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The disappearance of the 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. A sauropod grazes peacefully in the last seconds before the impact that ended the age of dinosaurs

The disappearance of the 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. A sauropod grazes peacefully in the last seconds before the impact that ended the age of dinosaurs

Dixon, Don (b.1951)

PIX4583689

Meteor Crater near Winslow, Arizona, 1988 (photo)

Meteor Crater near Winslow, Arizona, 1988 (photo)

Luisa Ricciarini

LRI4598306

Impact of an asteroid on Earth - Asteroid impact on Earth- Artwork - Artist view of the impact of the asteroid that would have fallen on the peninsula of Yucatan about 65 million years ago. This asteroid 10 km in diameter would be responsible for the disappearance of dinosaurs. An asteroid 5-10 miles across impacts in the Yucatan to end the age of dinosaurs 65 million years ago

Impact of an asteroid on Earth - Asteroid impact on Earth- Artwork - Artist view of the impact of the asteroid that would have fallen on the peninsula of Yucatan about 65 million years ago. This asteroid 10 km in diameter would be responsible for the disappearance of dinosaurs. An asteroid 5-10 miles across impacts in the Yucatan to end the age of dinosaurs 65 million years ago

L. Bret

PIX4583751

Vredefort Meteor Impact Crater, South Africa, True Colour Satellite Image

Vredefort Meteor Impact Crater, South Africa, True Colour Satellite Image

UIG520484

Asteroide Vesta and other asteroides - Asteroid Vesta compared to other asteroids - Comparison of the sizes of the nine asteroides visits to date by space probes. The asteroid Vesta, with a diameter of 530 km, is the largest. This composite image shows the comparative sizes of nine asteroids. Up until now, Lutetia, with a diameter of 81 miles (130 kilometers), was the largest asteroid visited by a spacecraft, which occurred during a flyby. Vesta, which is also considered a protoplanet because it's a large body that almost became a planet, dwarfs all other small bodies in this image, with its diameter sizing up at approximately 330 miles (530 kilometers)

Asteroide Vesta and other asteroides - Asteroid Vesta compared to other asteroids - Comparison of the sizes of the nine asteroides visits to date by space probes. The asteroid Vesta, with a diameter of 530 km, is the largest. This composite image shows the comparative sizes of nine asteroids. Up until now, Lutetia, with a diameter of 81 miles (130 kilometers), was the largest asteroid visited by a spacecraft, which occurred during a flyby. Vesta, which is also considered a protoplanet because it's a large body that almost became a planet, dwarfs all other small bodies in this image, with its diameter sizing up at approximately 330 miles (530 kilometers)

PIX4583518

Impact of an asteroid on the Yucatan - Yucatan impact - Artist view - Artist view of the impact of the asteroid that would have fallen on the Yucatan peninsula about 65 million years ago. This asteroid 10 km in diameter would be responsible for the disappearance of dinosaurs. An asteroid 5-10 miles across impacts in the Yucatan to end the age of dinosaurs 65 million years ago. A fine layer of clay, rich in the element iridium - more concentrated in meteorites than in terrestrial rocks - marks the geological boundary between the Cretaceous and Tertiary eras. This clay layer is believed to have precipitated out of a plant-blanketing cloud of dust that was ejected into the atmosphere by the impact and subsequent fires. The dust darkened and cooled the earth so much that many species became extinct

Impact of an asteroid on the Yucatan - Yucatan impact - Artist view - Artist view of the impact of the asteroid that would have fallen on the Yucatan peninsula about 65 million years ago. This asteroid 10 km in diameter would be responsible for the disappearance of dinosaurs. An asteroid 5-10 miles across impacts in the Yucatan to end the age of dinosaurs 65 million years ago. A fine layer of clay, rich in the element iridium - more concentrated in meteorites than in terrestrial rocks - marks the geological boundary between the Cretaceous and Tertiary eras. This clay layer is believed to have precipitated out of a plant-blanketing cloud of dust that was ejected into the atmosphere by the impact and subsequent fires. The dust darkened and cooled the earth so much that many species became extinct

Dixon, Don (b.1951)

PIX4583688

Manicouagan Crater, Quebec, Canada, True Colour Satellite Image

Manicouagan Crater, Quebec, Canada, True Colour Satellite Image

UIG601868

Cratere d'impact Vredefort - Afrique du Sud - Vredefort impact crater

Cratere d'impact Vredefort - Afrique du Sud - Vredefort impact crater

PIX5894615

Siljan Meteor Impact Crater, Sweden, True Colour Satellite Image

Siljan Meteor Impact Crater, Sweden, True Colour Satellite Image

UIG602033

Cratere Manicouagan - Quebec - seen by ISS 04/2002 - Cratere d'impact Manicouagan, Quebec, seen by the international space station on 04/14/2002

Cratere Manicouagan - Quebec - seen by ISS 04/2002 - Cratere d'impact Manicouagan, Quebec, seen by the international space station on 04/14/2002

PIX4630705

Mars surface seen by the probe Mariner 6 - Mariner 6 closeup view of Martian craters - Martian crateres in Sinus Meridiani seen by the probe Mariner 6 in July 1969. Recolorized image. Mars craters in Sinus Meridiani seen by Mariner 6 in july 1969. Recolorized picture

Mars surface seen by the probe Mariner 6 - Mariner 6 closeup view of Martian craters - Martian crateres in Sinus Meridiani seen by the probe Mariner 6 in July 1969. Recolorized image. Mars craters in Sinus Meridiani seen by Mariner 6 in july 1969. Recolorized picture

