Mars Surface Imaging

NASA's Mars Odyssey spacecraft captures detailed images of Martian terrain, showcasing rugged landscapes and geological features.

Candor Chasma's Rim
Candor Chasma's Rim
306 assets in this story
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This image from NASA's Mars Odyssey shows a portion of Aureum Chaos located just south of the Martian equator. This fractured landscape contains canyons and mesas with two large impact craters in the upper left.
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The floor of Melsa Chasma contains a variety of landforms. This image from NASA's 2001 Mars Odyssey shows deposits of fine materials as well as layered deposits.
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This region of Alba Patera is characterized by faulting with the down-dropped block on the southeast side of the fault
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This narrow canyon is part of Coprates Chasma. On the east side of the canyon a landslide is visible. The southern wall of the canyon is marked by bright and dark streaks where dust has slid down the cliff face
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This image captured by NASA's 2001 Mars Odyssey spacecraft shows sand dunes on the floor of an unnamed crater in Noachis Terra.
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This image from NASA's 2001 Mars Odyssey spacecraf shows part of Aspledon Undae, one of several dune fields near the north pole. The term Undae means dunes.
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The fractures in this image are part of a large system of fractures called Cerberus Fossae. Athabasca Valles is visible in the lower right corner of the image as seen by NASA's 2001 Mars Odyssey spacecraft.
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This image shows a small portion of the flank of Ascraeus Mons
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Uranius Fossae is region of multi directional graben. Graben are tectonic features created by extension, where blocks of material move downward between paired faults. This region of graben is located east of Uranius Mons. Orbit Number 78842 Latitude 23.1816 Longitude 269.606 Instrument VIS Captured 2019-09-23 04 08
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In this part of the Tharsis region, old lava flows have been fractured. Younger lava flows are unfractured (flow at bottom)
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This image from NASA's 2001 Mars Odyssey spacecraft shows an unnamed channel draining from the highlands of Promethei Terra to lowlands of the Hellas Basin.
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Pavonis Mons Flank. This VIS image shows a portion of the northern flank of Pavonis Mons. The linear features at the top of the image are concentric faults. The linear and sinuous channel-like features at the bottom of the image likely formed by collapse of the roof of lava tubes into the empty space beneath. Pavonis Mons is the central volcano of the three large Tharsis volcanoes. In order from north to south the volcanoes are Ascreaus Mons, Pavonis Mons and Arsia Mons. All three volcanoes form a line located along a tectonic bulge caused by extensional forces in the region. Along this trend there are increased tectonic features and additional lava flows that arose from the flanks of the volcanoes rather than just the summit. Like the other large volcanoes in the region, Pavonis Mons is a shield volcano. Shield volcanoes are formed by lava flows originating near or at the summit, building up layers upon layers of lava. In shield volcanoes summit calderas are typically formed where the
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This NASA Mars Odyssey image of rounded hills and ridges in Arcadia Planitia shows a very intriguing geomorphic feature that may be attributed to the presence of an icy-rock mixture of material.
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The dunes in this VIS image are located on the floor of an unnamed crater in Noachis Terra as seen by NASA's 2001 Mars Odyssey spacecraft.
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The lava flows and depressions in this image from NASA's 2001 Mars Odyssey spacecraft are located south of Alba Mons.
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This image from NASA's 2001 Mars Odyssey spacecraft was collected at the same time as yesterday's IR image. The dunes are dark in the VIS image, because the material is darker in color than the surrounding material.
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Today's VIS image shows part of Ariadnes Colles. The term colles means hills or knobs. The hills appear brighter than the surrounding lowlands, likely due to relatively less dust cover. Ariadnes Colles is located in Terra Cimmeria. Orbit Number 81566 Latitude -34.7232 Longitude 171.559 Instrument VIS Captured 2020-05-04 10 53
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NASA's Mars Reconnaissance Orbiter shows densely fractured light-toned rock in the vicinity of the Nili Fossae. The light-toned material is finely layered; these layers can be seen in cross-section along a scarp face at the bottom of the image.
