This image captured by NASA's 2001 Mars Odyssey spacecraft shows a small portion of Lobo Vallis near where it recombines with Kasei Valles and empties into Chryse Planitia.
Located on the western margin of Lunae Planum, Sacra Fossae is a group of linear depressions. The right angle turns and uniform width seen in this image from NASA's 2001 Mars Odyssey spacecraft indicate that these channels were formed by faulting.
This image combines two products from the first pointing at the Martian moon Phobos by the THEMIS camera on NASA's Mars Odyssey orbiter, on Sept. 29, 2017. Surface-temperature information from observation in thermal-infrared wavelengths is overlaid on a more detailed image from a visible-light observation.
This image of Phobos is one product of the first pointing at that Martian moon by the THEMIS camera on NASA's Mars Odyssey orbiter. The Sept. 29, 2017, observation also provided information about temperatures on different areas of Phobos. The oblong moon has an average diameter of about 14 miles.
This series of images was taken in visible-wavelength light as the THEMIS camera on NASA's Mars Odyssey scanned across the Martian moon Phobos on Sept. 29, 2017. The apparent motion is due to progression of the camera's pointing during 18 seconds of observing, not from motion of Phobos.
Colors in this image of the Martian moon Phobos indicate a range of surface temperatures detected by observing the moon on Sept. 29, 2017, with the Thermal Emission Imaging System (THEMIS) camera on NASA's Mars Odyssey orbiter.
Re-analysis of 2002-2009 data from a hydrogen-finding instrument on NASA's Mars Odyssey orbiter increased the resolution of maps of hydrogen abundance. The reprocessed data (lower map) shows more "water-equivalent hydrogen" (darker blue) in some parts of this equatorial region of Mars.
Valleys much younger than well-known ancient valley networks on Mars are evident near the informally named "Heart Lake" on Mars. This map presents color-coded topographical information overlaid onto a photo mosaic. Lower elevations are indicated with white and purple; higher elevations, yellow.
At 11:02 a.m. EDT on April 7, 2001, crowds watch a Boeing Delta II rocket lift off from Cape Canaveral Air Force Station, Florida, carrying NASA's 2001 Mars Odyssey spacecraft into space on its seven-month journey to Mars.
Morning clouds fill Coprates Chasma on Mars in this Nov. 25, 2015, image from the THEMIS camera on NASA's Mars Odyssey. No orbiter systematically observed Mars in morning sunlight before 2015. The clouds appear blue because ice particles in them scatter blue light more strongly than other colors.
Buzz Aldrin, an Apollo 11 astronaut who walked on the moon, makes a holographic appearance in 'Destination: Mars,' a mixed-reality tour of a part of Mars that NASA's Curiosity rover has explored.
This map shows unprecedented detail of local variations in Mars' gravitational pull on orbiters. The gravitational mapping has been applied to map variations in the thickness of the planet's crust and to deduce information about its deeper interior.
Newly detailed mapping of local variations in Mars' gravitational pull on orbiters (center), combined with topographical mapping of the planet's mountains and valleys (left), yields the best-yet mapping of Mars' crustal thickness (right).
Women working in science, technology, engineering and mathematics at NASA's Jet Propulsion Laboratory pose for a photo in mission control in honor of Women in Science Day.
This view combines information from two instruments on NASA's Mars Reconnaissance Orbiter to map color-coded composition over the shape of the ground in a small portion of the Nili Fossae plains region of Mars' northern hemisphere.
Researchers estimating the amount of carbon held in the ground at the largest known carbonate-containing deposit on Mars utilized data from three different NASA Mars orbiters.
Researchers estimating the amount of carbon held in the ground at the largest known carbonate-containing deposit on Mars utilized data from three different NASA Mars orbiters.
Gale Crater, home to NASA's Curiosity Mars rover, shows a new face in this image made using data from the THEMIS camera on NASA's Mars Odyssey orbiter.
Seen shortly after local Martian sunrise, clouds gather in the summit pit, or caldera, of Pavonis Mons, a giant volcano on Mars, in this image from the Thermal Emission Imaging System (THEMIS) on NASA's Mars Odyssey orbiter.
This graphic depicts the relative shapes and distances from Mars for five active orbiter missions plus the planet's two natural satellites. It illustrates the potential for intersections of the spacecraft orbits.