Steven Hobbs

PIX4615020

Towards the southern pole of the Moon - Moon: southwest part: Mosaic showing the southwest part of the visible face of the Moon. Images obtained on August 26, 2016, a day after the last quarter - Mosaic of images showing an area towards the south pole. August 26 2016, the day after the last quarter of the moon

Towards the southern pole of the Moon - Moon: southwest part: Mosaic showing the southwest part of the visible face of the Moon. Images obtained on August 26, 2016, a day after the last quarter - Mosaic of images showing an area towards the south pole. August 26 2016, the day after the last quarter of the moon

Sebastian Voltmer

PIX4614511

Apollo Missions - Artist View - Apollo program - Artist view - LEM separates from the control module to land on the Moon. The Lunar Excursion Module separates from the Command and Service Module in preparation for landing on the Moon

Apollo Missions - Artist View - Apollo program - Artist view - LEM separates from the control module to land on the Moon. The Lunar Excursion Module separates from the Command and Service Module in preparation for landing on the Moon

Steven Hobbs

PIX4596426

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 Fairchild metric camera in the Scientific Instrumentation Module (SIM) bay of the Apollo 15 Command and Service Module (CSM) in lunar orbit. This view is looking south. 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. The three - inch mapping camera was one of eight lunar orbital science experiments mounted in the SIM bay — 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 Fairchild metric camera in the Scientific Instrumentation Module (SIM) bay of the Apollo 15 Command and Service Module (CSM) in lunar orbit. This view is looking south. 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. The three - inch mapping camera was one of eight lunar orbital science experiments

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 Fairchild metric camera in the Scientific Instrumentation Module (SIM) bay of the Apollo 15 Command and Service Module (CSM) in lunar orbit. This view is looking south. 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. The three - inch mapping camera was one of eight lunar orbital science experiments

PIX4576935

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

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

PIX4583458

March: craters in Hellas Basin - Illustration - Mars: craters near Hellas - Illustration - Morning mist invades craters near Hellas Basin. Morning fog fills in the craters of the Martian highlands near Hellas Basin

March: craters in Hellas Basin - Illustration - Mars: craters near Hellas - Illustration - Morning mist invades craters near Hellas Basin. Morning fog fills in the craters of the Martian highlands near Hellas Basin

Steven Hobbs

PIX4617015

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 central peak, formed when the energy of the impact liquefied the crust long enough for it to rebound upward and solidify once again. Immediately above the horizon, Jupiter is still a majestic spectacle, even at a distance of nearly three times that between the Earth and its moon. Much closer on the upper right is Ganymede's sister satellite Europa. At a distance of 307 thousand miles from this vantage point, Europe is only a quarter again as far as the Earth is from its moon. To the lower left of Jupiter at nearly a million miles is Jupiter's volcanic satellite Io — 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

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

Tourist at Meteor Crater - Tourist at Meteor Crater, Arizona, USA. This crater measures 1,200 metres in diameter and 180 metres in depth. It would have formed about 50,000 years ago as a result of the impact of an asteroid 30 to 50 meters in diameter. A female tourist on the rim of Meteor Crater. Meteor Crater, near Flagstaff, Arizona was formed about 50,000 years ago following the impact of a 30 to 50 meter diameter asteroid; its diameter currently stands at 1,2 km and its depth is about 180m

Tourist at Meteor Crater - Tourist at Meteor Crater, Arizona, USA. This crater measures 1,200 metres in diameter and 180 metres in depth. It would have formed about 50,000 years ago as a result of the impact of an asteroid 30 to 50 meters in diameter. A female tourist on the rim of Meteor Crater. Meteor Crater, near Flagstaff, Arizona was formed about 50,000 years ago following the impact of a 30 to 50 meter diameter asteroid; its diameter currently stands at 1,2 km and its depth is about 180m

Alex Conu

PIX4661539

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

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

PIX4583752

Moon: Apennine Mountains - Moon: Apenninus Mountains - The Apennine Mountains are a chain of mountains between the Rainy Sea (left) and the Serenite Sea (right). Some peaks peak at 5000m. Mosaic of images obtained on September 2, 2007, two days before the last quarter of the Moon. Montes Apenninus are a mountain chain located between Mare Imbrium (left) and Mare Serenitatis (right). Some of these mountains are 5000 m high. Composite of images taken on september 2 2007, two days before last quarter of the moon

Moon: Apennine Mountains - Moon: Apenninus Mountains - The Apennine Mountains are a chain of mountains between the Rainy Sea (left) and the Serenite Sea (right). Some peaks peak at 5000m. Mosaic of images obtained on September 2, 2007, two days before the last quarter of the Moon. Montes Apenninus are a mountain chain located between Mare Imbrium (left) and Mare Serenitatis (right). Some of these mountains are 5000 m high. Composite of images taken on september 2 2007, two days before last quarter of the moon

PIX4576697

Impact on the window of the shuttle Discovery - 07/1995 - Windows's impact crater on space shuttle Discovery - 07/1995: Micro impact crater on one of the windows of the space shuttle Discovery. July 1995. Debris impact damage to flight deck window W6 next to the pilot's seat.

Impact on the window of the shuttle Discovery - 07/1995 - Windows's impact crater on space shuttle Discovery - 07/1995: Micro impact crater on one of the windows of the space shuttle Discovery. July 1995. Debris impact damage to flight deck window W6 next to the pilot's seat.

