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'Terraced wall crater on the lunar limb', 1 May 1969 'This oblique view featuring International Astronomical Union (IAU) Crater 302 on the Moon surface was photographed by the Apollo 10 astronauts in May 1969

'Terraced wall crater on the lunar limb', 1 May 1969 'This oblique view featuring International Astronomical Union (IAU) Crater 302 on the Moon surface was photographed by the Apollo 10 astronauts in May 1969

UIS5096643

Mount Vesuvius' crater, Kingdom of Naples, 1767

Mount Vesuvius' crater, Kingdom of Naples, 1767

UIS5080533

Inside the crater of Monte Nuovo, Kingdom of Naples, c 1770

Inside the crater of Monte Nuovo, Kingdom of Naples, c 1770

UIS5080633

German infantry shelter in a crater during the bitter Stalingrad fighting, 1942 (b/w photo)

German infantry shelter in a crater during the bitter Stalingrad fighting, 1942 (b/w photo)

NAM3062477

Volcano Fogo - Cape Verde - Volcano Fogo - Cape Verde islands - Fogo Island with its highest volcano 2800 meters south of the Cape Verde archipelago. Image obtained from the EO-1 satellite on 10 June 2009. Fogo is one of the Cape Verde Islands located roughly 640 kilometers off the westernmost tip of Africa, Fogo received its name from English colonists around 1500 AD. The Advanced Land Imager on Nasa's EO - 1 satellite captured this detailed image of the volcano on June 10, 2009. The volcano's most distinctive feature, its nine - kilometer wide caldera, Cha Caldera, is shown in this image. The eastern half of the crater wall is gone, erased in a massive collapse deep in its ancient history. In the center of the crater, a steep cone named Pico rises about 100 meters above the crater rim (more than a kilometer from the crater floor). The young peak reaches 2,829 meters (9,281 feet) above sea level, making it the island's highest point. The crater is inhabited. A straight road cuts betwe

Volcano Fogo - Cape Verde - Volcano Fogo - Cape Verde islands - Fogo Island with its highest volcano 2800 meters south of the Cape Verde archipelago. Image obtained from the EO-1 satellite on 10 June 2009. Fogo is one of the Cape Verde Islands located roughly 640 kilometers off the westernmost tip of Africa, Fogo received its name from English colonists around 1500 AD. The Advanced Land Imager on Nasa's EO - 1 satellite captured this detailed image of the volcano on June 10, 2009. The volcano's most distinctive feature, its nine - kilometer wide caldera, Cha Caldera, is shown in this image. The eastern half of the crater wall is gone, erased in a massive collapse deep in its ancient history. In the center of the crater, a steep cone named Pico rises about 100 meters above the crater rim (more than a kilometer from the crater floor). The young peak reaches 2,829 meters (9,281 feet) above sea level, making it the island's highest point. The crater is inhabited. A straight road cuts betwe

PIX4658526

Mount Vesuvius' crater, Kingdom of Naples, 1767

Mount Vesuvius' crater, Kingdom of Naples, 1767

UIS5080520

March: impact crater Maunder - Mars: Maunder crater - Perspective view of an impact crater located between Argyre Planitia and Hellas Planitia. The Maunder crater is 90 km in diameter and 900 m deep. The dark areas at the bottom of the crater are dunes. Image obtained by the Mars Express probe in 2005. On 29 November and 14 December 2005 the High - Resolution Stereo Camera (HRSC), onboard the ESA spacecraft Mars Express obtained image data with a ground resolution of approximately 15 meters per pixel. The data were acquired in the region of Noachis Terra at approximately 50* southern latitude and 2* eastern longitude. The Maunder Crater, located halfway between Argyre Planitia and Hellas Planitia on the southern Highlands of Mars, has a diameter of 90 kilometers and a current depth of barely 900 meters. In the east, the crater floor is bounded by an approximately 700 meters deep trough. It may be associated with the landslide on the western edge of the crater. Some gullies formed on th

March: impact crater Maunder - Mars: Maunder crater - Perspective view of an impact crater located between Argyre Planitia and Hellas Planitia. The Maunder crater is 90 km in diameter and 900 m deep. The dark areas at the bottom of the crater are dunes. Image obtained by the Mars Express probe in 2005. On 29 November and 14 December 2005 the High - Resolution Stereo Camera (HRSC), onboard the ESA spacecraft Mars Express obtained image data with a ground resolution of approximately 15 meters per pixel. The data were acquired in the region of Noachis Terra at approximately 50* southern latitude and 2* eastern longitude. The Maunder Crater, located halfway between Argyre Planitia and Hellas Planitia on the southern Highlands of Mars, has a diameter of 90 kilometers and a current depth of barely 900 meters. In the east, the crater floor is bounded by an approximately 700 meters deep trough. It may be associated with the landslide on the western edge of the crater. Some gullies formed on th

PIX4615975

This Dawn framing camera (FC) image of Asteroid Vesta shows Licinia crater, which is the large crater in the center of the image. Licinia has a fresh, sharp rim that is scalloped in shape. Around the side of Licinia crater there are many streaks of dark and bright material cascading towards the crater's center. This image is located in Vesta's Floronia quadrangle, in Vesta's northern hemisphere. NASA's Dawn spacecraft obtained this image with its framing camera on Oct. 11, 2011.