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The dark surface markings of Utopia Planitia are thought to be caused by dust devils as seen by NASA's 2001 Mars Odyssey spacecraft.
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Olympica Fossae is a complex channel located on the volcanic plains between Alba Mons and Olympus Mons. The sinuosity of the large channel in the middle of the image indicates that this is a channel created by liquid flow. In this case the location and other surface features point to lava rather than water as the liquid. The more linear depressions at the bottom third of the image are possibly tectonic features called graben and formed by movement along fault lines. The Alba Mons region contains extensive faulting which formed due to collapse of the volcano. Orbit Number 71183 Latitude 25.8417 Longitude 247.895 Instrument VIS Captured 2017-12-31 08 32
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Proposed MSL Site in Nilo Syrtis
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Sand Dunes in Rabe Crater
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Today's VIS image shows part of the floor of an unnamed crater in Margaritifer Terra. The crater floor is dissected by linear features, most likely faults. There is an offset of the large depression in the center of the image, where the linear feature has been pulled sideways along a perpendicular fault. With time and erosion this region of fault blocks will become chaos terrain. Orbit Number 81735 Latitude -18.403 Longitude 333.725 Instrument VIS Captured 2020-05-18 08 56
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Oti Fossae are paired fractures with a downdropped block called graben located on the eastern flank of Arsia Mons as seen by NASA's 2001 Mars Odyssey spacecraft.
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Craters, Pit Chains, and Graben, Oh My!
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Today's VIS image shows part of eastern Candor Chasma. Candor Chasma is one of the largest canyons that make up Valles Marineris. It is approximately 810 km long (503 miles) and has is divided into two regions - eastern and western Candor. Candor is located south of Ophir Chasma and north of Melas Chasma. The border with Melas Chasma contains many large landslide deposits. The floor of Candor Chasma includes a variety of landforms, including layered deposits, dunes, landslide deposits and steep sided cliffs and mesas. Many forms of erosion have shaped Candor Chasma. There is evidence of wind and water erosion, as well as significant gravity driven mass wasting (landslides). Orbit Number 88163 Latitude -7.04697 Longitude 292.058 Instrument VIS Captured 2021-10-29 15 27
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This image from NASA's Mars Reconnaissance Orbiter shows a graben (a trough formed when the ground drops between two parallel faults) and a lava flow in the Tharsis volcanic province of Mars. North is up.
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The landslide in the center of this image from NASA's 2001 Mars Odyssey spacecraft occurred in the Melas Chasma region of Valles Marineris.
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Dunes in Herschel Crater
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This image shows part of the southern flank of Pavonis Mons. The linear and sinuous features mark the locations of lava tubes and graben that occur on both sides of the volcano along a regional trend that passes thru Pavonis Mons, Ascreaus Mons (to the north), and Arsia Mons (to the south). The majority of the features are believed to be lava tubes where the ceiling has collapsed into the free space below. This often happens starting in a circular pit and then expanding along length of the tube until the entire ceiling of material has collapsed into the bottom of the tube. Pavonis Mons is one of the three aligned Tharsis Volcanoes. The four Tharsis volcanoes are Ascreaus Mons, Pavonis Mons, Arsia Mons, and Olympus Mars. All four are shield type volcanoes. Shield volcanoes are formed by lava flows originating near or at the summit, building up layers upon layers of lava. The Hawaiian islands on Earth are shield volcanoes. The three aligned volcanoes are located along a topographic rise
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The finely layered deposit in Becquerel crater, seen in the center of this NASA Mars Odyssey image, is slowly being eroded away by the action of windblown sand.
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The north/south trending parallel hills and valleys in this image captured by NASA's 2001 Mars Odyssey spacecraft were created by wind erosion and are called yardangs. These yardangs are located in Zephyria Planum.
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Marte Vallis, located in Amazonis Planitia, broad and shallow, is illustrated by the streamlined islands at the top and bottom of this image from NASA's 2001 Mars Odyssey spacecraft.