PIX4647178

Meteor Crater - Arizona - USA - Impact Crater Meteor Crater, Arizona, USA

Meteor Crater - Arizona - USA - Impact Crater Meteor Crater, Arizona, USA

PIX4630579

Meteor Crater - Arizona - USA - Impact Crater Meteor Crater, Arizona, USA

Meteor Crater - Arizona - USA - Impact Crater Meteor Crater, Arizona, USA

PIX4630560

Vredefort impact crater, South Africa - Vredefort impact crater, South Africa - The 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 Space Shuttle Discovery on August 29, 1985. 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 space shuttle Discovery on August 29, 1985

Vredefort impact crater, South Africa - Vredefort impact crater, South Africa - The 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 Space Shuttle Discovery on August 29, 1985. 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 space shuttle Discovery on August 29, 1985

PIX4630679

Meteor Crater - Arizona (USA) - seen by shuttle - Meteor Crater - Arizona (USA) - seen by shuttle - Impact Crater Meteor Crater, Arizona (USA), seen by shuttle STS - 40 in June 1991

Meteor Crater - Arizona (USA) - seen by shuttle - Meteor Crater - Arizona (USA) - seen by shuttle - Impact Crater Meteor Crater, Arizona (USA), seen by shuttle STS - 40 in June 1991

PIX4630602

Meteor Crater - Arizona - USA - Anaglyph - Meteor Crater - Arizona - USA - Anaglyph - Impact Crater Meteor Crater, Arizona, USA. This crater measures 1,200 metres in diameter and 180 metres in depth. It would have formed about 50,000 years ago as a result of the impact of an asteroid 30 to 50 meters in diameter. It was formed about 50,000 years ago following the impact of a 30 to 50 meter diameter asteroid; its diameter currently stands at 1,2 km and its depth is about 180m. Anaglyph image, use 3D Eyeglasse

Meteor Crater - Arizona - USA - Anaglyph - Meteor Crater - Arizona - USA - Anaglyph - Impact Crater Meteor Crater, Arizona, USA. This crater measures 1,200 metres in diameter and 180 metres in depth. It would have formed about 50,000 years ago as a result of the impact of an asteroid 30 to 50 meters in diameter. It was formed about 50,000 years ago following the impact of a 30 to 50 meter diameter asteroid; its diameter currently stands at 1,2 km and its depth is about 180m. Anaglyph image, use 3D Eyeglasse

Stefan Seip

PIX4630534

Cratere Manicouagan -Québec- Manicouagan impact crater seen from the space station: Cratere d'impact Manicouagan, Quebec, vu depuis la station spatiale internationale (ISS) on 15/04/2016. This 100 km-diameter crater formed 212 million years ago, following the fall of an asteroid on Earth. - Manicouagan Impact Crater, Quebec, Canada is a 212 million year old impact crater, roughly 100 km in diameter. This is one of the most photographed impact craters from ISS because it is often visible at the top of the orbit. April 15 2016

Cratere Manicouagan -Québec- Manicouagan impact crater seen from the space station: Cratere d'impact Manicouagan, Quebec, vu depuis la station spatiale internationale (ISS) on 15/04/2016. This 100 km-diameter crater formed 212 million years ago, following the fall of an asteroid on Earth. - Manicouagan Impact Crater, Quebec, Canada is a 212 million year old impact crater, roughly 100 km in diameter. This is one of the most photographed impact craters from ISS because it is often visible at the top of the orbit. April 15 2016

PIX4661579

Cratere Manicouagan - Quebec - March 2001 - The Manicouagan Impact Crater reservoir in Quebec, Canada - Cratere d'impact Manicouagan, Quebec, seen from the International Space Station in March 2001. 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 200

Cratere Manicouagan - Quebec - March 2001 - The Manicouagan Impact Crater reservoir in Quebec, Canada - Cratere d'impact Manicouagan, Quebec, seen from the International Space Station in March 2001. 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 200

PIX4630731

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

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

PIX4630749

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 inner island plateau, Rene - Levasseur Island. Because it is so unique and easily recognizable from the sky and space, the crater has been the subject of hundreds of images from astronauts for 45 - plus years. 2 Jan 2014 — 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

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

PIX4630745

Tenoumer Impact Crater, Mauritania (photo)

Tenoumer Impact Crater, Mauritania (photo)

PIX5973683

Impact Crater Oasis - Libya - Oasis Impact Crater - Libya - The Oasis Crater in Libya is said to have been formed 120 million years ago and has a diameter of 18 km. Image obtained from the International Space Station (ISS) on January 13, 2007. Oasis impact crater in Libya, as seen by the International Space Station (ISS) on January 13 2007. It was formed about 120 million years ago and its diameter currently stands at 18 km

Impact Crater Oasis - Libya - Oasis Impact Crater - Libya - The Oasis Crater in Libya is said to have been formed 120 million years ago and has a diameter of 18 km. Image obtained from the International Space Station (ISS) on January 13, 2007. Oasis impact crater in Libya, as seen by the International Space Station (ISS) on January 13 2007. It was formed about 120 million years ago and its diameter currently stands at 18 km

PIX4630651

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 ice, while reddish and brownish areas include non - ice components in higher concentrations. The polar regions, visible at the left and right of this view, are noticeably bluer than the more equatorial latitudes, which look more white. This color variation is thought to be due to differences in ice grain size in the two locations. Images taken through near - infrared, green and violet filters have been combined to produce this view. The images have been corrected for light scattered outside of the image, to provide a color correction that is calibrated by wavelength. Gaps in the images have been filled with simulated color based on the color of nearby surface areas with similar terrain types. This global color view consists of images acquired by the Galileo Solid - State Imaging (SSI) experiment on the spacecraft's first and fourteenth orbits through the Jupiter system, in 1995 and 1998, respectively. Image scale is 2 miles (1.6 kilometers) per pixel. North on Europa is at righ — 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

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

PIX4574821

Four steps in the formation of a complex impact crater, resulting in a central peak and terraces of collapsed material.