This Dawn framing camera (FC) image of Asteroid Vesta shows Licinia crater, which is the large crater in the center of the image. Licinia has a fresh, sharp rim that is scalloped in shape. Around the side of Licinia crater there are many streaks of dark and bright material cascading towards the crater's center. This image is located in Vesta's Floronia quadrangle, in Vesta's northern hemisphere. NASA's Dawn spacecraft obtained this image with its framing camera on Oct. 11, 2011.

UIG866601

Mount Vesuvius' crater, Kingdom of Naples, 1767

Mount Vesuvius' crater, Kingdom of Naples, 1767

UIS5080495

Battle of the Crater, American Civil War

Battle of the Crater, American Civil War

XLF3782686

Apollo 11: le module de commande - The Apollo 11 Command/Service modules seen from LM - Le module de commande d'Apollo 11 vu du LEM. 20/07/1969. The Apollo 11 Command/Service modules are photographed from the Lunar Module in lunar orbit during the Apollo 11 lunar landing mission. The lunar surface below is in north central Sea of Fertility. The coordinates of the center of the picture are 51 degrees east longitude and 1 degree north latitude. About half of the crater Taruntius G is visible in the lower left corner of the picture. Part of Taruntius H can be seen at lower right. 1969/07/2

Apollo 11: le module de commande - The Apollo 11 Command/Service modules seen from LM - Le module de commande d'Apollo 11 vu du LEM. 20/07/1969. The Apollo 11 Command/Service modules are photographed from the Lunar Module in lunar orbit during the Apollo 11 lunar landing mission. The lunar surface below is in north central Sea of Fertility. The coordinates of the center of the picture are 51 degrees east longitude and 1 degree north latitude. About half of the crater Taruntius G is visible in the lower left corner of the picture. Part of Taruntius H can be seen at lower right. 1969/07/2

PIX4595827

Explosion of the Chagan nuclear test conducted at the Semipalatinsk Test Site on January 15, 1965

Explosion of the Chagan nuclear test conducted at the Semipalatinsk Test Site on January 15, 1965

TME3619015

Occator Crater on Ceres - Occator Crater on Ceres: View of Occator crater in the northern hemisphere of the dwarf planet Ceres. Occator is 92 km wide and 4 km deep. Bright spots are visible, probably salt deposits. Mosaic of images taken by the Dawn probe. Occator Crater, home of Ceres' intriguing brightest areas, is 57 miles (92 kilometers) wide and 2.5 miles (4 kilometers) deep. Occator displays evidence of recent geologic activity. The latest research suggests that the bright material in this crater is comprised of salts left behind after a briny liquid emerged from below, froze and then sublimated, meaning it turned from ice into vapor. Mosaic of images taken by Dawn spacecraft

Occator Crater on Ceres - Occator Crater on Ceres: View of Occator crater in the northern hemisphere of the dwarf planet Ceres. Occator is 92 km wide and 4 km deep. Bright spots are visible, probably salt deposits. Mosaic of images taken by the Dawn probe. Occator Crater, home of Ceres' intriguing brightest areas, is 57 miles (92 kilometers) wide and 2.5 miles (4 kilometers) deep. Occator displays evidence of recent geologic activity. The latest research suggests that the bright material in this crater is comprised of salts left behind after a briny liquid emerged from below, froze and then sublimated, meaning it turned from ice into vapor. Mosaic of images taken by Dawn spacecraft

PIX4569144

Mercury by Messenger. 14/01/2008 - Mercury by Messenger - Jan 14 2008 - Image of the surface of Mercury obtained at a distance of 11,588 km by the Messenger probe on January 14, 2008. The large impact crater at the bottom left of the image is about 230 km in diameter. This image of Mercury's surface was acquired during Messenger's first flyby of the planet on January 14, 2008 when the spacecraft was 11,588 km (7,200 miles) from Mercury's surface. This scene shows at least five different events in Mercury's surface history. The large crater to the lower left of the image measures ~ 230 km (143 miles) in diameter and has a prominent crater, about 85 km (53 miles) across, nestled inside it, south of its center. Both of these craters were subsequently filled with a material that appears to have been emplaced in a relatively fluid form, as evidenced by the fact that the material “” embays”” or onlaps the ejecta blanket surrounding the rim of the smaller crater. The larger crater is filled a

