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Tectonics played the major role in shaping the surface of this image captured by NASA's 2001 Mars Odyssey spacecraft. This image contains arcuate fractures and isolated depressions containing chaos.
Tectonics played the major role in shaping the surface of this image captured by NASA's 2001 Mars Odyssey spacecraft. This image contains arcuate fractures and isolated depressions containing chaos.

Tectonics

This image captured by NASA's 2001 Mars Odyssey spacecraft shows part of the southern flank of Pavonis Mons. Visible at the bottom of the image are collapse features and lava channels.
This image captured by NASA's 2001 Mars Odyssey spacecraft shows part of the southern flank of Pavonis Mons. Visible at the bottom of the image are collapse features and lava channels.

Pavonis Mons

This image captured by NASA's 2001 Mars Odyssey spacecraft shows the rough terrain just inside the eastern rim of Gale Crater as well as the eastern extent of Mr. Sharp.
This image captured by NASA's 2001 Mars Odyssey spacecraft shows the rough terrain just inside the eastern rim of Gale Crater as well as the eastern extent of Mr. Sharp.

Images of Gale #8

The small dune forms seen in this image by NASA's 2001 Mars Odyssey spacecraft are located on the floor of Briault Crater.
The small dune forms seen in this image by NASA's 2001 Mars Odyssey spacecraft are located on the floor of Briault Crater.

Dunes in Briault Crater

Eridania Basin, located at the head of Ma'adim Vallis, has mounting geomorphic and spectral evidence that it may have been the site of an ancient inland sea. This image is from NASA's Mars Reconnaissance Orbiter.
Eridania Basin, located at the head of Ma'adim Vallis, has mounting geomorphic and spectral evidence that it may have been the site of an ancient inland sea. This image is from NASA's Mars Reconnaissance Orbiter.

Ridges in Eridania Basin

In an area like Russell Crater, very ancient impact crater, NASA's Mars Reconnaissance Orbiter can follow changes in the terrain by comparing images taken at different times. Frost (carbon dioxide ice) is seen in this image.
In an area like Russell Crater, very ancient impact crater, NASA's Mars Reconnaissance Orbiter can follow changes in the terrain by comparing images taken at different times. Frost (carbon dioxide ice) is seen in this image.

Fall Frost Accumulation on Russell Crater Dunes

This image captured by NASA's 2001 Mars Odyssey spacecraft shows another portion of the large dune field near the north polar cap.
This image captured by NASA's 2001 Mars Odyssey spacecraft shows another portion of the large dune field near the north polar cap.

Polar Dunes

This observation from NASA's Mars Reconnaissance Orbiter shows an excellent example of what is called 'fretted terrain,' termed so because of the eroded appearance of the surface.
This observation from NASA's Mars Reconnaissance Orbiter shows an excellent example of what is called 'fretted terrain,' termed so because of the eroded appearance of the surface.

Fretted Terrains and Ground Deformation

Polar surface winds can reach high velocities. These winds can cause clouds to form when the winds flow into troughs and become chaotic. This image from NASA's Mars Odyssey shows trough clouds as linear bands.
Polar surface winds can reach high velocities. These winds can cause clouds to form when the winds flow into troughs and become chaotic. This image from NASA's Mars Odyssey shows trough clouds as linear bands.

South Polar Clouds

Arsia Chasmata is a complex collapsed region at the northeastern flank of Arsia Mons. The collapsed region aligns with the Pavonis and Ascraeus Mons volcanoes, indicating that all three volcanoes are located on a major fracture in the Tharsis region.
Arsia Chasmata is a complex collapsed region at the northeastern flank of Arsia Mons. The collapsed region aligns with the Pavonis and Ascraeus Mons volcanoes, indicating that all three volcanoes are located on a major fracture in the Tharsis region.

Arsia Chasmata

This image, taken by NASA's 2001 Mars Odyssey spacecraft, shows the western wall of Uzboi Vallis near the intersection of the vallis and Holden Crater. Many channels dissect the wall of the channel.
This image, taken by NASA's 2001 Mars Odyssey spacecraft, shows the western wall of Uzboi Vallis near the intersection of the vallis and Holden Crater. Many channels dissect the wall of the channel.

Uzboi Vallis

This color image was acquired by the Surface Stereo Imager on NASA's Phoenix Mars Lander on the 21st day of the mission, or Sol 20 (June 15, 2008). It shows lumps of ice in the lower left corner of a trench nicknamed 'Dodo-Goldilocks.'
This color image was acquired by the Surface Stereo Imager on NASA's Phoenix Mars Lander on the 21st day of the mission, or Sol 20 (June 15, 2008). It shows lumps of ice in the lower left corner of a trench nicknamed 'Dodo-Goldilocks.'