Four steps in the formation of a complex impact crater, resulting in a central peak and terraces of collapsed material.

UIG533674

Impact Crater Vredefort, South Africa (photo)

Impact Crater Vredefort, South Africa (photo)

PIX5973684

Mars surface seen by the probe Mariner 7 - Mariner 7 view of martian craters - Martian crateres near the southern pole seen by the probe Mariner 7 in August 1969. Recolorized image. Mars craters near south pole seen by Mariner 7 in august 1969. Recolorized picture

Mars surface seen by the probe Mariner 7 - Mariner 7 view of martian craters - Martian crateres near the southern pole seen by the probe Mariner 7 in August 1969. Recolorized image. Mars craters near south pole seen by Mariner 7 in august 1969. Recolorized picture

Steven Hobbs

PIX4615030

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 measuring 20 km in diameter. Covering an area of approximately 150 sq km, a crater of this size on Earth could harbour cities such as Bonn or Kiel. In contrast to the smaller craters, it shows a blanket of ejecta with flow forms surrounding the rim — 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

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

PIX4616156

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 feature. Covering an area of approximately 150 sq km, this crater could harbour cities such as Bonn or Kiel. In contrast to the smaller craters, it shows a blanket of ejecta with flow forms surrounding the rim. The large craters were formed when loose, soft material was ejected due to impact, and the smaller ones formed due to secondary impacts, when consolidated material was ejected in a ballistic path and impacted the original crater at varying distances. Most martian water exists in the form of subsurface ice. The presence of a blanket of ejecta and outflow channels around the crater suggest that the primary impact may have penetrated the surface enough to melt a buried frozen water reservoir — 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

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

PIX4616151

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

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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Surface of Ceres - Ceres' surface - Surface of the dwarf planet Ceres. Artist's view. What is known about Ceres' surface is that it has an albedo (surface brightness) about the same as the Earth's Moon and never gets warmer than minus 30o F. In this image the artist is suggesting a lunar-like terrain modified by the presence of water ice

Surface of Ceres - Ceres' surface - Surface of the dwarf planet Ceres. Artist's view. What is known about Ceres' surface is that it has an albedo (surface brightness) about the same as the Earth's Moon and never gets warmer than minus 30o F. In this image the artist is suggesting a lunar-like terrain modified by the presence of water ice

Walter B Myers

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Impact Crater Roter Kamm, Namibia - Roter Kamm impact crater, Namibia - The impact crater of Roter Kamm would have been formed 3.7 million years ago and has a diameter of 2.5 km. Image obtained from the International Space Station (ISS) on 5 October 2007. Roter Kamm is a 2,5 km meteorite impact crater with an age estimated to be 3,7 million years. Image taken from the International space station (ISS) on October 5, 2007

Impact Crater Roter Kamm, Namibia - Roter Kamm impact crater, Namibia - The impact crater of Roter Kamm would have been formed 3.7 million years ago and has a diameter of 2.5 km. Image obtained from the International Space Station (ISS) on 5 October 2007. Roter Kamm is a 2,5 km meteorite impact crater with an age estimated to be 3,7 million years. Image taken from the International space station (ISS) on October 5, 2007

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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

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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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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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 flows from the Tharsis volcanic region — 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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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, Saturn's diffuse E-ring preferentially bombards Tethys' leading hemisphere, towards the right side of this image, with ice bright ice grains. At the same time, charged particles from Saturn's radiation belt bombard the surface on the trailing side, causing color changes due to chemical alteration of the materials there. The albedo - a measure of the surface's reflectivity - drops by 10 to 15 percent from the moon's leading side to the trailing side. Similar global color patterns exist on other Saturnian moons - This mosaic is an orthographic projection constructed from 52 Cassini images obtained on April 11, 2015 with the Cassini spacecraft narrow-angle camera. Resolution is about 1,000 feet (300 meters) per pixel. The images were obtained at a distance of approximately 33,000 miles (53,000 kilometers) from Tethys — 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

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

PIX4625625

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

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

PIX4616548

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

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

Steven Hobbs

PIX4616817

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

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

PIX4625591

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

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

PIX4616155

Moon: Tsiolkovsky crater on the hidden face - Moon: crater Tsiolkovsky on lunar farside - Image obtained during the Apollo 15 mission, August 1971. Image taken during Apollo 15 mission

Moon: Tsiolkovsky crater on the hidden face - Moon: crater Tsiolkovsky on lunar farside - Image obtained during the Apollo 15 mission, August 1971. Image taken during Apollo 15 mission

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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 tones in this simulated - true - color image. Deep green indicates vegetation lining the winding stream west of the crater. A road leads to the crater's rim, approaching from the south, then turning east. The crater itself appears fairly dark brown, but a bright white splotch occupies the crater's center. Wolfe Creek Crater measures roughly 880 meters (2,890 feet) in diameter, and the mostly flat crater floor sits some 55 meters (180 feet) below the crater rim and some 25 meters (82 feet) below the sand plain outside of the crater. At the crater's center, the ground rises slightly, and includes gypsum - - probably responsible for the bright white spot in this image - - and some surprisingly large trees. Geologists studying the crater have estimated that it formed some 300,000 years ago when a meteorite weighing more than 50,000 metric tons struck the Earth at an estimated 15 kilometers (9.3 miles) per second — 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

