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In this image from NASA's Mars Odyssey, eroded mesas and secondary craters dot the landscape in an area of Cydonia Mensae. The single oval-shaped crater displays a 'butterfly' ejecta pattern, indicating that the crater formed from a low-angle impact.
In this image from NASA's Mars Odyssey, eroded mesas and secondary craters dot the landscape in an area of Cydonia Mensae. The single oval-shaped crater displays a 'butterfly' ejecta pattern, indicating that the crater formed from a low-angle impact.

Cydonia Craters

The floor of the crater in this NASA Mars Odyssey image displays interesting textures and it appears to have been flooded by some type of material. It is unclear if this material was fluvially emplaced mud (hyperconcentrated flows) or lava.
The floor of the crater in this NASA Mars Odyssey image displays interesting textures and it appears to have been flooded by some type of material. It is unclear if this material was fluvially emplaced mud (hyperconcentrated flows) or lava.

Flooded Crater in Terra Sirenum

Pavonis Mons is the middle of the three large volcanoes on the Tharsis bulge. This image from NASA's Mars Odyssey spacecraft covers the edge of the volcano's caldera. Outside of the caldera, numerous lava flows and impact craters can be seen.
Pavonis Mons is the middle of the three large volcanoes on the Tharsis bulge. This image from NASA's Mars Odyssey spacecraft covers the edge of the volcano's caldera. Outside of the caldera, numerous lava flows and impact craters can be seen.

Pavonis Mons Caldera

Just north of the hematite deposit in Meridiani Planum, the remnants of a formerly extensive layer of material remain as isolated knobs and buttes in this image from NASA's Mars Odyssey spacecraft.
Just north of the hematite deposit in Meridiani Planum, the remnants of a formerly extensive layer of material remain as isolated knobs and buttes in this image from NASA's Mars Odyssey spacecraft.

Martian Braille

Dunes in the Vastitas Borealis region of Mars are seen in this image from NASA's Mars Odyssey spacecraft. These sand seas migrate around the north polar cap following the strong polar vortex winds.
Dunes in the Vastitas Borealis region of Mars are seen in this image from NASA's Mars Odyssey spacecraft. These sand seas migrate around the north polar cap following the strong polar vortex winds.

Polar Dunes

The smooth plains of Elysium embay the blocky broken up highlands of Aeolis in this image from NASA's Mars Odyssey spacecraft. The plains have been interpreted by researchers to be possibly mudflows or lava flows.
The smooth plains of Elysium embay the blocky broken up highlands of Aeolis in this image from NASA's Mars Odyssey spacecraft. The plains have been interpreted by researchers to be possibly mudflows or lava flows.

Highland/Lowland contact

This image from NASA's Mars Odyssey spacecraft shows part of Ganges Chasma in Valles Marineris. The colors indicate compositional variations in the rocks exposed in the wall and floor of Ganges and in the dust and sand on the rim of the canyon.
This image from NASA's Mars Odyssey spacecraft shows part of Ganges Chasma in Valles Marineris. The colors indicate compositional variations in the rocks exposed in the wall and floor of Ganges and in the dust and sand on the rim of the canyon.

Ganges Chasma

Images from NASA's Mars Odyssey spacecraft were used to create this mosaic of nighttime infrared images of Gusev Crater, which has been draped over topography data obtained by NASA's Mars Global Surveyor.
Images from NASA's Mars Odyssey spacecraft were used to create this mosaic of nighttime infrared images of Gusev Crater, which has been draped over topography data obtained by NASA's Mars Global Surveyor.

Gusev Crater

This mosaic of daytime infrared images of Gusev Crater, taken by NASA's Mars Odyssey spacecraft, has been draped over topography data obtained by NASA's Mars Global Surveyor.
This mosaic of daytime infrared images of Gusev Crater, taken by NASA's Mars Odyssey spacecraft, has been draped over topography data obtained by NASA's Mars Global Surveyor.

Gusev Crater

This graphic shows the radiation dose equivalent as measured by NASA's Mars Odyssey and by instruments aboard the International Space Station, for the 11-month period from April 2002 through February 2003.
This graphic shows the radiation dose equivalent as measured by NASA's Mars Odyssey and by instruments aboard the International Space Station, for the 11-month period from April 2002 through February 2003.

Comparison of Martian Radiation Environment with International Space Station

NASA's Mars Odyssey produced this gamma ray spectrometer map of the mid-latitude region of Mars is based on gamma-rays from the element silicon, one of the most abundant elements on the surface of both Mars and Earth.
NASA's Mars Odyssey produced this gamma ray spectrometer map of the mid-latitude region of Mars is based on gamma-rays from the element silicon, one of the most abundant elements on the surface of both Mars and Earth.

Map of Martian Silicon at Mid-Latitudes

NASA's Mars Odyssey spacecraft produced this gamma ray spectrometer map, which is centered on the north pole of Mars and based on gamma-rays from the element hydrogen. In this region, hydrogen is mainly in the form of water ice.
NASA's Mars Odyssey spacecraft produced this gamma ray spectrometer map, which is centered on the north pole of Mars and based on gamma-rays from the element hydrogen. In this region, hydrogen is mainly in the form of water ice.