Mercury by Messenger. 14/01/2008 - Mercury by Messenger - Jan 14 2008 - Image of the surface of Mercury obtained at a distance of 11,588 km by the Messenger probe on January 14, 2008. The large impact crater at the bottom left of the image is about 230 km in diameter. This image of Mercury's surface was acquired during Messenger's first flyby of the planet on January 14, 2008 when the spacecraft was 11,588 km (7,200 miles) from Mercury's surface. This scene shows at least five different events in Mercury's surface history. The large crater to the lower left of the image measures ~ 230 km (143 miles) in diameter and has a prominent crater, about 85 km (53 miles) across, nestled inside it, south of its center. Both of these craters were subsequently filled with a material that appears to have been emplaced in a relatively fluid form, as evidenced by the fact that the material “” embays”” or onlaps the ejecta blanket surrounding the rim of the smaller crater. The larger crater is filled a

PIX4617260

Moon: grooves and mountain, April 1972 (photo)

Moon: grooves and mountain, April 1972 (photo)

PIX4576961

Tenoumer impact crater, Mauritania - Tenoumer impact crater, Mauritania - The Tenoumer impact crater in Mauritania is said to have been formed 10,000 to 30,000 years ago and has a diameter of 1.9 km. Image made from the International Space Station on 1 March 2007. Tenoumer impact crater, Mauritania, as seen by the International Space Station on march 1st 2007. Nearly a perfect circle, it is 1.9 kilometers (1.2 miles) wide, and sports a rim 100 meters (330 feet) high. The crater sits in a vast plain of rocks so ancient they were deposited hundreds of millions of years before the first dinosaurs walked the Earth. Modern geologists long debated what caused this crater, some of them favoring a volcano. But closer examination of the structure revealed that the crater's hardened lava”” was actually rock that had melted from a meteorite impact. Although it resides in ancient rock, Tenoumer is geologically young, ranging in age between roughly 10,000 and 30,000 years old.

Tenoumer impact crater, Mauritania - Tenoumer impact crater, Mauritania - The Tenoumer impact crater in Mauritania is said to have been formed 10,000 to 30,000 years ago and has a diameter of 1.9 km. Image made from the International Space Station on 1 March 2007. Tenoumer impact crater, Mauritania, as seen by the International Space Station on march 1st 2007. Nearly a perfect circle, it is 1.9 kilometers (1.2 miles) wide, and sports a rim 100 meters (330 feet) high. The crater sits in a vast plain of rocks so ancient they were deposited hundreds of millions of years before the first dinosaurs walked the Earth. Modern geologists long debated what caused this crater, some of them favoring a volcano. But closer examination of the structure revealed that the crater's hardened lava”” was actually rock that had melted from a meteorite impact. Although it resides in ancient rock, Tenoumer is geologically young, ranging in age between roughly 10,000 and 30,000 years old.

PIX4630656

Martian panorama taken by the rover Opportunity - Martian panorama seen from rover Opportunity - 360 degres panorama obtained by the rover Opportunity from the position where the rover remained for five weeks in November and December 2008. The 276 images that make up this panorama were taken from November 21 to 24, 2008. In this image the rover, whose top of its antenna can be seen in the center of the image, is located about 1 km southwest of the Victoria crater. Opportunity returned to Endeavour crater on December 23, 2008. The Rover Opportunity landed on Mars in the Meridiani Planum region on January 25, 2004. This 360 - degree panorama shows the vista from the location where Nasa's Mars Exploration Rover Opportunity spent five weeks in November and December 2008 while the sun was almost directly in between Mars and Earth, limiting communications. Opportunity is approaching the fifth Earth - year anniversary of its landing on Mars, continuing a surface mission that was initially sch

Martian panorama taken by the rover Opportunity - Martian panorama seen from rover Opportunity - 360 degres panorama obtained by the rover Opportunity from the position where the rover remained for five weeks in November and December 2008. The 276 images that make up this panorama were taken from November 21 to 24, 2008. In this image the rover, whose top of its antenna can be seen in the center of the image, is located about 1 km southwest of the Victoria crater. Opportunity returned to Endeavour crater on December 23, 2008. The Rover Opportunity landed on Mars in the Meridiani Planum region on January 25, 2004. This 360 - degree panorama shows the vista from the location where Nasa's Mars Exploration Rover Opportunity spent five weeks in November and December 2008 while the sun was almost directly in between Mars and Earth, limiting communications. Opportunity is approaching the fifth Earth - year anniversary of its landing on Mars, continuing a surface mission that was initially sch