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Mensa in Kasei Vallis
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This image from NASA's Mars Odyssey of lava flows around the large scarp of Olympus Mons reveals textures characteristic of the variable surface roughness associated with different lava flows in this region.
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These windstreaks are located in northern Terra Tyrrhena. The wind was blowing from NE to SW to create the streaks in the lee of the craters. This image is from NASA's Mars Odyssey.
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This NASA Mars Odyssey image shows a remarkable array of dunes on the floor of a large impact crater named Baldet. Many of the dunes in this region are isolated features with large, sand-free 'interdune' surfaces between the individual dunes.
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This image captured by NASA's 2001 Mars Odyssey spacecraft show the dark marks left behind after the passage of a dust devil cover this region of Utopia Planitia.
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This image of Tharsis Rise from NASA's Mars Odyssey shows a series of linear features called graben, which are associated with crustal extension resulting in up and down blocks of crust that run perpendicular to the direction of the extension.
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. Ceraunius Fossae. This VIS image shows part of Cerunius Fossae. The linear depressions are fault bounded features called graben. Graben are formed by extension of the crust and faulting. When large amounts of pressure or tension are applied to rocks on timescales that are fast enough that the rock cannot respond by deforming, the rock breaks along faults. In the case of a graben, two parallel faults are formed by extension of the crust and the rock in between the faults drops downward into the space created by the extension. The largest graben in this THEMIS image trends from almost north/south. Because the faults defining the graben are formed perpendicular to the direction of the applied stress, we know that extensional forces were pulling the crust apart in the east/west direction. Ceraunius Fossae is located on the southern part of Alba Mons and is 1166km (724 miles) long. Orbit Number 94210 Latitude 32.086 Longitude 247.58 Instrument VIS Captured 2023-03-11 14 09
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This image shows a portion of Utopia Planitia that is covered by dust devil tracks as seen by NASA's 2001 Mars Odyssey spacecraft.
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These windstreaks occur on top of lava flows from Arsia Mons
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Are Ripples a Sign of Water
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Elysium Fossae. Today's VIS image contains a section of one of the many channel forms found radial to the Elysium Mons volcanic complex. In this case the fossae are located to the west of Elysium Mons. Elysium Fossae are comprised of both linear and sinuous channels, usually interpreted to have both fluid and tectonic forces playing a part in the formation. The linear depression resembles a graben (formed by tectonic forces) and sinuous channels more closely resembles features caused by fluid flow - either lava or water created by melting subsurface ice due to volcanic heating. Orbit Number 93771 Latitude 25.4228 Longitude 138.846 Instrument VIS Captured 2023-02-03 09 57 https //photojournal.jpl.nasa.gov/catalog/PIA25876
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Olympus Mons Lava Flows
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Today's VIS image shows part of the eastern side of Maunder Crater. This crater has a unique form, with a large amount of fill on the eastern half of the crater floor, and a valley between the crater rim and the crater fill. It is possible that a large landslide may have occurred in this region of the crater. In this image, multiple gullies are located on the west-facing side of the valley. Maunder Crater is located in Noachis Terra. Orbit Number 74622 Latitude -49.4561 Longitude 2.582 Instrument VIS Captured 2018-10-10 15 07
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Echus Chasma Mega-gully. This VIS image shows one of the mega-gullies that empties into Echus Chasma. Echus Chasma is approximately 4km deep in this region, and is the source of Kasei Valles. Orbit Number 91021 Latitude 0.839415 Longitude 278.09 Instrument VIS Captured 2022-06-21 23 25