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

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, Saturn's diffuse E-ring preferentially bombards Tethys' leading hemisphere, towards the right side of this image, with ice bright ice grains. At the same time, charged particles from Saturn's radiation belt bombard the surface on the trailing side, causing color changes due to chemical alteration of the materials there. The albedo - a measure of the surface's reflectivity - drops by 10 to 15 percent from the moon's leading side to the trailing side. Similar global color patterns exist on other Saturnian moons - Mountains on the floor of the 280 mile- (450 km-) wide Odysseus impact basin are visible at upper right, around the two o'clock position - This mosaic is an orthographic projection constructed from 52 Cassini images obtained on April 11, 2015 with the Cassini spacecraft narrow-angle camera. Resolution is about 1,000 feet (300 meters) per pixel. The images were obtained at a distance of approximately 33,000 miles (53,000 kilometers) from Tethys — 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

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

PIX4625616

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 basin in the north to Etus Chasma to the south. The impact crater at right is 35 km diameter — 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

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

PIX4616154

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

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

Sebastian Voltmer

PIX4614521

Appearance of life on Mars - Artist's view - Mars thermal crater - Artwork: Four billion years ago, the impacts of meteorites on Mars could create hot springs where life would have developed - A bombardment of the Red Planet 4 billion years ago could have created hot springs that allowed life to flourish

Appearance of life on Mars - Artist's view - Mars thermal crater - Artwork: Four billion years ago, the impacts of meteorites on Mars could create hot springs where life would have developed - A bombardment of the Red Planet 4 billion years ago could have created hot springs that allowed life to flourish

Miller, Ron (b.1947)

PIX4617102

Impact on the Moon - Artist's View - Formation of Aitken Basin on the Moon - An asteroid hits the Moon forming one of the largest impact crateres of the solar system, the Aitken Basin, at the southern pole of the Moon (2500 km diameter, 13 km depth). An asteroid smashes into the moon forming one of the largest impact crater known in the solar system, the South pole Aitken basin (2500 km wide, 13 km of depth)

Impact on the Moon - Artist's View - Formation of Aitken Basin on the Moon - An asteroid hits the Moon forming one of the largest impact crateres of the solar system, the Aitken Basin, at the southern pole of the Moon (2500 km diameter, 13 km depth). An asteroid smashes into the moon forming one of the largest impact crater known in the solar system, the South pole Aitken basin (2500 km wide, 13 km of depth)

Miller, Ron (b.1947)

PIX4579983

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, broad tracts of the trailing side are almost as bright as snow. The dark terrain covers about 40 percent of the surface and is named Cassini Regio. The names of the bright terrain are Roncesvaux Terra (north) and Saragossa Terra (south). On both hemispheres, the dominant landforms are impact craters. The largest known well - preserved basin on Iapetus, called Turgis, has a diameter of about 580 kilometers (360 miles). It lies at 17 degrees north latitude, 28 degrees west longitude at the eastern edge of the dark Cassini Regio and is visible on the right side of the left - hand panel. The prominent basin on the southern trailing side (at the lower left of the right - hand panel) is Engelier. Engelier is located at 41 degrees south latitude, 265 degrees west longitude, and has a diameter of about 504 kilometers (313 miles). Its formation destroyed about half of Gerin, another large basin on Iapetus. Gerin is located at 46 degrees south latitude, 233 degrees — 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,

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,

PIX4625409

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

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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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 seen in false colours by the Cassini probe on 13 February 2010 has a distance of 16,000 km from the satellite. Color differences reveal differences in terrain nature. Mimas is about 400 km in diameter. At the right centre is the large impact crater Herschel, 130 km wide. Subtle color differences on Saturn's moon Mimas are apparent in this false - color view of Herschel Crater captured by Nasa's Cassini spacecraft during its closest - ever flyby of that moon. The image shows terrain - dependent color variations, particularly the contrast between the bluish materials in and around Herschel Crater (130 kilometers, or 80 miles, wide) and the greenish cast on older, more heavily cratered terrain elsewhere. The origin of the color differences is not yet understood, but may be caused by subtle differences in the surface composition between the two terrains. Herschel Crater covers most of the bottom of this image. To create this false - color view, ultraviolet, green and infrared images were combined into a single picture that exaggerates the color differences of terrain on the moon. These data were combined with a high - resolution image taken in visible light to provide the high - resolution information from the clear - filter image and the color information from the ultraviolet, green and infrared filter images. The natural color of Mimas visible to the human eye may be a uniform gray or yellow color, but this mosaic has been contrast - enhanced and shows differences at other wavelengths of light. During its closest - ever flyby on Feb. 13, 2010, Cassini came within about 9,500 kilometers (5,900 miles) of Mimas. This view looks toward the northern part of the hemisphere of Mimas that leads in the moon's orbit around Saturn. Mimas is 396 kilometers (246 miles) across. North on Mimas is up — 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 seen in false colours by the Cassini probe on 13 February 2010 has a distance of 16,000 km from the satellite. Color differences reveal differences in terrain nature. Mimas is about 400 km in diameter. At the right centre is the large impact crater Herschel, 130 km wide. Subtle color differences on Saturn's moon Mimas are apparent in this false - color view of Herschel Crater captured by Nasa's Cassini spacecraft during its closest - ever flyby of that moon. The image shows terrain - dependent color variations, particularly the contrast between the bluish materials in and around Herschel Crater (130 kilometers, or 80 miles, wide) and the greenish cast on older, more heavily cratered terrain elsewhere. The origin of the color differences is not yet understood, but may be caused by subtle differences in the surface composition betwe

