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Dark spots appear on the south polar ice cap just after the sun starts to shine in this image captured by NASA's Mars Odyssey.
Dark spots appear on the south polar ice cap just after the sun starts to shine in this image captured by NASA's Mars Odyssey.

South Polar Spots

Small unnamed channels drain the surface in this region of Arabia Terra were captured by NASA's Mars Odyssey on August 3, 2010.
Small unnamed channels drain the surface in this region of Arabia Terra were captured by NASA's Mars Odyssey on August 3, 2010.

Arabia Terra

NASA's Phoenix Mars Lander, its backshell and heatshield visible within this enhanced-color image of the Phoenix landing site taken on Jan. 6, 2010 by the High Resolution Imaging Science Experiment (HiRISE) camera on NASA's Mars Reconnaissance Orbiter.
NASA's Phoenix Mars Lander, its backshell and heatshield visible within this enhanced-color image of the Phoenix landing site taken on Jan. 6, 2010 by the High Resolution Imaging Science Experiment (HiRISE) camera on NASA's Mars Reconnaissance Orbiter.

Phoenix Lander Amid Disappearing Spring Ice

This image of the southern flank of Ascraeus Mons, taken by NASA's 2001 Mars Odyssey spacecraft, shows a small sample of collapse features that are common in the area.
This image of the southern flank of Ascraeus Mons, taken by NASA's 2001 Mars Odyssey spacecraft, shows a small sample of collapse features that are common in the area.

Ascraeus Mons

This image, taken by NASA's 2001 Mars Odyssey spacecraft, shows part of the floor of Ganges Chasma. Sand dunes and windstreaks indicate long term wind action in the area.
This image, taken by NASA's 2001 Mars Odyssey spacecraft, shows part of the floor of Ganges Chasma. Sand dunes and windstreaks indicate long term wind action in the area.

Ganges Chasma

This image from NASA's 2001 Mars Odyssey shows a complex region of channels in Tharsis. Called Olympica Fossae, these channel forms were created by lava flows rather than water.
This image from NASA's 2001 Mars Odyssey shows a complex region of channels in Tharsis. Called Olympica Fossae, these channel forms were created by lava flows rather than water.

Olympica Fossae

This image shows the eight sharp tips of the NASA's Phoenix Mars Lander's Atomic Force Microscope, or AFM. The AFM is part of Phoenix's Microscopy, Electrochemistry, and Conductivity Analyzer, or MECA.
This image shows the eight sharp tips of the NASA's Phoenix Mars Lander's Atomic Force Microscope, or AFM. The AFM is part of Phoenix's Microscopy, Electrochemistry, and Conductivity Analyzer, or MECA.

Sharp Tips on the Atomic Force Microscope

This image indicated NASA's Phoenix Mars Lander landing area on Mars to a topographical map indicating relative elevations in the landing region prior to landing. The elevations could have affected wind patterns at the site.
This image indicated NASA's Phoenix Mars Lander landing area on Mars to a topographical map indicating relative elevations in the landing region prior to landing. The elevations could have affected wind patterns at the site.

Wind-Related Topography in Phoenix's Region of Mars (Animation)

This anaglyph, acquired by NASA's Phoenix Lander on Jun. 15, 2008, shows the largest rock informally called 'Midgard.' 3D glasses are necessary to view this image.
This anaglyph, acquired by NASA's Phoenix Lander on Jun. 15, 2008, shows the largest rock informally called 'Midgard.' 3D glasses are necessary to view this image.

Martian Surface as Seen by Phoenix

This view from NASA's Phoenix Mars Lander shows a portion of the trench informally named 'Snow White,' 3D glasses are necessary to view this image.
This view from NASA's Phoenix Mars Lander shows a portion of the trench informally named 'Snow White,' 3D glasses are necessary to view this image.

'Snow White' Trench After Scraping (Stereo View)

This image was acquired by NASA's Phoenix Mars Lander's Surface Stereo Imager (SSI) in the late afternoon of the 30th Martian day of the mission, or Sol 30 (June 25, 2008). This is hours after the beginning of Martian northern summer.
This image was acquired by NASA's Phoenix Mars Lander's Surface Stereo Imager (SSI) in the late afternoon of the 30th Martian day of the mission, or Sol 30 (June 25, 2008). This is hours after the beginning of Martian northern summer.

Happy Mars Solstice!

This false-color polar map was generated from images obtained by the Mars Reconnaissance Orbiter's Mars Color Imager (MARCI). It shows a large local dust storm that researchers were monitoring on May 25, 2008.
This false-color polar map was generated from images obtained by the Mars Reconnaissance Orbiter's Mars Color Imager (MARCI). It shows a large local dust storm that researchers were monitoring on May 25, 2008.

Clear Skies Ahead

This animation shows a hypothetical flyover above Victoria Crater, where NASA's Mars Exploration Rover Opportunity is perched on a rim. The rover is expected to begin rolling down into the crater in early July 2007.
This animation shows a hypothetical flyover above Victoria Crater, where NASA's Mars Exploration Rover Opportunity is perched on a rim. The rover is expected to begin rolling down into the crater in early July 2007.

