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2001 Mars Odyssey
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Although it is 45 kilometers (28 miles) wide, countless layers of ice and dust have all but buried Udzha Crater.
Mars Odyssey All Stars: Udzha Crater
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West of Valles Marineris lies a checkerboard named Noctis Labyrinthus, which formed when the Martian crust stretched and fractured.
Mars Odyssey All Stars: Noctis Vista
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A false-color mosaic focuses on one junction in Noctis Labyrinthus where canyons meet to form a depression 4,000 meters (13,000 feet) deep.
Mars Odyssey All Stars: Noctis Canyon
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Fans and ribbons of dark sand dunes creep across the floor of Bunge Crater in response to winds blowing from the direction at the top of the picture.
Mars Odyssey All Stars: Bunge Crater Dunes
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In Ares Vallis, teardrop mesas extend like pennants behind impact craters, where the raised rocky rims diverted the floods and protected the ground from erosion.
Mars Odyssey All Stars: Ares Vallis
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Wind shadow and real shadow combine to give a striking image of a comet.
THEMIS Images as Art
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Mars Odyssey Project Manager Gaylon McSmith, of NASA's Jet Propulsion Laboratory
Mars Odyssey Project Manager Gaylon McSmith
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Large fractures have formed 'steps' in this region of Tempe Terra.
Tempe Terra
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This image shows a 90-mile-wide portion of the giant Valles Marineris canyon system. Landslide debris and gullies in the canyon walls on Mars can be seen at 100 meters (330 feet) per pixel.
Close View of Valles Marineris
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Valles Marineris, the "Grand Canyon of Mars," sprawls wide enough to reach from Los Angeles to nearly New York City, if it were located on Earth. The red outline box shows the location of a second, full-resolution image.
Valles Marineris, the "Grand Canyon of Mars"
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This unnamed channel is located in Xanthe Terra.
Channel in Xanthe Terra
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Martian Pit Feature Found by Seventh Graders
Martian Pit Feature Found by Seventh Graders
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Orbital View of Opportunity's Region
Orbital View of Opportunity's Region
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Stages in the seasonal disappearance of surface ice from the ground around the Phoenix Mars Lander are visible in these images taken on Feb. 8, 2010, (left) and Feb. 25, 2010, during springtime on northern Mars.
Ice Around Phoenix Lander Continues to Lessen in Spring
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Phoenix Lander Amid Disappearing Spring Ice
Phoenix Lander Amid Disappearing Spring Ice
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Continuing our survey of non-crater dune fields brings us to this group of dunes in Aonia Terra. The daytime IR illustrates the warmth of the dune material compared to the surrounding materials.
Aonia Terra Dunes
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Pastel colors swirl across Mars, revealing differences in the composition and nature of the surface in this false-color infrared image.
Improved Infrared Imaging from Changed Odyssey Orbit
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This image superimposes Gamma-Ray Spectrometer data from NASA's Mars Odyssey orbiter onto topographic data from the laser altimeter on NASA's Mars Global Surveyor.
Potassium Concentrations on Mars
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Chloride Salt Deposit in Southern Highlands of Mars
Bright Exposures of Chloride Salt on Southern Mars
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Seven Possible Cave Skylights on Mars
Seven Possible Cave Skylights 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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Odyssey Views A Surface Changed by Floods
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The floor of this unnamed crater in Aonia Terra has been filled with multiple layers of material.
Layered Fill
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The dune field in this polar region crater looks like a stubby arrow pointing the way west. This unnamed crater is located in Planum Chronium.
Unnamed crater is located in Planum Chronium.
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