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'Hirise' images and/or videos results

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Images of 'Hirise' found, 30

 
Martian dunes at the end of winter - March: Late Winter view of Dunes: Detail on dunes in the southern hemisphere of Mars. With the end of winter, the Sun melts the carbon dioxide ice present all winter. Image obtained by the HIRISE camera of the Mars Reconnaissance probe orbiter on March 21, 2016. HIRISE is a 50 cm telescope that observes visible and near infrared. Sand dunes cover much of this terrain, which has large boulders lying on flat areas between the dunes. It is now late winter here in the Southern hemisphere, and these dunes are just getting enough sunlight to start defrosting their seasonal cover of carbon dioxide. Spots form where pressurized carbon dioxide gas escapes to the surface

PIX4580064

Martian dunes at the end of winter - March: Late Winter view of Dunes: Detail on dunes in the southern hemisphere of Mars. With the end of winter, the Sun melts the carbon dioxide ice present all winter. Image obtained by the HIRISE camera of the Mars Reconnaissance probe orbiter on March 21, 2016. HIRISE is a 50 cm telescope that observes visible and near infrared. Sand dunes cover much of this terrain, which has large boulders lying on flat areas between the dunes. It is now late winter here in the Southern hemisphere, and these dunes are just getting enough sunlight to start defrosting their seasonal cover of carbon dioxide. Spots form where pressurized carbon dioxide gas escapes to the surface

PIX4580064

 
Laminate structures near the north pole on Mars - Layers Exposed at North Polar Cap on Mars: Laminated structures near the north polar cap of Mars. These different layers of ice and girders correspond to climatic variations over the last ten thousand years. Image obtained on 18 April 2016 by the HIRISE camera on board the Mars Reconnaissance orbiter probe. HIRISE is a 50 cm telescope that observes visible and near infrared. At the edge of Mars' permanent North Polar cap, we see an exposure of the internal layers, each with a different mix of water ice, dust and dirt. These layers are believed to correspond to different climate conditions over the past tens of thousands of years. When we zoom in closer, we see that the distinct layers erode differently. Some are stronger and more resistant to erosion, others only weakly cemented. The strong layers form ledges

PIX4580071

Laminate structures near the north pole on Mars - Layers Exposed at North Polar Cap on Mars: Laminated structures near the north polar cap of Mars. These different layers of ice and girders correspond to climatic variations over the last ten thousand years. Image obtained on 18 April 2016 by the HIRISE camera on board the Mars Reconnaissance orbiter probe. HIRISE is a 50 cm telescope that observes visible and near infrared. At the edge of Mars' permanent North Polar cap, we see an exposure of the internal layers, each with a different mix of water ice, dust and dirt. These layers are believed to correspond to different climate conditions over the past tens of thousands of years. When we zoom in closer, we see that the distinct layers erode differently. Some are stronger and more resistant to erosion, others only weakly cemented. The strong layers form ledges

PIX4580071

 
Dunes near the north pole on Mars - Dunes at North Polar Cap on Mars: Image obtained on March 26, 2014 by the HIRISE camera on board the Mars Reconnaissance orbiter probe. HIRISE is a 50 cm telescope that observes visible and near infrared. Formative down-slope winds descending on Mars' North Polar ice cap likely play an important role in transporting sediment from the base of the ice cap into the dune fields that sit beyond the ice cap. The deep chasm that formed on the polar cap edge is identified as an area of strong down-slope winds and has a clear connection to Mars' largest dune field, Olympia Undae. Repeat HiRise images from this chasm that specifically targets the dunes, provides the basis to evaluate the sand fluxes which are associated with the dune and ripple movement in this area

PIX4580075

Dunes near the north pole on Mars - Dunes at North Polar Cap on Mars: Image obtained on March 26, 2014 by the HIRISE camera on board the Mars Reconnaissance orbiter probe. HIRISE is a 50 cm telescope that observes visible and near infrared. Formative down-slope winds descending on Mars' North Polar ice cap likely play an important role in transporting sediment from the base of the ice cap into the dune fields that sit beyond the ice cap. The deep chasm that formed on the polar cap edge is identified as an area of strong down-slope winds and has a clear connection to Mars' largest dune field, Olympia Undae. Repeat HiRise images from this chasm that specifically targets the dunes, provides the basis to evaluate the sand fluxes which are associated with the dune and ripple movement in this area

