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Back-and-forth blinking of this two-image animation shows movement of a sand dune on Mars. The images are part of a study published by Nature on May 9, 2012, reporting movement of Martian sand dunes at about the same flux (volume per time) as movement of dunes in Antarctica on Earth.
Advancing Dune in Nili Patera, Mars
Back-and-forth blinking of this two-image animation shows movement of ripples covering a sand dune on Mars.
Ripple Movement on Sand Dune in Nili Patera, Mars
A Martian dust devil roughly 12 miles (20 kilometers) high was captured winding its way along the Amazonis Planitia region of Northern Mars on March 14, 2012 by the High Resolution Imaging Science Experiment (HiRISE) camera on NASA's Mars Reconnaissance Orbiter.
Mars' Whirling Dust Devil
A towering dust devil, casts a serpentine shadow over the Martian surface in this image acquired by the High Resolution Imaging Science Experiment (HiRISE) camera on NASA's Mars Reconnaissance Orbiter.
The Serpent Dust Devil of Mars
This image, taken Jan. 26, 2012, shows NASA's no-longer-active Phoenix Mars Lander spacecraft after its second Martian arctic winter.
Phoenix Lander After Second Martian Winter
Near the lower left corner of this view is the three-petal lander platform that NASA's Mars Exploration Rover Spirit drove off in January 2004.
Spirit Lander and Bonneville Crater in Color
This image, taken Jan. 26, 2012, shows the back shell of NASA's Phoenix Mars Lander spacecraft after its second Martian arctic winter.
Phoenix Back Shell After Second Martian Winter
This enhanced-color image shows sand dunes trapped in an impact crater in Noachis Terra, Mars.
Dunes in Noachis Terra Region of Mars
This scene is from early spring in the northern hemisphere of Mars. These dunes are covered with a layer of seasonal carbon dioxide ice (dry ice).
Edge of North Polar Erg
Recent small craters discovered by the High Resolution Imaging Science Experiment camera on NASA's Mars Reconnaissance Orbiter expose buried ice in the middle latitudes of Mars.
Fresh Crater Revealing Buried Ice
A rippled patch of sand in Becquerel Crater on Mars moved about two meters (about two yards) between November 24, 2006 and September 5, 2010, as observed in these images taken by NASA's Mars Reconnaissance Orbiter.
Blowing in the Martian Wind
The eastern margin of a rippled dune in Herschel Crater on Mars moved an average distance of three meters (about three yards) between March 3, 2007 and December 1, 2010, as seen by NASA's Mars Reconnaissance Orbiter.
Shifting Sand in Herschel Crater
A rippled dune front in Herschel Crater on Mars moved an average of about two meters (about two yards) between March 3, 2007 and December 1, 2010, as seen in these images from NASA's Mars Reconnaissance Orbiter.
Rippling Dune Front in Herschel Crater on Mars
A rippled dune front in Herschel Crater on Mars moved an average of about one meter (about one yard) between March 3, 2007 and December 1, 2010, as seen in these images from NASA's Mars Reconnaissance Orbiter.
Rippling Dune Front in Herschel Crater on Mars
A dune in the northern polar region of Mars shows significant changes between two images taken on June 25, 2008 and May 21, 2010 by NASA's Mars Reconnaissance Orbiter.
Movement in Martian Dune Field
Impact cratering and erosion combine to reveal the composition of the Martian underground by exposing materials from the subsurface.
Clay Minerals in Craters and Escarpments on Mars
Impact cratering and erosion combine to reveal the composition of the Martian underground by exposing materials from the subsurface.
Clay Minerals in Craters and Escarpments on Mars (Figure 1)
Impact cratering and erosion combine to reveal the composition of the Martian underground by exposing materials from the subsurface.
Clay Minerals in Craters and Escarpments on Mars (Figure 3)
Impact cratering and erosion combine to reveal the composition of the Martian underground by exposing materials from the subsurface.
Clay Minerals in Craters and Escarpments on Mars (Figure 4)
Impact cratering and erosion combine to reveal the composition of the Martian underground by exposing materials from the subsurface.
Clay Minerals in Craters and Escarpments on Mars (Figure 2)
This map of Mars shows relative locations of three types of findings related to salt or frozen water, plus a new type of finding that may be related to both salt and water.
Ice, Salt and Warm-Season Flows on Mars
Unfrozen brine in cryopegs and fracture networks provides habitats for the survival and growth of organisms both within and under frozen rocky materials on Earth and, by analogy, could provide habitats on Mars.
Plausible Martian Habitats
An image combining orbital imagery with 3-D modeling shows flows that appear in spring and summer on a slope inside Mars' Newton crater.
Oblique View of Warm Season Flows in Newton Crater
This image contrasts gullies and recurring warm-season slope flows appearing in the same crater, in the middle southern latitudes of Mars.
Gullies and Newly Identified Flow Features in Same Mars Crater (Arrows)
This image contrasts gullies and recurring warm-season slope flows appearing in the same crater, in the middle southern latitudes of Mars.
Gullies and Newly Identified Flow Features in Same Mars Crater
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