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'Ice Flow' immagini e video risultati page 1 of 1

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Immagini di 'Ice Flow' trovate, 56

Watching an arctic ice flow from a camp on arctic ice 1930
Pancake ice adrift on the Ross Sea; Antarctica
Watching an arctic iceberg breakup during a cruise in the North Atlantic 1930
Russian forces cross an ice flow in Manchuria during the Russo-Japanese War, 1900
satellite view over Hudson Bay, Canada. Large ice flow is shown over the bay.
Ice Flow, 2015 (oil & acrylic on canvas on panel)
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Downstream Cool Flow, 2004 (acrylic collage on canvas)
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Penguins run across ice, Unites States, 1970s
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KAYAKER MANEUVERS AROUND ICE FLOW IN FRIGID WEATHER, 1998-12-24 (photo)
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MEMBER OF BERLIN'S ICE SWIMMING CLUB THROWS AWAY ICE FLOW IN ORANKE LAKE IN BERLIN, 2003-12-25 (photo)
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A RESIDENT OF MOKROPSY VILLAGE CHECKS AN ICE FLOW ON RIVER BEROUNKA, 2002-01-22 (photo)
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Unites States, 1970s: men dig ice from roof of submarine
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Ironbridge gorge and world's first iron bridge with ice flows in River Severn, Ironbridge, Shropshire, England (photo)
Unites States, 1970s: penguins jump out of water onto ice
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Unites States, 1970s: close up of icebreaker ship at sea
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Unites States, 1970s: man presents to camera from beach
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Battle cruiser Seydlitz. Black steam from the front funnel. Ice drift and seagulls (b/w photo)
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Dave Kreitzmann manuevers his kayak around an ice flow on the Rock River near Rockford, Illinois on .., 1998-12-24 (photo)
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Rock Creek Park, Washington, D.C. 2007 (photo)
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 color of the Martian surface and ice was estimated from MRO HiRise color images of other Martian craters and the polar ice caps. The buried ice in these craters as measured by SHARAD is ~ 250 meter thick on the upper crater and ~ 300 and 450 meters on the middle and lower levels respectively. Each image is 20 km (12.8 mi.) across and extends to 50 km (32 mi) in the distance. Recent measurements from the Mars Reconnaissance Orbiter SHARAD radar sounder have detected large amounts of water ice in such deposits over widespread areas, arguing for the flow of glacial - like structures on Mars in the relatively recent geologic past. This suggests that snow and ice accumulated on higher topography, flowed downhill and is now protected from sublimation by a layer of rock debris and dust. Furrows and ridges on the surface were caused by deforming ice
Retreat of the Helheim Glacier, Greenland - Retreat of the Helheim Glacier, Greenland - These three photos show the Helheim Glacier in Greenland in June 2005 (top), July 2003 (middle) and May 2001 (bottom). The glacier occupies the left part of the images, the icebergs on the fjord on the right. Between 2001 and 2005, the glacier front retreated 7.5 km. Images obtained from the Terra satellite. Retreat of the Helheim Glacier, Greenland Along the margin of the Greenland Ice Sheet, outlet glaciers flow as icy rivers through narrow fjords and out to sea. As long as the thickness of the glacier and the depth of the water allow the ice to remain grounded, it stays intact. Where the ice becomes too thin or the water too deep, the edge floats and rapidly crumbles into icebergs. Satellite observations of eastern Greenland's Helheim Glacier show that the position of the iceberg's calving front, or margin, has undergone rapid and dramatic change since 2001, and the glacier's flow to the sea has sped up as well. These images from the Advanced Spaceborne Thermal Emission and Reflection Radiometer (ASTER) on Nasa's Terra satellite show the Helheim glacier in June 2005 (top), July 2003 (middle), and May 2001 (bottom). The glacier occupies the left part of the images, while large and small icebergs pack the narrow fjord in the right part of the images. Bare ground appears brown or tan, while vegetation appears in shades of red. From the 1970s until about 2001, the position of the glacier's margin changed little. But between 2001 and 2005, the margin retreated landward about 7.5 kilometers (4.7 miles), and its speed increased from 8 to 11 kilometers per year. Between 2001 and 2003, the glacier also thinned by up to 40 meters (about 131 feet). Overall, the margins of the Greenland Ice Sheet have been thinning by tens of meters over the last decade
Time Running Out, 2022, (tinted gesso on wood)
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Niagara Falls from International Bridge (b/w photo)
Upper Steel Arch Bridge, Niagara (b/w photo)
Polar bear, Ursus maritimus (Ursus polaris) on an ice flow. Vulnerable. Lithograph by Karl Joseph Brodtmann from Heinrich Rudolf Schinz's Illustrated Natural History of Men and Animals, 1836.