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Gorgonum Chaos. This VIS image shows part of Gorgonum Chaos. Chaos terrain is typified by regions of blocky, often steep sided, mesas interspersed with deep valleys. With time and erosion the valleys widen and the mesas become smaller. Chaotic regions form when groundwater escapes to the surface, undermining it and causing the ground to collapse. The linear depressions at the bottom of the image are part of Sirenum Fossae. Gorgonum Chaos is located in Terra Sirenum. Orbit Number 92266 Latitude -36.8519 Longitude 189.676 Instrument VIS Captured 2022-10-02 10 57 https //photojournal.jpl.nasa.gov/catalog/PIA25754
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Layered Deposits in Ritchey Crater
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Aram Chaos is a complex region which contains layered material with different surface textures and heavily fractured material forming chaos
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Today's VIS image shows a section of Cerberus Fossae. Cerberus Fossae are located in Elysium Planitia, southeast of the Elysium Mons volcanic complex. The linear features in the image are tectonic graben. Graben are formed by extension of the crust and faulting. When large amounts of pressure or tension are applied to rocks on timescales that are fast enough that the rock cannot respond by deforming, the rock breaks along faults. In the case of a graben, two parallel faults are formed by extension of the crust and the rock in between the faults drops downward into the space created by the extension. Numerous sets of graben are visible in this THEMIS image, trending from north-northwest to south-southeast. Because the faults defining the graben are formed perpendicular to the direction of the applied stress, we know that extensional forces were pulling the crust apart in the east-northeast/west-southwest direction. The Cerberus Fossae graben are sources of both channels and significant
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Holden Crater Dune Field
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Windstreaks. Today's VIS image shows windstreaks located in Syrtis Major Planum. These streaks are formed by the wind interaction with positive topographic features (like craters), with the 'tail' located down wind of the crater. The streaks in this image indicate the prevailing wind was from the upper right to the lower left side of the image (northeast to southwest). Orbit Number 94023 Latitude 6.9785 Longitude 71.5019 Instrument VIS Captured 2023-02-24 03 50 https //photojournal.jpl.nasa.gov/catalog/PIA25942
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Elysium Fossae. Today's VIS image contains a section of one of the many channel forms found radial to the Elysium Mons volcanic complex. In this case the fossae are located to the west of Elysium Mons. Elysium Fossae are comprised of both linear and sinuous channels, usually interpreted to have both fluid and tectonic forces playing a part in the formation. The linear depression resembles a graben (formed by tectonic forces) and sinuous channels more closely resembles features caused by fluid flow - either lava or water created by melting subsurface ice due to volcanic heating. The Elysium Fossae system is 1044 km (649 miles) in length. Orbit Number 93983 Latitude 27.1871 Longitude 142.629 Instrument VIS Captured 2023-02-20 20 54 https //photojournal.jpl.nasa.gov/catalog/PIA25941
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This VIS image shows part of the extensive dune field on the floor of Proctor Crater. Proctor Crater is located in Noachis Terra. Orbit Number 74883 Latitude -47.6285 Longitude 30.2768 Instrument VIS Captured 2018-11-01 03 03
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This image shows part of the dune field located on the floor of Proctor Crater as seen by NASA's 2001 Mars Odyssey spacecraft.
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This VIS image shows the part of the crater rim and ejecta surrounding Lonar Crater in the northern plains of Vastitas Borealis. There is a fine scale, radial grooved outer layer of ejecta covered by lobate ejecta nearer the crater rim. The ends of the lobes are taller than the material just inside the end of the lobe. Often called rampart ejecta, this morphology can be caused by impact into a surface that includes volatiles such as sub-surface water or ice. Orbit Number 71327 Latitude 73.428 Longitude 38.7539 Instrument VIS Captured 2018-01-12 05 31
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Today's image shows the eastern portion of the complex caldera at the summit of Olympus Mon as seen by NASA's 2001 Mars Odyssey spacecraft.
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Walls of Noctus Labyrinthus
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Alluvial Fans in Mojave Crater: Did It Rain on Mars
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This image captured by NASA's 2001 Mars Odyssey spacecraft shows some of the extensive wind etched terrain in Memnonia Sulci, located south west of Olympus Mons.