PIX4580075

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

PIX4616480

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

PIX4616480

 
The coldest place on Mars - Coolest place on Mars: Detail of the ice cap of the southern pole of Mars, composed mainly of carbon dioxide. This dry ice accumulates on the surface mainly in winter, the temperature of this area can sometimes drop to 130 degrees Celsius below zero. Image obtained on August 29, 2016 by the HIRISE camera on board the Mars Reconnaissance orbiter probe. HIRISE is a 50 cm telescope that observes visible and near infrared. The polar cap is made from carbon dioxide (dry ice), which does not occur naturally on the Earth. The circular pits are holes in this dry ice layer that expand by a few meters each Martian year. New dry ice is constantly being added to this landscape by freezing directly out of the carbon dioxide atmosphere or falling as snow. Freezing out the atmosphere like this limits how cold the surface can get to the frost point at -130 degrees Celsius (-200 F). Nowhere on Mars can ever get any colder this, making this coolest landscape on Earth and Mars

PIX4580080

The coldest place on Mars - Coolest place on Mars: Detail of the ice cap of the southern pole of Mars, composed mainly of carbon dioxide. This dry ice accumulates on the surface mainly in winter, the temperature of this area can sometimes drop to 130 degrees Celsius below zero. Image obtained on August 29, 2016 by the HIRISE camera on board the Mars Reconnaissance orbiter probe. HIRISE is a 50 cm telescope that observes visible and near infrared. The polar cap is made from carbon dioxide (dry ice), which does not occur naturally on the Earth. The circular pits are holes in this dry ice layer that expand by a few meters each Martian year. New dry ice is constantly being added to this landscape by freezing directly out of the carbon dioxide atmosphere or falling as snow. Freezing out the atmosphere like this limits how cold the surface can get to the frost point at -130 degrees Celsius (-200 F). Nowhere on Mars can ever get any colder this, making this coolest landscape on Earth and Mars

PIX4580080

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

PIX4616532

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

PIX4616532

 
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

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

 
Glaciers under Martian crateres - Buried glaciers on Mars - Computer reconstructed views of three Martian crateres in the Hellas region that house glaciers. The images show the crateres as they appear today with a layer of Martian soil covering the ice with water and, on the right, the glaciers updated according to radar measurements obtained by the Mars Reconnaissance Orbiter probe (MRO). These glaciers would have a thickness of 250 to 450 meters. Each image covers 20 km wide. This computer graphic image shows three craters in the eastern Hellas region of Mars containing concealed glaciers detected by radar. The images shows how the surface looks today with the ice covered with a layer of Martian soil and what the ice may look like underneath. The image was created using image data from the Context Camera on the Mars Reconnaissance Orbiter (MRO) spacecraft combined with results from the SHARAD radar sounder on MRO and HRSC digital elevation map from the Mars Express spacecraft. The co

PIX4616544

Glaciers under Martian crateres - Buried glaciers on Mars - Computer reconstructed views of three Martian crateres in the Hellas region that house glaciers. The images show the crateres as they appear today with a layer of Martian soil covering the ice with water and, on the right, the glaciers updated according to radar measurements obtained by the Mars Reconnaissance Orbiter probe (MRO). These glaciers would have a thickness of 250 to 450 meters. Each image covers 20 km wide. This computer graphic image shows three craters in the eastern Hellas region of Mars containing concealed glaciers detected by radar. The images shows how the surface looks today with the ice covered with a layer of Martian soil and what the ice may look like underneath. The image was created using image data from the Context Camera on the Mars Reconnaissance Orbiter (MRO) spacecraft combined with results from the SHARAD radar sounder on MRO and HRSC digital elevation map from the Mars Express spacecraft. The co

PIX4616544

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

PIX4616489

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

PIX4616489

 
Martian dunes in Spring - March: Spring view of Dunes - Detail on sand dunes near the north pole of Mars. These dunes are covered with carbon dioxide gel during the Martian winter. In spring, dark streaks appear, sand flows caused by the degel. Image obtained by the HIRISE camera of the Mars Reconnaissance probe orbiter on April 7, 2008. HIRISE is a 50 cm telescope that observes visible and near infrared. Falling Material Kicks Up Cloud of Dust on Dunes. There is a vast region of sand dunes at high northern latitudes on Mars. In the winter, a layer of carbon dioxide ice covers the dunes, and in the spring as the sun warms the ice it evaporates. This is a very active process, and sand dislodged from the crests of the dunes cascades down, forming dark streaks. In thid image falling material has kicked up a small cloud of dust. The color of the ice surrounding adjacent streaks of material suggests that dust has settled on the ice at the bottom after similar events. Also discernible in thi