Niagara Falls from Prospect Point (photo)
March: Promethei Planum - Mars: Promethei Planum - Promethei Planum is a region located near the southern pole of Mars. This region is seasonally covered with a thick layer of ice up to 3500 metres thick. On this image obtained by the Mars Express probe on September 22, 2005, an impact crater about 100 km wide and 800 metres deep is visible to the right (north). It is partially covered with ice. In the center of the image, structures formed by lava flows; on the left of the image, ice, which is an extension of the southern polar cap. Promethei Planum, an area seasonally covered with layer of ice more than 3500 m thick layer of ice in the martian south polar region, was the subject of the High Resolution Stereo Camera's focus on 22 September 2005 as Mars Express was in orbit above the Red Planet. Promethei Planum lies at approximately 76* south and 105* east. An approximately 100 km - large and 800 m - deep impact crater is visible in the northern part of the image. The crater's interior is partly covered in ice. In the centre of the image are structures that may have been created by basaltic lava flow from a volcano. This area is covered in ice. The dark dunes towards the bottom of the image are most likely made up of dust originating from this lava flow or volcanic ash. A broad sheet of ice, which is an extension of the south polar ice cap is located south of the lava flow, to the left in the (nadir) image. The steep flanks clearly show white, clean ice. The thickness of the ice is between 900 and 1100 m
March: Promethei Planum - Mars: Promethei Planum - Promethei Planum is a region located near the southern pole of Mars. This region is seasonally covered with a thick layer of ice up to 3500 metres thick. On this perspective image obtained by the Mars Express probe on September 22, 2005, an impact crater about 100 km wide and 800 metres deep is visible at the bottom of the image. It is partially covered with ice. On top, structures formed by lava flows; at the top of the picture, ice, which is an extension of the southern polar cap. Promethei Planum, an area seasonally covered with layer of ice more than 3500 m thick layer of ice in the martian south polar region, was the subject of the High Resolution Stereo Camera's focus on 22 September 2005 as Mars Express was in orbit above the Red Planet. Promethei Planum lies at approximately 76* south and 105* east. An approximately 100 km - large and 800 m - deep impact crater is visible in the bottom of the image. The crater's interior is partly covered in ice. Above, are structures that may have been created by basaltic lava flow from a volcano. This area is covered in ice. The dark dunes towards the left side of the image are most likely made up of dust originating from this lava flow or volcanic ash. A broad sheet of ice, which is an extension of the south polar ice cap is visible in the higher part of the image. The steep flanks clearly show white, clean ice. The thickness of the ice is between 900 and 1100 m
Icefall on the Dnieper, 1942 (b/w photo)
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Icefall on the Dnieper, 1942 (b/w photo)
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Anticipation: wireless telegraphy. In "Readings for All" of May 15, 1913 (print)
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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 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 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
Mars: crater in Myers Valles - Mars: crater in Myers Valles - Mamers Valles is a valley about 1000 km long located in the region of Deuteronilus Mensae, north of Arabia Terra. The image obtained by the Mars Express probe on 5 August 2006 shows a crater at the end of this valley. This circular formation measures about thirty kilometres in diameter and is 1400 metres deep. There are traces of flow of material probably composed of water ice, similar to the relief left by the passage of glaciers on Earth. The High - Resolution Stereo Camera (HRSC) onboard the ESA spacecraft Mars Express obtained images focusing on a depression that displays a crater at the end of the long, winding valley, Mamers Valles. The data was obtained on 5 August 2006 with a ground resolution of approximately 14 m/per pixel. The image is centred at approximately 39* north and 17* east on the planet. The valley of Mamers Valles is approximately 1000 km long, running along the boundary between the