Surveying the Scene Above Opportunity (Simulation)

This sprawling look at the martian landscape surrounding the Mars Exploration Rover Spirit is the first 3-D stereo image from the rover's navigation camera. 'Sleepy Hollow' can be seen to center left of the image. 3D glasses are necessary.
This sprawling look at the martian landscape surrounding the Mars Exploration Rover Spirit is the first 3-D stereo image from the rover's navigation camera. 'Sleepy Hollow' can be seen to center left of the image. 3D glasses are necessary.

First 3-D Panorama of Spirit's Landing Site

The surface textures observed in this NASA Mars Odyssey image of Ascraeus Mons are due to different volcanic flow types. Textural variations can be produced under a variety of different conditions such as varying cooling and flow rates.
The surface textures observed in this NASA Mars Odyssey image of Ascraeus Mons are due to different volcanic flow types. Textural variations can be produced under a variety of different conditions such as varying cooling and flow rates.

Ascraeus Mons

This image from NASA's Mars Odyssey spacecraft shows grooves within channels of Kasei Valles that can be interpreted as evidence for fluvial activity.
This image from NASA's Mars Odyssey spacecraft shows grooves within channels of Kasei Valles that can be interpreted as evidence for fluvial activity.

Kasei Vallis

This pair of infrared images from NASA's Mars Odyssey spacecraft shows the so-called 'face on Mars' landform viewed during both the day and night.
This pair of infrared images from NASA's Mars Odyssey spacecraft shows the so-called 'face on Mars' landform viewed during both the day and night.

The So-called "Face on Mars" at Night

Except for the loss of its ring of ejecta, the crater at the leading edge of this streamlined island in Kasei Vallis, imaged here by NASA's Mars Odyssey, shows no hint of the catastrophic floods that passed by it.
Except for the loss of its ring of ejecta, the crater at the leading edge of this streamlined island in Kasei Vallis, imaged here by NASA's Mars Odyssey, shows no hint of the catastrophic floods that passed by it.

Kasei Vallis Streamlined Island

Cerberus, seen in this image from NASA's Mars Odyssey spacecraft, is a dark region on Mars that has shrunk down from a continuous length of about 1000 km to roughly three discontinuous spots a few 100 kms in length in less than 20 years.
Cerberus, seen in this image from NASA's Mars Odyssey spacecraft, is a dark region on Mars that has shrunk down from a continuous length of about 1000 km to roughly three discontinuous spots a few 100 kms in length in less than 20 years.

Cerberus Wind Streaks

The focus of this image from NASA's Mars Reconnaissance Orbiter is on the western end of a fan-shaped landform, located at the end point of a sinuous valley.
The focus of this image from NASA's Mars Reconnaissance Orbiter is on the western end of a fan-shaped landform, located at the end point of a sinuous valley.

A Fan-Shaped Landform and Nearby Light-Toned Material

Gully and defrosting activity have been visible here along the edge of a dune field, along with blocks of frost. Observations from NASA's Mars Reconnaissance Orbiter of the same area help check for repeat activity.
Gully and defrosting activity have been visible here along the edge of a dune field, along with blocks of frost. Observations from NASA's Mars Reconnaissance Orbiter of the same area help check for repeat activity.

Active High-Latitude Dune-Gullies

Melas Chasma is part of the Valles Marineris canyon system, the largest canyon in the Solar System. This image was taken by NASA's Mars Reconnaissance Orbiter.
Melas Chasma is part of the Valles Marineris canyon system, the largest canyon in the Solar System. This image was taken by NASA's Mars Reconnaissance Orbiter.

Finding Faults in Melas Chasma

This image shows numerous dark shapes and bright spots on a sand dune in the Northern polar regions of Mars. This observation is from NASA's Mars Reconnaissance Orbiter.
This image shows numerous dark shapes and bright spots on a sand dune in the Northern polar regions of Mars. This observation is from NASA's Mars Reconnaissance Orbiter.

Giant Gullies North of the Argyre Impact Basin

This image shows numerous dark shapes and bright spots on a sand dune in the Northern polar regions of Mars. This observation is from NASA's Mars Reconnaissance Orbiter.
This image shows numerous dark shapes and bright spots on a sand dune in the Northern polar regions of Mars. This observation is from NASA's Mars Reconnaissance Orbiter.

Shapes and Spots on a Polar Sand Dune

The formation of 'recurring slope lineae' is a fascinating process on Mars. These RSLs show up in the spring and fade in the winter as seen by NASA's Mars Reconnaissance Orbiter.
The formation of 'recurring slope lineae' is a fascinating process on Mars. These RSLs show up in the spring and fade in the winter as seen by NASA's Mars Reconnaissance Orbiter.

Slope Lineae along Coprates Chasma Ridge

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