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 seen in false colours by the Cassini probe on 13 February 2010 has a distance of 16,000 km from the satellite. Color differences reveal differences in terrain nature. Mimas is about 400 km in diameter. At the right centre is the large impact crater Herschel, 130 km wide. Subtle color differences on Saturn's moon Mimas are apparent in this false - color view of Herschel Crater captured by Nasa's Cassini spacecraft during its closest - ever flyby of that moon. The image shows terrain - dependent color variations, particularly the contrast between the bluish materials in and around Herschel Crater (130 kilometers, or 80 miles, wide) and the greenish cast on older, more heavily cratered terrain elsewhere. The origin of the color differences is not yet understood, but may be caused by subtle differences in the surface composition betwe

PIX4625563

Mars polar cap seen by the Mariner 7 probe - The Martian polar cap as seen by the Mariner 7 spacecraft - Part of the polar cap south of Mars seen by the Mariner 7 probe in August 1969. Recolorized image. The southern martian polar cap as seen by the Mariner 7 spacecraft in august 1969. Recolorized picture

Mars polar cap seen by the Mariner 7 probe - The Martian polar cap as seen by the Mariner 7 spacecraft - Part of the polar cap south of Mars seen by the Mariner 7 probe in August 1969. Recolorized image. The southern martian polar cap as seen by the Mariner 7 spacecraft in august 1969. Recolorized picture

Steven Hobbs

PIX4615022

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 craters and are marked in green in the annotated version of the image. Cassini scientists interpret this darkening as evidence for the gradual concentration of impurities from evaporating icy materials in areas where the dark impurities slide slowly down the crater wall. There, the bright ice is baked away by the sun and the vacuum of space. At Herschel, the edge where the darker regions contact the crater floor is interrupted by an extensive hummocky area. Scientists believe the hummocky texture came from the flow of melted ice that occurred during the impact that created the crater. That melt filled the bottom of the crater around the central peak. Dark streaks are seen making their way down the sides of some craters and often originated from pockets of dark contaminants embedded just below the rim of the crater wall. The pockets themselves likely represent small, pre - existing, dark - floored craters that were buried by the blanket of material thrown out from the newer im — 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

PIX4625578

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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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 the rebound of intense shock waves that penetrated the body at the time of impact. Tethys is 1,071 kilometers (665 miles) across. This mosaic was assembled from four clear filter, narrow - angle camera images. The view is an orthographic projection centered on 3 degrees south latitude, 119 degrees west longitude and has a resolution of 572 meters (0.35 mile) per pixel. An orthographic view is most like the view seen by a distant observer looking through a telescope. North is up. The view was obtained by the Cassini spacecraft on Aug. 30, 2007, from a distance of approximately 97,000 kilometers (60,000 miles) and at a sun - Tethys - spacecraft, or phase, angle of 51 degrees — 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

PIX4625574

Moon: Cratere Eratosthene - Moon: Eratosthenes crater - Cratere Eratosthene seen from the control module of Apollo 12. View of Eratosthenes crater, on the lunar nearside, as photographed from the Apollo 12 spacecraft

Moon: Cratere Eratosthene - Moon: Eratosthenes crater - Cratere Eratosthene seen from the control module of Apollo 12. View of Eratosthenes crater, on the lunar nearside, as photographed from the Apollo 12 spacecraft

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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 region that leads on Mimas 'orbit around Saturn and the region of the moon facing away from Saturn. Mimas is 396 kilometers (246 miles) across. This view is centered on terrain at 11 degrees south latitude, 158 degrees west longitude. North is up. This view was obtained at a distance of approximately 50,000 kilometers (31,000 miles) from Mimas and at a sun - Mimas - spacecraft, or phase, angle of 17 degrees. Image scale is 240 meters (790 feet) per pixel — 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

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

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

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

PIX4576947

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 along the lower portion of their crater walls (marked in green in the annotated version of the image). Cassini scientists interpret this darkening as evidence for the gradual concentration of impurities from evaporating icy materials in areas where the dark impurities slide slowly down the crater wall. There, bright ice is baked away by the sun and the vacuum of space. At Herschel, the edge where the darker regions contact the crater floor is interrupted by an extensive hummocky area. Scientists believe the hummocky texture came from the flow of melted ice that occurred during the impact that created the crater. That melt filled the bottom of the crater around the central peak. Dark streaks are seen making their way down the sides of some craters, often originating from pockets of dark contaminants embedded just below the rim of the crater wall. The pockets themselves likely represent small, pre - existing, dark - floored craters that were buried by the blanket of material that — 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

PIX4625545

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 high southern latitudes, seen here at the bottom, were not imaged by Nasa's Voyager spacecraft during their flybys of Tethys 25 years ago. The mosaic is composed of nine images taken during Cassini's close flyby of Tethys (1,071 kilometers, or 665 miles across) on Sept. 24, 2005, during which the spacecraft passed approximately 1,500 kilometers (930 miles) above the Moon's surface. This view is centered on terrain at approximately 1.2 degrees south latitude and 342 degrees west longitude on Tethys. It has been rotated so that north is up. The clear filter images in this mosaic were taken with the Cassini spacecraft narrow - angle camera at distances ranging from 71,600 kilometers (44,500 miles) to 62,400 kilometers (38,800 miles) from Tethys and at a Sun - Tethys - spacecraft, or phase, angle of 21 degrees. The image scale is 370 meters (1,200 feet) per pixel — 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

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

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

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

PIX4577258

Impact on the Moon - Artist's View - Moon Collision: An asteroid hits the Moon as seen from the Earth in formation. Based on the recent idea that the earth's moon once underwent a massive collision event

Impact on the Moon - Artist's View - Moon Collision: An asteroid hits the Moon as seen from the Earth in formation. Based on the recent idea that the earth's moon once underwent a massive collision event

