular band of icy mountains. Multi - ring basins are seen on rocky bodies as well as icy ones. The complex internal structure and multi - ringed nature of these very large basins are believed to arise from

PIX4625574

 
Moon: Copernicus crater - Moon: Copernicus crater - Copernic Crateres (in the centre near the limbo) and Reinhold (in the foreground) seen in November 1969 from the control module of Apollo 12. An Apollo 12 high - oblique view of the lunar nearside looking northeast towards the crater Copernicus (in center near horizon), as photographed from lunar orbit. The shaded crater in the foreground is Reinhold. Reinhold B is the crater next to Reinhold which as the small crater in the center of it. November 1969

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Moon: Copernicus crater - Moon: Copernicus crater - Copernic Crateres (in the centre near the limbo) and Reinhold (in the foreground) seen in November 1969 from the control module of Apollo 12. An Apollo 12 high - oblique view of the lunar nearside looking northeast towards the crater Copernicus (in center near horizon), as photographed from lunar orbit. The shaded crater in the foreground is Reinhold. Reinhold B is the crater next to Reinhold which as the small crater in the center of it. November 1969

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Moon: Theophile crater - Moon: Theophilus crater - View of the large impact crater Theophile with the Madler crater and the Nectar Sea on its left. Image obtained in July 1969 from the command module of Apollo 11. An Apollo 11 oblique view of the large crater Theophilus located at the northwest edge of the Sea of Nectar on the lunar nearside. Theophilus is about 60 statute miles in diameter. The smooth area is Mare Nectaris. The smaller crater Madler, about 14 statute miles in diameter, is located to the east of Theophilus. Visible in the background are the large crater Fracastorius and the smaller crater Beaumont. The coordinates of the center of this photograph are 29 degrees east longitude and 11 degrees south latitude

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Moon: Theophile crater - Moon: Theophilus crater - View of the large impact crater Theophile with the Madler crater and the Nectar Sea on its left. Image obtained in July 1969 from the command module of Apollo 11. An Apollo 11 oblique view of the large crater Theophilus located at the northwest edge of the Sea of Nectar on the lunar nearside. Theophilus is about 60 statute miles in diameter. The smooth area is Mare Nectaris. The smaller crater Madler, about 14 statute miles in diameter, is located to the east of Theophilus. Visible in the background are the large crater Fracastorius and the smaller crater Beaumont. The coordinates of the center of this photograph are 29 degrees east longitude and 11 degrees south latitude

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Mars - Atmosphere - View of Mars Planet with Argyre Basin, obtained by the Viking 1 probe in July 1976. Argyre measures 1300 km in diameter and is the second largest impact crater on Mars, after Hellas Planitia. The Argyre impact basin in the southern highlands of Mars. The basin, which is approximately 1,300 kilometers in diameter, was formed about 4 billion years ago during the Heavy Bombardment Period of the early Solar System when an asteroid or comet roughly 50 kilometers across impacted Mars. Argyre is believed to be the second - largest impact basin on Mars after Hellas Planitia and may be one of the best preserved ancient impact basins from the Heavy Bombardment Period

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Mars - Atmosphere - View of Mars Planet with Argyre Basin, obtained by the Viking 1 probe in July 1976. Argyre measures 1300 km in diameter and is the second largest impact crater on Mars, after Hellas Planitia. The Argyre impact basin in the southern highlands of Mars. The basin, which is approximately 1,300 kilometers in diameter, was formed about 4 billion years ago during the Heavy Bombardment Period of the early Solar System when an asteroid or comet roughly 50 kilometers across impacted Mars. Argyre is believed to be the second - largest impact basin on Mars after Hellas Planitia and may be one of the best preserved ancient impact basins from the Heavy Bombardment Period

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Moon: Copernicus crater and Sea of the Islands - Moon: Copernicus crater and Mare Insularum - The Copernic crater, on the top left, is about 90 km in diameter

P. Lazzarotti

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Moon: Copernicus crater and Sea of the Islands - Moon: Copernicus crater and Mare Insularum - The Copernic crater, on the top left, is about 90 km in diameter

