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The 4 kilometer (2.5 mile) diameter crater in this image appears relatively fresh, but not remarkably so.
The 4 kilometer diameter crater in this image appears relatively fresh, but with little erosion or underground upheaval on Mars and no evidence of an extremely recent meteor hit, "fresh" is a relative term.NASA/JPL-Caltech/University of Arizona
The 4 kilometer (2.5 mile) diameter crater in this image appears relatively fresh, but not remarkably so.
A towering dust devil casts a serpentine shadow over the Martian surface in this stunning, late springtime image of Amazonis Planitia. The length of the shadow indicates that the dust plume reaches more than 800 meters, or half a mile, in height.
Mars has extremely large temperature changes from winter to summer compared to the Earth. It gets cold enough to freeze carbon dioxide out of the atmosphere during the winter, but this ice is unstable when the warmer summer arrives and forces it to sublimate (transform directly back into a gas) away.
On Mars the seasonal polar caps are composed of dry ice (carbon dioxide). In the springtime as the sun shines on the ice, it turns from solid to gas and causes erosion of the surface.
A "fossa" is a cavity or depression..Floods of water and lava are thought to have emanated from the larger fossae nearby, perhaps forming the Athabasca channel and later filling it with lava.
Most of the dunes visible in this observation are barchan dunes. On barchan dunes, the steep slip face is between two "horns" that point downwind.
HiRISE acquired this color image of Santa Maria Crater, with the Opportunity rover perched on the southeast rim. Rover tracks are clearly visible to the east.Opportunity has been studying this relatively fresh 90 meter diameter crater to better understand how crater excavation occurred during the impact and how it has been modified by weathering and erosion since.
The dune gullies (at edge of the field and here in this subimage) appear active and are anomalous in their location (high latitude).
The dunes imaged here are similar to barchan dunes, commonly found in desert regions on Earth.
Sand dunes are among the most widespread aeolian features present on Mars. Their spatial distribution and morphology, sensitive to subtle shifts in wind circulation patterns and wind strengths, can relate to patterns of erosion and deposition, and give clues to the sedimentary history of the surrounding terrain.
This image is located within Aram Chaos near the outlet to Ares Valles. Aram Chaos is a 1300 kilometer (approximately 800 miles) diameter depression from which enormous cataclysmic releases of ground water are thought to have exploded onto the surface of Mars. The water then flowed northwards across the southern highlands, helping to carve the approximately 2000 kilometer (1200 miles) long Ares Valles outflow channel system.
Sand dunes are among the most widespread aeolian features present on Mars. Their spatial distribution and morphology are sensitive to subtle shifts in wind circulation patterns and wind strengths. These provide clues to the sedimentary history of the surrounding terrain.
The 4 kilometer diameter crater in this image appears relatively fresh, but with little erosion or underground upheaval
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NASA/JPL-Caltech/University of Arizona
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Martian Vistas: A Look at the Curiosity Rover’s Strange Home

Aug 06, 2014
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