PIX4615883

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 16,000 km from the satellite. Mimas is about 400 km in diameter. In the centre left, the large impact crater Herschel, 130 km wide. Relatively dark regions below bright crater walls and streaks on some of the walls are seen in this mosaic of Saturn's moon Mimas, created from images taken by Nasa's Cassini spacecraft during its closest flyby of the moon. The crater floors and surroundings are about 20 percent darker than the steep crater walls in this view. Mimas 'original surface, like the surfaces of most of the other major Saturnian moons without atmospheres, is not pure ice but contains some dark impurities. The relatively dark markings appear along the lower portion of the walls of Herschel Crater (130 kilometers, 80 miles wide) and some of the smaller cra

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 16,000 km from the satellite. Mimas is about 400 km in diameter. In the centre left, the large impact crater Herschel, 130 km wide. Relatively dark regions below bright crater walls and streaks on some of the walls are seen in this mosaic of Saturn's moon Mimas, created from images taken by Nasa's Cassini spacecraft during its closest flyby of the moon. The crater floors and surroundings are about 20 percent darker than the steep crater walls in this view. Mimas 'original surface, like the surfaces of most of the other major Saturnian moons without atmospheres, is not pure ice but contains some dark impurities. The relatively dark markings appear along the lower portion of the walls of Herschel Crater (130 kilometers, 80 miles wide) and some of the smaller cra

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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

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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This Dawn framing camera (FC) image of the Asteroid Vesta, shows the Arruntia crater, which is the large crater offset to the top right of the center of the image. Slightly over half of Arruntia crater is covered in a large shadow. But, the non-shadowed part of Arruntia shows impressive details. There is bright material cropping out slightly below the left rim and just below the top and bottom rims there are distinct ridges of material, which are probably formed by material from the rim cascading down towards the center of Arruntia. This image is located in Vesta's Bellicia quadrangle, in Vesta's northern hemisphere. NASA's Dawn spacecraft obtained this image with its framing camera on Oct. 24, 2011.

This Dawn framing camera (FC) image of the Asteroid Vesta, shows the Arruntia crater, which is the large crater offset to the top right of the center of the image. Slightly over half of Arruntia crater is covered in a large shadow. But, the non-shadowed part of Arruntia shows impressive details. There is bright material cropping out slightly below the left rim and just below the top and bottom rims there are distinct ridges of material, which are probably formed by material from the rim cascading down towards the center of Arruntia. This image is located in Vesta's Bellicia quadrangle, in Vesta's northern hemisphere. NASA's Dawn spacecraft obtained this image with its framing camera on Oct. 24, 2011.

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The Tide of Victory', First World War, August 1917

The Tide of Victory', First World War, August 1917

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Martian dunes in winter - March: Winter view of Dunes - Detail on dunes in a crater located in the southern hemisphere of Mars. Clearly, areas covered with gel appear on this image obtained by the HIRISE camera of the Mars Reconnaissance probe orbiter on November 25, 2006. HIRISE is a 50 cm telescope that observes visible and near infrared. Dunes within a crater on Mars are visible in this HiRise image. This crater is located in the southern hemisphere where it was winter at the time this image was taken on November 25, 2006. This observation documents new seasonal processes occurring on dunes at this latitude, as well as other interesting phenomena. The bright tones are interpreted as carbon dioxide or water frost. This is generally concentrated on the east - facing slopes of the dunes, which are in shadow and therefore cooler. Some dark spots on the dunes may be areas that have defrosted more than surrounding terrain. Landslides and dark - toned streaks are seen on many of the west -

Martian dunes in winter - March: Winter view of Dunes - Detail on dunes in a crater located in the southern hemisphere of Mars. Clearly, areas covered with gel appear on this image obtained by the HIRISE camera of the Mars Reconnaissance probe orbiter on November 25, 2006. HIRISE is a 50 cm telescope that observes visible and near infrared. Dunes within a crater on Mars are visible in this HiRise image. This crater is located in the southern hemisphere where it was winter at the time this image was taken on November 25, 2006. This observation documents new seasonal processes occurring on dunes at this latitude, as well as other interesting phenomena. The bright tones are interpreted as carbon dioxide or water frost. This is generally concentrated on the east - facing slopes of the dunes, which are in shadow and therefore cooler. Some dark spots on the dunes may be areas that have defrosted more than surrounding terrain. Landslides and dark - toned streaks are seen on many of the west -

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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