PIX4616482

Martian dunes in Spring - March: Spring view of Dunes - Detail on sand dunes near the north pole of Mars. These dunes are covered with carbon dioxide gel during the Martian winter. In spring, dark streaks appear, sand flows caused by the degel. Image obtained by the HIRISE camera of the Mars Reconnaissance probe orbiter on April 7, 2008. HIRISE is a 50 cm telescope that observes visible and near infrared. Falling Material Kicks Up Cloud of Dust on Dunes. There is a vast region of sand dunes at high northern latitudes on Mars. In the winter, a layer of carbon dioxide ice covers the dunes, and in the spring as the sun warms the ice it evaporates. This is a very active process, and sand dislodged from the crests of the dunes cascades down, forming dark streaks. In thid image falling material has kicked up a small cloud of dust. The color of the ice surrounding adjacent streaks of material suggests that dust has settled on the ice at the bottom after similar events. Also discernible in thi

PIX4616482

 
Martian dunes in summer - Mars: Summer view of Dunes: Detail on dunes near the northern polar cap of Mars in summer. Image obtained by the HIRISE camera of the Mars Reconnaissance probe orbiter on 1 September 2008. HIRISE is a 50 cm telescope that observes visible and near infrared. This dune field formed near the base of the North Polar cap. Dunes require a source of loose particulate material to form. The source of the northern dune fields around the polar cap may be from the layers of dusty ice that are eroded by strong polar winds. This image was taken during the Martian northern summer, so there is no frost present on the dunes. The dunes closest to the base of the polar cap are long and parallel, indicating strong winds from the direction of the cap. As they get farther away from the polar cap, they start to form more crescent shaped dunes, called barchan dunes. Repeated observations by HiRise of dunes like these show measurable changes in some locations. This discovery adds to t

PIX4580056

Martian dunes in summer - Mars: Summer view of Dunes: Detail on dunes near the northern polar cap of Mars in summer. Image obtained by the HIRISE camera of the Mars Reconnaissance probe orbiter on 1 September 2008. HIRISE is a 50 cm telescope that observes visible and near infrared. This dune field formed near the base of the North Polar cap. Dunes require a source of loose particulate material to form. The source of the northern dune fields around the polar cap may be from the layers of dusty ice that are eroded by strong polar winds. This image was taken during the Martian northern summer, so there is no frost present on the dunes. The dunes closest to the base of the polar cap are long and parallel, indicating strong winds from the direction of the cap. As they get farther away from the polar cap, they start to form more crescent shaped dunes, called barchan dunes. Repeated observations by HiRise of dunes like these show measurable changes in some locations. This discovery adds to t

PIX4580056

 
March: Victoria crater. - March: Victoria Crater at Meridiani Planum - View of the Victoria crater obtained by the HIRISE camera on board the Mars Reconnaissance orbiter probe. This crater is 800 meters in diameter. The opportunity rover reached this crater on September 27, 2006. After exploring about a quarter of the crater's edges, the rover descended almost a year later to begin an exploration of the crater's interior. Victoria Crater, about 800 meters (one - half mile) in diameter, has been home ground for Nasa's Mars Exploration Rover Opportunity for more 14 of the rover's first 46 months on Mars. Opportunity first reached the crater's rim on Sept. 27, 2006, during the 951st Martian day, or sol, of the rover's work in the Meridian Planum region of Mars. The rover then explored clockwise about one - fourth of the way around the rim before returning to a point close to its first overlook. On the mission's 1,293rd sol (Sept. 13, 2007), Opportunity began a sustained exploration of the

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March: Victoria crater. - March: Victoria Crater at Meridiani Planum - View of the Victoria crater obtained by the HIRISE camera on board the Mars Reconnaissance orbiter probe. This crater is 800 meters in diameter. The opportunity rover reached this crater on September 27, 2006. After exploring about a quarter of the crater's edges, the rover descended almost a year later to begin an exploration of the crater's interior. Victoria Crater, about 800 meters (one - half mile) in diameter, has been home ground for Nasa's Mars Exploration Rover Opportunity for more 14 of the rover's first 46 months on Mars. Opportunity first reached the crater's rim on Sept. 27, 2006, during the 951st Martian day, or sol, of the rover's work in the Meridian Planum region of Mars. The rover then explored clockwise about one - fourth of the way around the rim before returning to a point close to its first overlook. On the mission's 1,293rd sol (Sept. 13, 2007), Opportunity began a sustained exploration of the

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