The so-called 'Face on Mars' can be seen slightly above center and to the right in this NASA Mars Odyssey image. This 3-km long knob was first imaged by NASA's Viking spacecraft in the 1970's and to some resembled a face carved into the rocks of Mars.

The so-called 'Face on Mars' can be seen slightly above center and to the right in this NASA Mars Odyssey image. This 3-km long knob was first imaged by NASA's Viking spacecraft in the 1970's and to some resembled a face carved into the rocks of Mars.
SuperStock offers millions of photos, videos, and stock assets to creatives around the world. This image of The so-called 'Face on Mars' can be seen slightly above center and to the right in this NASA Mars Odyssey image. This 3-km long knob was first imaged by NASA's Viking spacecraft in the 1970's and to some resembled a face carved into the rocks of Mars. by Piemags/PL Photography Limited is available for licensing today.

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Kepler's Rim
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This image from NASA's Mars Reconnaissance Orbiter spacecraft contains interesting examples of crosscutting, sinuous and straight ridges. Both ridges may be ancient river deposits.
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The North Polar layered deposits (NPLD) are a stack of layers of ice and dust at the North Pole of Mars. The layers are thought to have been deposited over millions of years. This image is from NASA's Mars Reconnaissance Orbiter.
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Cross-Cutting Faults
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Sirenum Troughs
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Athabasca Vallis Streamlined Islands
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During periods in Mars' history when the planet had greater axial tilt, shifts in atmospheric circulation may have favored the extensive accumulation of snow in some locations. Protonilus Mensae is just such a site of extensive glaciation. We can see a flow of material through the valleys between a complex of small mesas. Streamlines and flow fronts appear as subtle ridges. Some ridges appear perpendicular to the mesas indicating flow direction. Others appear concentric to the mesas and parallel to the valleys, where debris and now-underlying ice bunched up and moved down valley. Deflation of the ice has led to a rich collection of small-scale features. Polygonal patterns of fractures and fissures may be related to a combination of thermal contraction cycles and overall subsidence of the surface. Larger fractures may be glacial crevasses, caused by differential flow rates in the underlying ice. Other more complex patterns of swirled pits and hummocks may result from the continual loss
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THEMIS Images as Art #14
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Double Impact
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Images of the Cydonia region of Mars continue to be popular among visitors to the Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC)web site. The two pictures (one annotated, the other not) are mosaics of two images from MGS MOC and one from the Mars Odyssey Thermal Emission Imaging System visible camera (THEMIS VIS). The mosaics highlight a Cydonia landform popularly known as the D&M Pyramid. It is located near 40.7°N, 9.6°W. Although it is not really shaped like a pyramid, the Cydonia landform is one of thousands of massifs, buttes, mesas, knobs, and blocks that mark the transition from the far northwestern Arabia Terra cratered highlands down to the northeastern Acidalia Planitia lowlands. Each block, whether shaped like a face, a pyramid, or simply a mesa, massif, or knob, is a remnant of the bedrock of northeastern Arabia that was left behind as erosion slowly degraded the terrain along this zone between the highlands and the lowlands. A few outcroppings of layers in this ancien
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Ancient Paleo-Dunes Battered by Impact Craters
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Image Number: 6145-44576477Royalty FreeCredit Line:Piemags/PL Photography Limited/SuperStockCollection:PL Photography LimitedStory:Martian Geological FeaturesContributor:PiemagsModel Release:NoProperty Release:NoResolution:967×2738
2001 Mars Odyssey
Mars|