This artist's concept shows NASA's Mars orbiters lining up behind the Red Planet for their "duck and cover" maneuver to shield them fro comet dust that may result from the close flyby of comet Siding Spring (C/2013 A1) on Oct. 19, 2014. Credit: NASA/JPL-Caltech
NASA's NEOWISE mission detected comet C/2013 A1 Siding Spring on July 28, 2014, less than three months before this comet's close flyby of Mars on Oct. 19. This merging of multiple images presents the comet in four different positions relative to the background stars.
This map of Mars indicates locations of new craters that have excavated ice (blue) and those that have not (red). The underlying map is based on the brightness, or albedo, of the Martian surface.
This pair of maps indicates locations of confirmed sites of recurrent slope linea on Mars, with respect to elevation (upper map) and surface brightness, or albedo (lower map).
This false-color map shows the area within Gale Crater on Mars, where NASA's Curiosity rover landed on Aug. 5, 2012 PDT (Aug. 6, 2012 EDT) and the location where Curiosity collected its first drilled sample at the "John Klein" rock.
As fractures opened near the summit of Tyrrhena Patera, the ground collapsed to make pits and chains of pits aligned with the fractures. The large pit seen here is about 400 m (1,300 ft) deep.
Fans and ribbons of dark sand dunes creep across the floor of Bunge Crater in response to winds blowing from the direction at the top of the picture. The frame is about 14 kilometers (9 miles) wide.
This mosaic image of Valles Marineris - colored to resemble the martian surface - comes from the Thermal Emission Imaging System (THEMIS), a visible-light and infrared-sensing camera on NASA's Mars Odyssey orbiter.
When the Mars Exploration Rover, Opportunity, landed on Meridiani Planum in January 2004, it quickly found what it had been sent from Earth to find: evidence of liquid water in the Martian past.
On the southwest edge of the immense volcanic region of Tharsis, lava from its giant volcanoes flowed down to meet the old cratered landscape of Terra Sirenum.
The Thermal Emission Imaging System (THEMIS) camera on NASA's Mars Odyssey spacecraft has completed an unprecedented full decade of observing Mars from orbit.
Echus Chasma forms the boundary between the Tharsis volcanoes to the west and Lunae Planum to the east. This region is one of both tectonically fractured rocks (top of image) and volcanic flows (middle and bottom of image). Echus Chasma empties into Kasei Valles.
Just as on Earth, volcanism and tectonism are found together on Mars. Here is an example: the ridges and fractures of Claritas Fossae are affecting or perhaps hosting the volcanic flows of Solis Planum.
A vast dune field lies near the northern polar cap of Mars. Seen here in summer, the dunes have partially buried an impact crater about 1,000 meters (3,300 feet) wide.
Sand dunes shaped like blue-black flames lie next to a central hill within an unnamed, 120-kilometer-wide (75-mile-wide) crater in eastern Arabia on Mars.
In Ares Vallis, teardrop mesas extend like pennants behind impact craters, where the raised rocky rims diverted the floods and protected the ground from erosion.
This image shows a 90-mile-wide portion of the giant Valles Marineris canyon system. Landslide debris and gullies in the canyon walls on Mars can be seen at 100 meters (330 feet) per pixel.
Valles Marineris, the "Grand Canyon of Mars," sprawls wide enough to reach from Los Angeles to nearly New York City, if it were located on Earth. The red outline box shows the location of a second, full-resolution image.
Sixteen seventh-graders at Evergreen Middle School in Cottonwood, Calif., found the Martian pit feature at the center of the superimposed red square in this image while participating in a program that enables students to use the camera on NASA's Mars Odyssey orbiter.
This view of an area about 140 kilometers (about 90 miles) wide in the Meridiani Planum region of Mars shows the region around NASA's Mars Exploration Rover Opportunity.
Stages in the seasonal disappearance of surface ice from the ground around the Phoenix Mars Lander are visible in these images taken on Feb. 8, 2010, (left) and Feb. 25, 2010, during springtime on northern Mars.
NASA's Phoenix Mars Lander, its backshell and its heatshield are 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.
Continuing our survey of non-crater dune fields brings us to this group of dunes in Aonia Terra. The daytime IR illustrates the warmth of the dune material compared to the surrounding materials.