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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Asteroide Vesta seen by the Hubble Space Telescope - Asteroid Vesta - Photo obtained in visible view of the Vesta asteroid in May 1996 by the Hubble Space Telescope. The images reveal a huge impact crater 450 km in diameter south of the asteroid; the original image is at the top left, modeled in 3D on the right. Astronomers have used the Hubble Space telescope to discover a giant impact crater on the asteroid Vesta. <BR>Left is a Hubble Space Telescope image of the asteroid Vesta, taken in May 1996 when the asteroid was 110 million miles from Earth. The asymmetry of the asteroid and “” nub”” and the south pole is suggestive that it suffered a large impact event. Center is a color-encoded elevation map of Vesta that clearly shows the giant 285- mile diameter impact basin and “” bull 's-eye”” central peak. Right is a 3-D computer model of the asteroid Vesta synthesized from Hubble topographic data. The crater's 8-mile high central peak can clearly be seen near the pole. At the bottom an

Asteroide Vesta seen by the Hubble Space Telescope - Asteroid Vesta - Photo obtained in visible view of the Vesta asteroid in May 1996 by the Hubble Space Telescope. The images reveal a huge impact crater 450 km in diameter south of the asteroid; the original image is at the top left, modeled in 3D on the right. Astronomers have used the Hubble Space telescope to discover a giant impact crater on the asteroid Vesta. <BR>Left is a Hubble Space Telescope image of the asteroid Vesta, taken in May 1996 when the asteroid was 110 million miles from Earth. The asymmetry of the asteroid and “” nub”” and the south pole is suggestive that it suffered a large impact event. Center is a color-encoded elevation map of Vesta that clearly shows the giant 285- mile diameter impact basin and “” bull 's-eye”” central peak. Right is a 3-D computer model of the asteroid Vesta synthesized from Hubble topographic data. The crater's 8-mile high central peak can clearly be seen near the pole. At the bottom an

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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

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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Martian dunes in Spring - March: Frost - covered dunes in crater - Detail on dunes in a crater located near the north pole of Mars. Clearly, areas covered with carbon dioxide gel appear on this image obtained by the HIRISE camera of the Mars Reconnaissance probe orbiter on January 1, 2010. HIRISE is a 50 cm telescope that observes visible and near infrared Dunes are often found on crater floors. In the winter time at high northern latitudes the terrain is covered by carbon dioxide ice (dry ice). In the spring as this seasonal ice evaporates many unusual features unique to Mars are visible. On the floor of this crater where there are no dunes, the ice forms an uninterrupted layer. On the dunes however, dark streaks form as surface material from below the ice is mobilized and deposited on top of the ice. In some cases this mobile material probably slides down the steep face of the dune, while in other cases it may be literally blown out in a process of gas release similar to removing a c

Martian dunes in Spring - March: Frost - covered dunes in crater - Detail on dunes in a crater located near the north pole of Mars. Clearly, areas covered with carbon dioxide gel appear on this image obtained by the HIRISE camera of the Mars Reconnaissance probe orbiter on January 1, 2010. HIRISE is a 50 cm telescope that observes visible and near infrared Dunes are often found on crater floors. In the winter time at high northern latitudes the terrain is covered by carbon dioxide ice (dry ice). In the spring as this seasonal ice evaporates many unusual features unique to Mars are visible. On the floor of this crater where there are no dunes, the ice forms an uninterrupted layer. On the dunes however, dark streaks form as surface material from below the ice is mobilized and deposited on top of the ice. In some cases this mobile material probably slides down the steep face of the dune, while in other cases it may be literally blown out in a process of gas release similar to removing a c

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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

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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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

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

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Le Piton de la Fournaise, Ile de la Reunion - Piton de la Fournaise, Reunion island - Le Piton de la Fournaise seen by satellite EO - 1 on 16 January 2009. This shield volcano is one of the most active volcanoes in the world. Considered one of the world's most active volcanoes, Piton de la Fournaise occupies the east - southeastern end of Reunion Island in the western Indian Ocean. It is a shield volcano with a low, broad shape that resemble an ancient warrior shield. The volcano sports an 8 - kilometer - (5 - mile -) wide crater that slopes eastward to the coast. Within that crater sits a lava shield, Dolomieu, and most of Piton de la Fournaise's historic eruptions have occurred from the summit or flanks of Dolomieu. The Advanced Land Imager (ALI) on Nasa's Earth Observing - 1 satellite captured this image of Piton de la Fournaise on January 16, 2009. Dolomieu is the circular feature at the center of the large crater. Lava flows from earlier eruptions have left their marks around Dolo

Le Piton de la Fournaise, Ile de la Reunion - Piton de la Fournaise, Reunion island - Le Piton de la Fournaise seen by satellite EO - 1 on 16 January 2009. This shield volcano is one of the most active volcanoes in the world. Considered one of the world's most active volcanoes, Piton de la Fournaise occupies the east - southeastern end of Reunion Island in the western Indian Ocean. It is a shield volcano with a low, broad shape that resemble an ancient warrior shield. The volcano sports an 8 - kilometer - (5 - mile -) wide crater that slopes eastward to the coast. Within that crater sits a lava shield, Dolomieu, and most of Piton de la Fournaise's historic eruptions have occurred from the summit or flanks of Dolomieu. The Advanced Land Imager (ALI) on Nasa's Earth Observing - 1 satellite captured this image of Piton de la Fournaise on January 16, 2009. Dolomieu is the circular feature at the center of the large crater. Lava flows from earlier eruptions have left their marks around Dolo