Miller, Ron (b.1947)

PIX4614871

Mistastin Crater - Canada - Mistastin Impact Crater - Canada - Mistastin Impact Crater seen since the Space Shuttle Challenger in 1985. The Mistastin Crater is a meteoritic crater located in Canada in the Labrador region and contains circular lake Mistastin. Mistastin crater is a meteorite crater in Labrador, Canada which contains the roughly circular Mistastin Lake

Mistastin Crater - Canada - Mistastin Impact Crater - Canada - Mistastin Impact Crater seen since the Space Shuttle Challenger in 1985. The Mistastin Crater is a meteoritic crater located in Canada in the Labrador region and contains circular lake Mistastin. Mistastin crater is a meteorite crater in Labrador, Canada which contains the roughly circular Mistastin Lake

PIX4661605

Moon: Aristarchus crater - Moon: Aristarchus crater - Apollo 15 - The Aristarchus crater, on the left, the Herodote crater, on the right, 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

Moon: Aristarchus crater - Moon: Aristarchus crater - Apollo 15 - The Aristarchus crater, on the left, the Herodote crater, on the right, 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

PIX4576886

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 of the imag — 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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Apollo 8: lunar craters - Moon craters seen from Apollo 8 - View of Goclenius crateres (foreground), Colombo A and Magelhaens from the Apollo 8 module in December 1968. This oblique view of the lunar surface was taken from the Apollo 8 spacecraft looking southward toward Goclenius and other large craters near 45 degrees east longitude and 10 degrees south latitude in the Sea of Fertility. Goclenius, the crater in the foreground with a rille - broken flat floor, is about 70 kilometers (45 statute miles) in diameter. One rille, approximately horizontal in this view, crosses both crater rims and the central peak, and, on adjoining Apollo 8 photographs, can be traced several kilometers across the mare surface beyond the high crater wall. In the background, the two large craters with smooth floors are Colombo A (left) and Magelhaens. Magelhaens A, the crater with the irregular floor, is about 35 kilometers (20 statute miles) in diameter

Apollo 8: lunar craters - Moon craters seen from Apollo 8 - View of Goclenius crateres (foreground), Colombo A and Magelhaens from the Apollo 8 module in December 1968. This oblique view of the lunar surface was taken from the Apollo 8 spacecraft looking southward toward Goclenius and other large craters near 45 degrees east longitude and 10 degrees south latitude in the Sea of Fertility. Goclenius, the crater in the foreground with a rille - broken flat floor, is about 70 kilometers (45 statute miles) in diameter. One rille, approximately horizontal in this view, crosses both crater rims and the central peak, and, on adjoining Apollo 8 photographs, can be traced several kilometers across the mare surface beyond the high crater wall. In the background, the two large craters with smooth floors are Colombo A (left) and Magelhaens. Magelhaens A, the crater with the irregular floor, is about 35 kilometers (20 statute miles) in diameter

PIX4576771

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

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

PIX4576879

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

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

Saturn seen from his satellite Mimas - Illustration - Saturn as seen from Mimas - Illustration - Artist's view of the Herschel crater on the surface of the satellite Mimas. In the background, the planet Saturn. Artist's impression of crater Herschel on Mimas surface with planet Saturn in background

Saturn seen from his satellite Mimas - Illustration - Saturn as seen from Mimas - Illustration - Artist's view of the Herschel crater on the surface of the satellite Mimas. In the background, the planet Saturn. Artist's impression of crater Herschel on Mimas surface with planet Saturn in background

Miller, Ron (b.1947)

PIX4626337

Impact on the Moon - Artist's View - Moon Collision - An asteroid hits the Moon as seen from the Earth in formation. Based on the recent idea that the earth's moon once underwent a massive collision event

Impact on the Moon - Artist's View - Moon Collision - An asteroid hits the Moon as seen from the Earth in formation. Based on the recent idea that the earth's moon once underwent a massive collision event

Miller, Ron (b.1947)

PIX4973567

Moon: cratere Copernic - Moon: Copernicus crater - Cratere Copernic. Image obtained in December 1972 from the control module of Apollo 17. An oblique view of the large crater Copernicus on the lunar nearside, as photographed from the Apollo 17 spacecraft in lunar orbit. This view is looking generally southwest towards the crater on the horizon. The coordinates of the center of Copernicus are approximately 20 degrees west longitude and 9.5 degrees north latitude

Moon: cratere Copernic - Moon: Copernicus crater - Cratere Copernic. Image obtained in December 1972 from the control module of Apollo 17. An oblique view of the large crater Copernicus on the lunar nearside, as photographed from the Apollo 17 spacecraft in lunar orbit. This view is looking generally southwest towards the crater on the horizon. The coordinates of the center of Copernicus are approximately 20 degrees west longitude and 9.5 degrees north latitude

PIX4577012

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

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

PIX4576885

Moon: grooves and mountain, April 1972 (photo)

Moon: grooves and mountain, April 1972 (photo)

PIX4576961

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

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

PIX4577170

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

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

PIX4576872

Cratere Copernic - Copernicus crater - Crateres Copernic and Gay - Lussac (in the foreground). Image obtained in December 1972 from the control module of Apollo 17. View of Copernicus and small Gay - Lussac (foreground) craters, on the lunar nearside, as photographed from the Apollo 17 spacecraft. Dec 1972

Cratere Copernic - Copernicus crater - Crateres Copernic and Gay - Lussac (in the foreground). Image obtained in December 1972 from the control module of Apollo 17. View of Copernicus and small Gay - Lussac (foreground) craters, on the lunar nearside, as photographed from the Apollo 17 spacecraft. Dec 1972