Ice on Mars - Now You See It

A football-field-size crater, informally named
A football-field-size crater, informally named

'Santa Maria' Crater in 360-Degree View, Sol 2451 (Polar)

This diagram illustrates how the Dynamic Albedo of Neutrons (DAN) instrument on NASA's Curiosity Mars rover detects hydrogen in the ground beneath the rover.
This diagram illustrates how the Dynamic Albedo of Neutrons (DAN) instrument on NASA's Curiosity Mars rover detects hydrogen in the ground beneath the rover.

Physics of How DAN on Curiosity Checks for Water, Part 1

This image captured by NASA's 2001 Mars Odyssey spacecraft shows the western flank of Elysium Mons.
This image captured by NASA's 2001 Mars Odyssey spacecraft shows the western flank of Elysium Mons.

Elysium Mons

Do you see what I see in this image from NASA's Mars Odyssey spacecraft? The ejecta surrounding the small craters near the bottom of this image look like interlocking gears.
Do you see what I see in this image from NASA's Mars Odyssey spacecraft? The ejecta surrounding the small craters near the bottom of this image look like interlocking gears.

THEMIS Art #105

Channels dissect the hillside of Terra Sirenum in this image from NASA's 2001 Mars Odyssey spacecraft.
Channels dissect the hillside of Terra Sirenum in this image from NASA's 2001 Mars Odyssey spacecraft.

Channels

NASA's Mars Exploration Rover Opportunity studied layers in the Burns Cliff slope of Endurance Crater in 2004. The layers show different types of deposition of sulfate-rich sediments. Opportunity's panoramic camera recorded this image.
NASA's Mars Exploration Rover Opportunity studied layers in the Burns Cliff slope of Endurance Crater in 2004. The layers show different types of deposition of sulfate-rich sediments. Opportunity's panoramic camera recorded this image.

Layers in Burns Cliff Examined by Opportunity

This unnamed channel drains the highland region near Pulawy Crater as seen by NASA's 2001 Mars Odyssey spacecraft.
This unnamed channel drains the highland region near Pulawy Crater as seen by NASA's 2001 Mars Odyssey spacecraft.

Channel near Pulawy Crater

Chaos and small channels mark the boundary between the highlands of Terra Sabaea and the lowlands of Utopia Planitia in this image captured by NASA's Mars Odyssey.
Chaos and small channels mark the boundary between the highlands of Terra Sabaea and the lowlands of Utopia Planitia in this image captured by NASA's Mars Odyssey.

Highland Margin

This Gale image from NASA's Mars Odyssey spacecraft shows the region just slightly south of yesterday's image. The dark region on the crater floor is sand. The dunes that encircle Mt. Sharp are most likely comprised of sand eroded from Mt. Sharp itself.
This Gale image from NASA's Mars Odyssey spacecraft shows the region just slightly south of yesterday's image. The dark region on the crater floor is sand. The dunes that encircle Mt. Sharp are most likely comprised of sand eroded from Mt. Sharp itself.

Images of Gale #11

This image from NASA's Mars Odyssey shows Bahram Vallis where it enters Waspam Crater. Bahram Vallis exits the crater to the north a short distance from this location along the rim of Waspam Crater.
This image from NASA's Mars Odyssey shows Bahram Vallis where it enters Waspam Crater. Bahram Vallis exits the crater to the north a short distance from this location along the rim of Waspam Crater.

Bahram Vallis

The dark lines in this image from NASA's Mars Odyssey are the tracks of dust devils in this region of Arcadia Plainitia. As the swirling winds move along the surface, they remove the dust cover, revealing the darker rock beneath.
The dark lines in this image from NASA's Mars Odyssey are the tracks of dust devils in this region of Arcadia Plainitia. As the swirling winds move along the surface, they remove the dust cover, revealing the darker rock beneath.

Dust Devil Tracks

This image captured by NASA's 2001 Mars Odyssey spacecraft shows more north polar dunes.
This image captured by NASA's 2001 Mars Odyssey spacecraft shows more north polar dunes.

More Polar Dunes

A sand sheet with surface dune forms covers part of the floor of this unnamed crater, as shown in this image from NASA's 2001 Mars Odyssey spacecraft. This crater is located in Acidalia Planitia.
A sand sheet with surface dune forms covers part of the floor of this unnamed crater, as shown in this image from NASA's 2001 Mars Odyssey spacecraft. This crater is located in Acidalia Planitia.

Crater Dunes

Currently displaying images 2076-2100 of 2623
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