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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

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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March: Promethei Planum - Mars: Promethei Planum - Promethei Planum is a region located near the southern pole of Mars. This region is seasonally covered with a thick layer of ice up to 3500 metres thick. On this perspective image obtained by the Mars Express probe on September 22, 2005, an impact crater about 100 km wide and 800 metres deep is visible at the bottom of the image. It is partially covered with ice. On top, structures formed by lava flows; at the top of the picture, ice, which is an extension of the southern polar cap. Promethei Planum, an area seasonally covered with layer of ice more than 3500 m thick layer of ice in the martian south polar region, was the subject of the High Resolution Stereo Camera's focus on 22 September 2005 as Mars Express was in orbit above the Red Planet. Promethei Planum lies at approximately 76* south and 105* east. An approximately 100 km - large and 800 m - deep impact crater is visible in the bottom of the image. The crater's interior is par

March: Promethei Planum - Mars: Promethei Planum - Promethei Planum is a region located near the southern pole of Mars. This region is seasonally covered with a thick layer of ice up to 3500 metres thick. On this perspective image obtained by the Mars Express probe on September 22, 2005, an impact crater about 100 km wide and 800 metres deep is visible at the bottom of the image. It is partially covered with ice. On top, structures formed by lava flows; at the top of the picture, ice, which is an extension of the southern polar cap. Promethei Planum, an area seasonally covered with layer of ice more than 3500 m thick layer of ice in the martian south polar region, was the subject of the High Resolution Stereo Camera's focus on 22 September 2005 as Mars Express was in orbit above the Red Planet. Promethei Planum lies at approximately 76* south and 105* east. An approximately 100 km - large and 800 m - deep impact crater is visible in the bottom of the image. The crater's interior is par

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March: Promethei Planum - Mars: Promethei Planum - Promethei Planum is a region located near the southern pole of Mars. This region is seasonally covered with a thick layer of ice up to 3500 metres thick. On this image obtained by the Mars Express probe on September 22, 2005, an impact crater about 100 km wide and 800 metres deep is visible to the right (north). It is partially covered with ice. In the center of the image, structures formed by lava flows; on the left of the image, ice, which is an extension of the southern polar cap. Promethei Planum, an area seasonally covered with layer of ice more than 3500 m thick layer of ice in the martian south polar region, was the subject of the High Resolution Stereo Camera's focus on 22 September 2005 as Mars Express was in orbit above the Red Planet. Promethei Planum lies at approximately 76* south and 105* east. An approximately 100 km - large and 800 m - deep impact crater is visible in the northern part of the image. The crater's interio

March: Promethei Planum - Mars: Promethei Planum - Promethei Planum is a region located near the southern pole of Mars. This region is seasonally covered with a thick layer of ice up to 3500 metres thick. On this image obtained by the Mars Express probe on September 22, 2005, an impact crater about 100 km wide and 800 metres deep is visible to the right (north). It is partially covered with ice. In the center of the image, structures formed by lava flows; on the left of the image, ice, which is an extension of the southern polar cap. Promethei Planum, an area seasonally covered with layer of ice more than 3500 m thick layer of ice in the martian south polar region, was the subject of the High Resolution Stereo Camera's focus on 22 September 2005 as Mars Express was in orbit above the Red Planet. Promethei Planum lies at approximately 76* south and 105* east. An approximately 100 km - large and 800 m - deep impact crater is visible in the northern part of the image. The crater's interio

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Mars: Sedimentary layers in Becquerel crater - Mars: Periodic Layering in Becquerel Crater - Detail on sedimentary layers in Becquerel crater (Arabia Terra region), obtained on June 10, 2007 by the HIRISE camera on board the Mars Reconnaissance orbiter probe. This image in false colors shows sedimentary rocks in pink, sand in blue. The study of these sedimentary depot strata suggests that the climate of Mars is linked to the inclination of the axis of rotation of the planet. Rhythmic bedding in sedimentary bedrock within Becquerel crater on Mars is suggested by the patterns in this image from the High Resolution Imaging Science Experiment (HiRise) camera on Nasa's Mars Reconnaissance Orbiter. Three dimensional analysis based on stereo pairs of images confirmed the regularity of repetition in the thickness of the beds. In the top half of this image, some of the rhythm is apparent as a series of bundles of about 10 individual layers per bundle. By corresponding to a known 10 - to - one p