P. Lazzarotti

PIX4576479

 
Japet, satellite of Saturn, seen by Cassini - Saturn's moon Iapetus seen by Cassini spacecraft - Comparison of the two hemispheres of Japet, a satellite of Saturn of 1471 kilometres in diameter. Its main feature is the color difference between the two hemispheres. On the left, the dark region called Cassini Regio with to the east the largest crater of Japet, named Turgis (580 km in diameter). On the right, the bright side of the satellite with Roncevaux Terra (north) and Saragossa Terra (south) housing the large impact crater Engelier (504 km in diameter). Both images were obtained by the Cassini probe on 10 September 2007 (right) and 27 December 2004 (left). These two global images of Iapetus show the extreme brightness dichotomy on the surface of this peculiar Saturnian moon. The left - hand panel shows the moon's leading hemisphere and the right - hand panel shows the moon's trailing side. While low and mid latitudes of the leading side exhibit a surface almost as dark as charcoal,

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Japet, satellite of Saturn, seen by Cassini - Saturn's moon Iapetus seen by Cassini spacecraft - Comparison of the two hemispheres of Japet, a satellite of Saturn of 1471 kilometres in diameter. Its main feature is the color difference between the two hemispheres. On the left, the dark region called Cassini Regio with to the east the largest crater of Japet, named Turgis (580 km in diameter). On the right, the bright side of the satellite with Roncevaux Terra (north) and Saragossa Terra (south) housing the large impact crater Engelier (504 km in diameter). Both images were obtained by the Cassini probe on 10 September 2007 (right) and 27 December 2004 (left). These two global images of Iapetus show the extreme brightness dichotomy on the surface of this peculiar Saturnian moon. The left - hand panel shows the moon's leading hemisphere and the right - hand panel shows the moon's trailing side. While low and mid latitudes of the leading side exhibit a surface almost as dark as charcoal,

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Moon: King crater - Moon: King crater - The King impact crater on the hidden face of the Moon. This crater is about 75 km in diameter and 4 km in depth. Image obtained in April 1972 from the control module of Apollo 16. This vertical view shows the King Crater on the lunar surface. It was exposed with color positive film in a hand - held 70 mm camera onboard the Command and Service Modules during the Apollo 16 mission's 98th orbit of the moon. Center point coordinates are located at 5.4 degrees north latitude and 120.8 degrees east longitude. April 1972

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Moon: King crater - Moon: King crater - The King impact crater on the hidden face of the Moon. This crater is about 75 km in diameter and 4 km in depth. Image obtained in April 1972 from the control module of Apollo 16. This vertical view shows the King Crater on the lunar surface. It was exposed with color positive film in a hand - held 70 mm camera onboard the Command and Service Modules during the Apollo 16 mission's 98th orbit of the moon. Center point coordinates are located at 5.4 degrees north latitude and 120.8 degrees east longitude. April 1972

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Tethys, Saturn satellite, seen by the Cassini probe - Saturn's moon Tethys seen by Cassini spacecraft - The southern pole of the Tethys satellite photographed by the Cassini probe on September 24, 2005. Mosaic of nine images. With this full - disk mosaic, Cassini presents the best view yet of the south pole of Saturn's moon Tethys. The giant rift Ithaca Chasma cuts across the disk. Much of the topography seen here, including that of Ithaca Chasma, has a soft, muted appearance. It is clearly very old and has been heavily bombarded by impacts over time. Many of the fresh - appearing craters (ones with crisp relief) exhibit unusually bright crater floors. The origin of the apparent brightness (or “” albedo”) contrast is not known. It is possible that impacts punched through to a brighter layer underneath, or perhaps it is brighter because of different grain sizes or textures of the crater floor material in comparison to material along the crater walls and surrounding surface. The moon's h

PIX4625583

Tethys, Saturn satellite, seen by the Cassini probe - Saturn's moon Tethys seen by Cassini spacecraft - The southern pole of the Tethys satellite photographed by the Cassini probe on September 24, 2005. Mosaic of nine images. With this full - disk mosaic, Cassini presents the best view yet of the south pole of Saturn's moon Tethys. The giant rift Ithaca Chasma cuts across the disk. Much of the topography seen here, including that of Ithaca Chasma, has a soft, muted appearance. It is clearly very old and has been heavily bombarded by impacts over time. Many of the fresh - appearing craters (ones with crisp relief) exhibit unusually bright crater floors. The origin of the apparent brightness (or “” albedo”) contrast is not known. It is possible that impacts punched through to a brighter layer underneath, or perhaps it is brighter because of different grain sizes or textures of the crater floor material in comparison to material along the crater walls and surrounding surface. The moon's h