PIX4577000

Dione, satellite of Saturn, seen by Cassini - Dione, moon of Saturn, as seen by Cassini - Mosaic of images obtained by the Cassini probe on 11 October 2005 at a distance of about 25,000 km from the satellite. As it departed its encounter with Saturn's moon Dione, Cassini sailed above an unreal landscape blasted by impacts. The rising Sun throws craters into sharp contrast and reveals steep crater walls. At the far right, a medium - sized crater is bisected by a fracture, revealing a cross section of the impact site. The seven clear - filter images in this mosaic were taken with the Cassini spacecraft narrow - angle camera on Oct. 11, 2005, at distances ranging from 21.650 to 25.580 kilometers (13,450 to 15,890 miles) from Dione and at a Sun - Dione - spacecraft, or phase, angle of 154 degrees. Resolution in the original images ranges from 126 to 154 meters (413 to 505 feet) per pixel. The images have been re - sized to have an image scale of about 100 meters (330 feet) per pixel. North on Dione is 140 degrees to the left — Dione, satellite of Saturn, seen by Cassini - Dione, moon of Saturn, as seen by Cassini - Mosaic of images obtained by the Cassini probe on 11 October 2005 at a distance of about 25,000 km from the satellite. As it departed its encounter with Saturn's moon Dione, Cassini sailed above an unreal landscape blasted by impacts. The rising Sun throws craters into sharp contrast and reveals steep crater walls. At the far right, a medium - sized crater is bisected by a fracture, revealing a cross section of the impact site. The seven clear - filter images in this mosaic were taken with the Cassini spacecraft narrow - angle camera on Oct. 11, 2005, at distances ranging from 21.650 to 25.580 kilometers (13,450 to 15,890 miles) from Dione and at a Sun - Dione - spacecraft, or phase, angle of 154 degrees. Resolution in the original images ranges from 126 to 154 meters (413 to 505 feet) per pixel. The images have been re - sized to have an image scale of about 100 meters (330 feet) per pixel. North

Dione, satellite of Saturn, seen by Cassini - Dione, moon of Saturn, as seen by Cassini - Mosaic of images obtained by the Cassini probe on 11 October 2005 at a distance of about 25,000 km from the satellite. As it departed its encounter with Saturn's moon Dione, Cassini sailed above an unreal landscape blasted by impacts. The rising Sun throws craters into sharp contrast and reveals steep crater walls. At the far right, a medium - sized crater is bisected by a fracture, revealing a cross section of the impact site. The seven clear - filter images in this mosaic were taken with the Cassini spacecraft narrow - angle camera on Oct. 11, 2005, at distances ranging from 21.650 to 25.580 kilometers (13,450 to 15,890 miles) from Dione and at a Sun - Dione - spacecraft, or phase, angle of 154 degrees. Resolution in the original images ranges from 126 to 154 meters (413 to 505 feet) per pixel. The images have been re - sized to have an image scale of about 100 meters (330 feet) per pixel. North

PIX4625507

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

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

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 young crater newly imaged by MESSENGER, providing a view of the planet distinctly unique from that obtained during Messenger's first flyby. This young, extensively rayed crater, along with the prominent rayed crater to the southeast of Kuiper, near the limb of the planet, were both seen in Earth - based radar images of Mercury but not previously imaged by spacecraft. Recolored Image — 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

PIX4617327

Impact on the Moon seen from primitive Earth - Asteroid Impact on the Moon seen from primitive Earth: An asteroid hits the Moon forming one of the largest impact crateres of the solar system, the Aitken Basin, at the southern pole of the Moon (2500 km in diameter, 13 km in depth). The date of this impact is uncertain, probably just over three billion years ago. On Earth, the first algae grow - An asteroid impact, perhaps the largest endured by the moon since the little splat, created the South Pole Aitkens Basin, one of the largest impact structures in the solar system. The date of the impact is uncertain: it might have occurred only a little over 3 billion years ago. If so, from the earth - where primitive algae would have been the only witness - the impact would have been an impressive sight

Impact on the Moon seen from primitive Earth - Asteroid Impact on the Moon seen from primitive Earth: An asteroid hits the Moon forming one of the largest impact crateres of the solar system, the Aitken Basin, at the southern pole of the Moon (2500 km in diameter, 13 km in depth). The date of this impact is uncertain, probably just over three billion years ago. On Earth, the first algae grow - An asteroid impact, perhaps the largest endured by the moon since the little splat, created the South Pole Aitkens Basin, one of the largest impact structures in the solar system. The date of the impact is uncertain: it might have occurred only a little over 3 billion years ago. If so, from the earth - where primitive algae would have been the only witness - the impact would have been an impressive sight

Miller, Ron (b.1947)

PIX4614916

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

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

PIX4576807

Moon: Bullialdus crater - Moon: Bullialdus crater - Apollo 16 - The Moon with the Bullialdus crater (high center). Image obtained from the Apollo 16 control module. An oblique view of the crater Bullialdus (top center), as photographed by the metric camera in the Scientific Instrumentation Module (SIM) bay of the Apollo 16 Command and Service Module (CSM) in lunar orbit

Moon: Bullialdus crater - Moon: Bullialdus crater - Apollo 16 - The Moon with the Bullialdus crater (high center). Image obtained from the Apollo 16 control module. An oblique view of the crater Bullialdus (top center), as photographed by the metric camera in the Scientific Instrumentation Module (SIM) bay of the Apollo 16 Command and Service Module (CSM) in lunar orbit

PIX4576952

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