northern lowlands and southern highlands in the region of Deuteronilus Mensae. This region shows numerous deep and wide labyrinth - like valleys and circular depressions which often show structures formed by flowing liquid on their even floors. The structures formed by the flows are thought to be ice - rich debris flows. They show some resemblance to block glaciers seen on Earth. The patches of rock at the centre of the depression are thought to be remnants of rock detached from the flanks of the depression and transported into its centre. The wrinkle ridges, are formed by compressive forces acting on the surface. The dark coloured material inside the crater could have formed in - situ or was transported by the wind. The depression is approximately 30 km wide and 1400 m deep
Mars: crater in Myers Valles - Mars: crater in Myers Valles - Mamers Valles is a valley about 1000 km long located in the region of Deuteronilus Mensae, north of Arabia Terra. The image obtained by the Mars Express probe on 5 August 2006 shows a crater at the end of this valley. This circular formation measures about thirty kilometres in diameter and is 1400 metres deep. There are traces of flow of material probably composed of water ice, similar to the relief left by the passage of glaciers on Earth. The darker area could be caused by local erosion or wind-driven material. The High - Resolution Stereo Camera (HRSC) onboard the ESA spacecraft Mars Express obtained images focusing on a depression that displays a crater at the end of the long, winding valley, Mamers Valles. The data was obtained on 5 August 2006 with a ground resolution of approximately 14 m/per pixel. The image is centred at approximately 39* north and 17* east on the planet. The valley of Mamers Valles is approximately 1000 km long, running along the boundary between the northern lowlands and southern highlands in the region of Deuteronilus Mensae. This region shows numerous deep and wide labyrinth - like valleys and circular depressions which often show structures formed by flowing liquid on their even floors. The structures formed by the flows are thought to be ice - rich debris flows. They show some resemblance to block glaciers seen on Earth. The patches of rock at the centre of the depression are thought to be remnants of rock detached from the flanks of the depression and transported into its centre. The wrinkle ridges, are formed by compressive forces acting on the surface. The dark coloured material inside the crater could have formed in - situ or was transported by the wind. The depression is approximately 30 km wide and 1400 m deep
Mars: crater in Myers Valles - Mars: crater in Myers Valles - Mamers Valles is a valley about 1000 km long located in the region of Deuteronilus Mensae, north of Arabia Terra. The image obtained by the Mars Express probe on 5 August 2006 shows a crater at the end of this valley. This circular formation measures about thirty kilometres in diameter and is 1400 metres deep. There are traces of flow of material probably composed of water ice, similar to the relief left by the passage of glaciers on Earth. The darker area could be caused by local erosion or wind-driven material. The High - Resolution Stereo Camera (HRSC) onboard the ESA spacecraft Mars Express obtained images focusing on a depression that displays a crater at the end of the long, winding valley, Mamers Valles. The data was obtained on 5 August 2006 with a ground resolution of approximately 14 m/per pixel. The image is centred at approximately 39* north and 17* east on the planet. The valley of Mamers Valles is approximately 1000 km long, running along the boundary between the northern lowlands and southern highlands in the region of Deuteronilus Mensae. This region shows numerous deep and wide labyrinth - like valleys and circular depressions which often show structures formed by flowing liquid on their even floors. The structures formed by the flows are thought to be ice - rich debris flows. They show some resemblance to block glaciers seen on Earth. The patches of rock at the centre of the depression are thought to be remnants of rock detached from the flanks of the depression and transported into its centre. The wrinkle ridges, are formed by compressive forces acting on the surface. The dark coloured material inside the crater could have formed in - situ or was transported by the wind. The depression is approximately 30 km wide and 1400 m deep
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