PIX4625583

 
Mars - Gale Crater Region - Gale Crater area on planet Mars - View of the region of the impact crater Gale in which the Curiosity rover will be installed in 2012. This crater (in the top center of the picture) is 154 km in diameter. Image recomposed from data obtained by the Mars Global Surveyor probe. This computer - generated view depicts part of Mars at the boundary between darkness and daylight, with an area including Gale Crater beginning to catch morning light. Northward is to the left. Gale is the crater with a mound inside it near the center of the image. NASA has selected Gale as the landing site for the Mars Science Laboratory mission. The mission's rover will be placed on the ground in a northern portion of Gale crater in August 2012. Gale crater is 96 miles (154 kilometers) in diameter and holds a layered mountain rising about 3 miles (5 kilometers) above the crater floor. The intended landing site is at 4.5 degrees south latitude, 137.4 degrees east longitude. This view wa

PIX4615396

Mars - Gale Crater Region - Gale Crater area on planet Mars - View of the region of the impact crater Gale in which the Curiosity rover will be installed in 2012. This crater (in the top center of the picture) is 154 km in diameter. Image recomposed from data obtained by the Mars Global Surveyor probe. This computer - generated view depicts part of Mars at the boundary between darkness and daylight, with an area including Gale Crater beginning to catch morning light. Northward is to the left. Gale is the crater with a mound inside it near the center of the image. NASA has selected Gale as the landing site for the Mars Science Laboratory mission. The mission's rover will be placed on the ground in a northern portion of Gale crater in August 2012. Gale crater is 96 miles (154 kilometers) in diameter and holds a layered mountain rising about 3 miles (5 kilometers) above the crater floor. The intended landing site is at 4.5 degrees south latitude, 137.4 degrees east longitude. This view wa

PIX4615396

 
Moon: Copernicus crater - Moon: Copernicus crater - Copernic Crateres (in the centre near the limbo) and Reinhold (in the foreground) seen in November 1969 from the control module of Apollo 12. An Apollo 12 high - oblique view of the lunar nearside looking northeast towards the crater Copernicus (in center near horizon), as photographed from lunar orbit. The shaded crater in the foreground is Reinhold. Reinhold B is the crater next to Reinhold which as the small crater in the center of it. November 1969

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Moon: Copernicus crater - Moon: Copernicus crater - Copernic Crateres (in the centre near the limbo) and Reinhold (in the foreground) seen in November 1969 from the control module of Apollo 12. An Apollo 12 high - oblique view of the lunar nearside looking northeast towards the crater Copernicus (in center near horizon), as photographed from lunar orbit. The shaded crater in the foreground is Reinhold. Reinhold B is the crater next to Reinhold which as the small crater in the center of it. November 1969

PIX4576831

 
Mimas, satellite of Saturn, seen by the Cassini probe on 13/02/2010 - Saturn's moon Mimas seen by Cassini spacecraft - February 13 2010 - The Mimas satellite photographed by the Cassini probe on 13 February 2010 has a distance of 50,000 km from the satellite. Mimas is about 400 km in diameter. At the right centre is the large impact crater Herschel, 130 km wide. In this view captured by Nasa's Cassini spacecraft on its closest - ever flyby of Saturn's moon Mimas, large Herschel Crater dominates Mimas, making the moon look like the Death Star in the movie “” Star Wars.”” Herschel Crater is 130 kilometers, or 80 miles, wide and covers most of the right of this image. Cassini came within about 9,500 kilometers (5,900 miles) of Mimas on Feb. 13, 2010.This mosaic was created from six images taken that day in visible light with Cassini's narrow - angle camera on Feb. 13, 2010. The images were re - projected into an orthographic map projection. This view looks toward the area between the regi

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Mimas, satellite of Saturn, seen by the Cassini probe on 13/02/2010 - Saturn's moon Mimas seen by Cassini spacecraft - February 13 2010 - The Mimas satellite photographed by the Cassini probe on 13 February 2010 has a distance of 50,000 km from the satellite. Mimas is about 400 km in diameter. At the right centre is the large impact crater Herschel, 130 km wide. In this view captured by Nasa's Cassini spacecraft on its closest - ever flyby of Saturn's moon Mimas, large Herschel Crater dominates Mimas, making the moon look like the Death Star in the movie “” Star Wars.”” Herschel Crater is 130 kilometers, or 80 miles, wide and covers most of the right of this image. Cassini came within about 9,500 kilometers (5,900 miles) of Mimas on Feb. 13, 2010.This mosaic was created from six images taken that day in visible light with Cassini's narrow - angle camera on Feb. 13, 2010. The images were re - projected into an orthographic map projection. This view looks toward the area between the regi

PIX4625548

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