Mars: Sedimentary layers in Becquerel crater - Mars: Periodic Layering in Becquerel Crater - Detail on sedimentary layers in Becquerel crater (Arabia Terra region), obtained on June 10, 2007 by the HIRISE camera on board the Mars Reconnaissance orbiter probe. This image in false colors shows sedimentary rocks in pink, sand in blue. The study of these sedimentary depot strata suggests that the climate of Mars is linked to the inclination of the axis of rotation of the planet. Rhythmic bedding in sedimentary bedrock within Becquerel crater on Mars is suggested by the patterns in this image from the High Resolution Imaging Science Experiment (HiRise) camera on Nasa's Mars Reconnaissance Orbiter. Three dimensional analysis based on stereo pairs of images confirmed the regularity of repetition in the thickness of the beds. In the top half of this image, some of the rhythm is apparent as a series of bundles of about 10 individual layers per bundle. By corresponding to a known 10 - to - one p

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Mars: crater in Myers Valles - Mars: crater in Myers Valles - Mamers Valles is a valley about 1000 km long located in the region of Deuteronilus Mensae, north of Arabia Terra. The image obtained by the Mars Express probe on 5 August 2006 shows a crater at the end of this valley. This circular formation measures about thirty kilometres in diameter and is 1400 metres deep. There are traces of flow of material probably composed of water ice, similar to the relief left by the passage of glaciers on Earth. The darker area could be caused by local erosion or wind-driven material. The High - Resolution Stereo Camera (HRSC) onboard the ESA spacecraft Mars Express obtained images focusing on a depression that displays a crater at the end of the long, winding valley, Mamers Valles. The data was obtained on 5 August 2006 with a ground resolution of approximately 14 m/per pixel. The image is centred at approximately 39* north and 17* east on the planet. The valley of Mamers Valles is approximately

Mars: crater in Myers Valles - Mars: crater in Myers Valles - Mamers Valles is a valley about 1000 km long located in the region of Deuteronilus Mensae, north of Arabia Terra. The image obtained by the Mars Express probe on 5 August 2006 shows a crater at the end of this valley. This circular formation measures about thirty kilometres in diameter and is 1400 metres deep. There are traces of flow of material probably composed of water ice, similar to the relief left by the passage of glaciers on Earth. The darker area could be caused by local erosion or wind-driven material. The High - Resolution Stereo Camera (HRSC) onboard the ESA spacecraft Mars Express obtained images focusing on a depression that displays a crater at the end of the long, winding valley, Mamers Valles. The data was obtained on 5 August 2006 with a ground resolution of approximately 14 m/per pixel. The image is centred at approximately 39* north and 17* east on the planet. The valley of Mamers Valles is approximately

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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

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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Traces of the impact crater Chicxulub - Chicxulub impact crater - Excessive relief view of the Yucatan peninsula obtained from radar altimetric data acquired by the SRTM instrument aboard the space shuttle Endeavour in 2000. An arc of circle is visible to the north-west of the peninsula, marking the outer edge of the Chicxulub impact crater whose centre is located off the Mexican coast. This meteorite impact would have caused the disappearance of dinosaurs 65 million years ago. This shaded relief image of Mexico's Yucatan Peninsula show a subtle, but unmistakable, indication of the Chicxulub impact crater. Most scientists now agree that this impact was the cause of the Cretatious - Tertiary Extinction, the event 65 million years ago that marked the sudden extinction of the dinosaurs as well as the majority of life then on Earth. Most of the peninsula is visible here, along with the island of Cozumel off the east coast. The Yucatan is a plateau composed mostly of limestone and is an are

Traces of the impact crater Chicxulub - Chicxulub impact crater - Excessive relief view of the Yucatan peninsula obtained from radar altimetric data acquired by the SRTM instrument aboard the space shuttle Endeavour in 2000. An arc of circle is visible to the north-west of the peninsula, marking the outer edge of the Chicxulub impact crater whose centre is located off the Mexican coast. This meteorite impact would have caused the disappearance of dinosaurs 65 million years ago. This shaded relief image of Mexico's Yucatan Peninsula show a subtle, but unmistakable, indication of the Chicxulub impact crater. Most scientists now agree that this impact was the cause of the Cretatious - Tertiary Extinction, the event 65 million years ago that marked the sudden extinction of the dinosaurs as well as the majority of life then on Earth. Most of the peninsula is visible here, along with the island of Cozumel off the east coast. The Yucatan is a plateau composed mostly of limestone and is an are