Map of Martian Polar Hydrogen

This gamma ray spectrometer map from NASA's Mars Odyssey of the mid-latitude region of Mars is based on gamma-rays from the element iron, one of the most abundant elements on Mars and Earth. It is responsible for the red color on the surface of Mars.
This gamma ray spectrometer map from NASA's Mars Odyssey of the mid-latitude region of Mars is based on gamma-rays from the element iron, one of the most abundant elements on Mars and Earth. It is responsible for the red color on the surface of Mars.

Map of Martian Iron at Mid-Latitudes

An unusual mix of textures is featured in this image from NASA's Mars Odyssey spacecraft of a surface east of the Phlegra Montes. Scabby mounds, commonly occurring around degraded craters, mix with a more muted, knobby terrain.
An unusual mix of textures is featured in this image from NASA's Mars Odyssey spacecraft of a surface east of the Phlegra Montes. Scabby mounds, commonly occurring around degraded craters, mix with a more muted, knobby terrain.

Textures in Arcadia Planitia

With its rim eroded off by catastrophic floods in Tiu Vallis and its strangely angular shape, this 12 km (about 7.5 mile) diameter crater imaged by NASA's Mars Odyssey spacecraft looks vaguely like a stop sign.
With its rim eroded off by catastrophic floods in Tiu Vallis and its strangely angular shape, this 12 km (about 7.5 mile) diameter crater imaged by NASA's Mars Odyssey spacecraft looks vaguely like a stop sign.

Stop Sign Crater

The wind-sculpted yardangs in this scene from NASA's Mars Odyssey spacecraft are part of the Medusae Fossae Formation, a regionally extensive geologic unit that probably was produced from the accumulation of volcanic ash.
The wind-sculpted yardangs in this scene from NASA's Mars Odyssey spacecraft are part of the Medusae Fossae Formation, a regionally extensive geologic unit that probably was produced from the accumulation of volcanic ash.

Memnonia Sulci

The long sharp-crested features observed in this image from NASA's Mars Odyssey spacecraft are named yardangs. Yardangs form by wind erosion and typically lie in the direction of the dominant wind.
The long sharp-crested features observed in this image from NASA's Mars Odyssey spacecraft are named yardangs. Yardangs form by wind erosion and typically lie in the direction of the dominant wind.

Lycus Sulci

The top half of this NASA Mars Odyssey image shows interior layered deposits that have long been recognized in Valles Marineris. Upon close examination, the layers appear to be eroding differently, indicating different levels of competency.
The top half of this NASA Mars Odyssey image shows interior layered deposits that have long been recognized in Valles Marineris. Upon close examination, the layers appear to be eroding differently, indicating different levels of competency.

Valles Marineris - with 3-D

This image from NASA's Mars Odyssey spacecraft shows the easternmost end of Valles Marineris, where a rugged, jumbled terrain known as chaos displays a stratigraphy that could be described as precarious.
This image from NASA's Mars Odyssey spacecraft shows the easternmost end of Valles Marineris, where a rugged, jumbled terrain known as chaos displays a stratigraphy that could be described as precarious.

Arsinoes Chaos

The sinuous channel in this NASA Mars Odyssey image begins at the edge of Cerulli Crater in northern Arabia and snakes its way across 1,000 km (621 miles) of cratered highlands before reaching Deuteronilus Mensae at the boundary of the northern lowlands.
The sinuous channel in this NASA Mars Odyssey image begins at the edge of Cerulli Crater in northern Arabia and snakes its way across 1,000 km (621 miles) of cratered highlands before reaching Deuteronilus Mensae at the boundary of the northern lowlands.

Mamers Vallis

Freedom crater, located in Acidalia Planitia, exhibits a concentric ring pattern in its interior as seen in this image from NASA's Mars Odyssey spacecraft, suggesting that there has been some movement of these materials towards the center of the crater.
Freedom crater, located in Acidalia Planitia, exhibits a concentric ring pattern in its interior as seen in this image from NASA's Mars Odyssey spacecraft, suggesting that there has been some movement of these materials towards the center of the crater.

Freedom Crater

This image from NASA's Mars Odyssey spacecraft shows Granicus Vallis, which is located northwest of the Elysium volcanic complex and may owe its origin to the interaction of volcanic heating and subsurface ground ice.
This image from NASA's Mars Odyssey spacecraft shows Granicus Vallis, which is located northwest of the Elysium volcanic complex and may owe its origin to the interaction of volcanic heating and subsurface ground ice.

Granicus Vallis

This visible-light image, taken by NASA's Mars Odyssey spacecraft, indicates that gullies on Martian crater walls may be carved by liquid water melting from remnant snow packs.
This visible-light image, taken by NASA's Mars Odyssey spacecraft, indicates that gullies on Martian crater walls may be carved by liquid water melting from remnant snow packs.

Gullies on Martian Crater (THEMIS)

This somewhat cloudy image from NASA's Mars Odyssey spacecraft shows a stunning example of layered deposits in Terby crater, just north of the Hellas impact basin.
This somewhat cloudy image from NASA's Mars Odyssey spacecraft shows a stunning example of layered deposits in Terby crater, just north of the Hellas impact basin.

Layered Deposits in Terby Crater

In this NASA Mars Odyssey image of western Acidalia, two craters of similar size dramatically display the effects of geologic activity. The younger one on the left has been left relatively well preserved.
In this NASA Mars Odyssey image of western Acidalia, two craters of similar size dramatically display the effects of geologic activity. The younger one on the left has been left relatively well preserved.

A Tale of Two Craters

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