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Bright Exposures of Chloride Salt on Southern Mars
Bright Exposures of Chloride Salt on Southern Mars
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NASA's Mars Exploration Rover Spirit has this view northward from the position at the north edge of the "Home Plate" plateau where the rover will spend its third Martian winter.
View from Spirit's Overwintering Position (False Color)
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During four months prior to the fourth anniversary of its landing on Mars, Opportunity examined rocks inside an alcove called "Duck Bay" in the western portion of Victoria Crater.
'Lyell' Panorama inside Victoria Crater
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Dust-Devil Tracks in Southern Schiaparelli Basin
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NASA's twin Mars Exploration Rovers got smarter as they got older. This view from Opportunity shows the tracks left by a drive executed with more onboard autonomy than has been used on any other drive by a Mars rover.
D-Star Panorama by Opportunity
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This observation shows a wrinkle ridge in Solis Planum, located in the Thaumasia region of Mars, a high-elevation volcanic plain located south of the Valles Marineris canyon system and east of the Tharsis volcanic complex. Solis Planum contains some of the most distinct and well studied arrays of wrinkle ridges on Mars.

Wrinkle ridges are long, winding topographic highs and are often characterized by a broad arch topped with a crenulated ridge. These features have been identified on many other planetary bodies such as the Moon, Mercury, and Venus. On Mars, they are many tens to hundreds of kilometers long, tens of kilometers wide, and have a relief of a few hundred meters. Wrinkle ridges are most commonly believed to form from horizontal compression or shortening of the crust due to faulting and are often located in volcanic plains. They commonly have asymmetrical cross sectional profiles and an offset in elevation on either side of the ridge. Large dunes are also visible bordering the wrinkle ridge.

The reddish colors seen in this image most likely indicate the presence of dust (or indurated dust) and the darker, bluish colors most likely indicate the presence of larger rocks and boulders on the wrinkle ridge.
Wrinkle Ridge in Solis Planum
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Global View of Candor Chasm Study Location
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Spectrometer on NASA Orbiter Maps Minerals at Possible Landing Sites
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Color Image of Nili Fossae Trough, a Candidate MSL Landing Site
Color Image of Layers in Holden Crater, a Candidate MSL Landing Site
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NASA's Mars rovers keep getting bigger. This photo provides a comparison of the wheel sizes for three generations of them.
Rover Wheel Sizes (Isometric)
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The team developing NASA's Mars Science Laboratory calls this test rover "Scarecrow" because the vehicle does not include a computer brain. Mobility engineers use this test rover to evaluate mobility and suspension performance.
"Scarecrow"
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Onlookers watch as Scarecrow, a mobility-testing model for NASA's Mars Science Laboratory, easily conquers boulders in the Mars Yard testing area at NASA's Jet Propulsion Laboratory.
Shutterbugs Shoot "Scarecrow"
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An engineering model for NASA's Mars Science Laboratory makes its way up a hill in the Mars Yard testing area at NASA's Jet Propulsion Laboratory.
"Scarecrow" Descends Hill
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Scarecrow, a mobility-testing model for NASA's Mars Science Laboratory, easily traverses large rocks in the Mars Yard testing area at NASA's Jet Propulsion Laboratory.
"Scarecrow" Climbs Rocks
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Seven Possible Cave Skylights on Mars
Seven Possible Cave Skylights on Mars
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Lava-Draped Channel System on Mars
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On the southwest edge of the immense volcanic region of Tharsis, lava from its giant volcanoes flowed down to meet the old cratered landscape of Terra Sirenum.
A Colorful Marriage of Old & Young
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In Search of Landing Sites on Mars
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The formation of the large outflow channels on Mars have been attributed to catastrophic discharges of ground water. Many of the channels start in areas where the ground has apparently collapsed: the surface is now well below the surrounding undisturbed ground. Within the collapsed region, blocks of undisturbed material can often be seen and this has led to such regions being called chaotic terrain.

In Aureum Chaos, the OMEGA experiment on Mars Express indicated the presence of phyllosilicates (clay minerals) which have been detected in a variety of bright outcrops and scarps. The subimage shows such an outcrop in a chaotic terrain region. At the highest resolution, layering can be seen. The image will be used to assess at what stage in Mars's history these clays minerals were formed and how.

The area referred to as Aureum Chaos is located at 334 degrees East, 4 degrees South on the West side of the Margaritifer Terra region of Mars.
Light-Toned Outcrop in Aureum Chaos
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Phoenix Mars Lander's Chemistry Lab in a Box
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Microscopes for NASA's Phoenix Mars Lander
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Phoenix Mars Lander's Chemistry Lab in a Box
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Chemistry Lab for Phoenix Mars Lander
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Microscopes for NASA's Phoenix Mars Lander
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Chemistry Lab for Phoenix Mars Lander
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