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Mars: crater in Myers Valles - Mars: crater in Myers Valles - Mamers Valles is a valley about 1000 km long located in the region of Deuteronilus Mensae, north of Arabia Terra. The image obtained by the Mars Express probe on 5 August 2006 shows a crater at the end of this valley. This circular formation measures about thirty kilometres in diameter and is 1400 metres deep. There are traces of flow of material probably composed of water ice, similar to the relief left by the passage of glaciers on Earth. The High - Resolution Stereo Camera (HRSC) onboard the ESA spacecraft Mars Express obtained images focusing on a depression that displays a crater at the end of the long, winding valley, Mamers Valles. The data was obtained on 5 August 2006 with a ground resolution of approximately 14 m/per pixel. The image is centred at approximately 39* north and 17* east on the planet. The valley of Mamers Valles is approximately 1000 km long, running along the boundary between the northern lowlands an

Mars: crater in Myers Valles - Mars: crater in Myers Valles - Mamers Valles is a valley about 1000 km long located in the region of Deuteronilus Mensae, north of Arabia Terra. The image obtained by the Mars Express probe on 5 August 2006 shows a crater at the end of this valley. This circular formation measures about thirty kilometres in diameter and is 1400 metres deep. There are traces of flow of material probably composed of water ice, similar to the relief left by the passage of glaciers on Earth. The High - Resolution Stereo Camera (HRSC) onboard the ESA spacecraft Mars Express obtained images focusing on a depression that displays a crater at the end of the long, winding valley, Mamers Valles. The data was obtained on 5 August 2006 with a ground resolution of approximately 14 m/per pixel. The image is centred at approximately 39* north and 17* east on the planet. The valley of Mamers Valles is approximately 1000 km long, running along the boundary between the northern lowlands an

PIX4616082

Mars: crater in Myers Valles - Mars: crater in Myers Valles - Mamers Valles is a valley about 1000 km long located in the region of Deuteronilus Mensae, north of Arabia Terra. The image obtained by the Mars Express probe on 5 August 2006 shows a crater at the end of this valley. This circular formation measures about thirty kilometres in diameter and is 1400 metres deep. There are traces of flow of material probably composed of water ice, similar to the relief left by the passage of glaciers on Earth. The darker area could be caused by local erosion or wind-driven material. The High - Resolution Stereo Camera (HRSC) onboard the ESA spacecraft Mars Express obtained images focusing on a depression that displays a crater at the end of the long, winding valley, Mamers Valles. The data was obtained on 5 August 2006 with a ground resolution of approximately 14 m/per pixel. The image is centred at approximately 39* north and 17* east on the planet. The valley of Mamers Valles is approximately

Mars: crater in Myers Valles - Mars: crater in Myers Valles - Mamers Valles is a valley about 1000 km long located in the region of Deuteronilus Mensae, north of Arabia Terra. The image obtained by the Mars Express probe on 5 August 2006 shows a crater at the end of this valley. This circular formation measures about thirty kilometres in diameter and is 1400 metres deep. There are traces of flow of material probably composed of water ice, similar to the relief left by the passage of glaciers on Earth. The darker area could be caused by local erosion or wind-driven material. The High - Resolution Stereo Camera (HRSC) onboard the ESA spacecraft Mars Express obtained images focusing on a depression that displays a crater at the end of the long, winding valley, Mamers Valles. The data was obtained on 5 August 2006 with a ground resolution of approximately 14 m/per pixel. The image is centred at approximately 39* north and 17* east on the planet. The valley of Mamers Valles is approximately

PIX4616083

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 30,000 km from the satellite. Mimas is about 400 km in diameter. In the centre, the large impact crater Herschel, 130 km wide. This mosaic, created from images taken by Nasa's Cassini spacecraft during its closest flyby of Saturn's moon Mimas, looks straight at the moon's huge Herschel Crater and reveals new insights about the moon's surface. Bright - walled craters, with floors and surroundings about 20 percent darker than the steep crater walls, are notable in this view. Mimas 'original surface, like the surfaces of most of the other major Saturnian moons without atmospheres, is not pure ice but contains some dark impurities. Herschel Crater (130 kilometers, 80 miles wide) and some of the smaller craters seen in this mosaic show relatively dark markings alon

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 30,000 km from the satellite. Mimas is about 400 km in diameter. In the centre, the large impact crater Herschel, 130 km wide. This mosaic, created from images taken by Nasa's Cassini spacecraft during its closest flyby of Saturn's moon Mimas, looks straight at the moon's huge Herschel Crater and reveals new insights about the moon's surface. Bright - walled craters, with floors and surroundings about 20 percent darker than the steep crater walls, are notable in this view. Mimas 'original surface, like the surfaces of most of the other major Saturnian moons without atmospheres, is not pure ice but contains some dark impurities. Herschel Crater (130 kilometers, 80 miles wide) and some of the smaller craters seen in this mosaic show relatively dark markings alon

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