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Today's VIS image shows part of the wind eroded Amazonis Mensa. Just one of several large linear mounds of material, Amazonis Mensa has been carved by long term surface winds. The linear grooves are aligned with the prevailing winds. The mensa has to be formed of soft, relatively uncemented materials to be eroded so easily. It has been suggested that the surface material may be volcanic ash from nearby volcanoes. Orbit Number 79493 Latitude 1.56883 Longitude 210.942 Instrument VIS Captured 2019-11-15 18 32
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Olympica Fossae is a complex channel located on the Tharsis volcanic plains between Alba Mons and Olympus Mons. The sinuosity of the large channel in the top half of the image indicates that this is a channel created by liquid flow. In this case the location and other surface features visible in the image indicate that lava flow rather than water created the channel. The more linear depression at the bottom left side of the image is probably a tectonic feature called a graben and was formed by movement along fault lines. Orbit Number 78693 Latitude 25.836 Longitude 248.007 Instrument VIS Captured 2019-09-10 21 41
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This image captured by NASA's 2001 Mars Odyssey spacecraft shows a sand sheet with surface dune forms located on the floor of an unnamed crater in Vastitas Borealis.
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Today's VIS image shows a complex crater located in Terra Cimmeria, just north of Hesperia Planum. The floor of this unnamed crater has features indicating a substantial amount of crater fill material was deposited at some point after the formation of the crater. These materials have since been eroded into multiple different forms. There are valley and mesa forms in the bottom part of the crater in this image, with the valleys becoming more shallow and channel-like toward the northern part of the crater floor. It is thought that the formation of the valley and mesa formation (called chaos terrain) arises from the release of subsurface fluids. Orbit Number 90328 Latitude -8.81454 Longitude 112.309 Instrument VIS Captured 2022-04-25 21 52
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Hebrus Valles is located in the Elysium Planitia region of the northern lowlands of Mars. This image from NASA's Mars Odyssey spacecraft shows three sinuous tributaries of the channel system which carved up the surrounding plains.
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This VIS image shows part of the floor of Ganges Chasma. Deposits of fine surface materials and bright layered deposits are visible in this image. Ganges Chasma is part of the Valles Marineris chasma system, but is north of the main section of canyons. Orbit Number 82734 Latitude -7.8794 Longitude 311.753 Instrument VIS Captured 2020-08-08 15 10
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Landslides
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In this section of Tinto Vallis there are no tributary stream channels joining the main channel. This tells us that whatever carved the channel originated in some other region
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This image captured by NASA's 2001 Mars Odyssey spacecraft shows depressions near the south polar cap. All surface ice in this region has been removed by the relative warmth of summer, revealing subtle features of the surface.
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The linear depressions in this image from NASA's 2001 Mars Odyssey spacecraft are graben. Graben are formed from tectonic activity with large blocks of material moving downward between paired faults.
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This image from NASA's Mars Odyssey shows a portion of a large landslide deposit in Ius Chasma.
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This image captured by NASA's 2001 Mars Odyssey spacecraft shows part of the caldera at the summit of Arsia Mons.
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Channel by Day and Night
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Holden Crater Layers
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This VIS image shows part of the western flank of Pavonis Mons. Pavonis Mons is the central volcano of the three large Tharsis volcanoes. All three volcanoes form a line located along a tectonic bulge caused by extensional forces in the region. Pavonis Mons is the smallest of the three with a summit of only 14km (46,000 ft). The linear features at the top of the image are concentric faults. The linear and sinuous channel-like features at the bottom of the image likely formed by collapse of the roof of lava tubes into the empty space beneath. Pavonis means peacock in Latin, making the name peacock mountain. Orbit Number 89637 Latitude 0.453403 Longitude 246.269 Instrument VIS Captured 2022-02-28 00 23
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NASA's Mars Odyssey captured this image of Ulysses Fossae, located in the Tharsis Volcanic region. Cross cutting tectonic fractures indicate that this region underwent stresses in multiple directions.
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The north-south trending fractures and graben (block down-dropped between two fractures) in this region are called Ceraunius Fossae and are likely related to Alba Mons to the north shown in this image from NASA's 2001 Mars Odyssey spacecraft.
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Located in the center of this VIS image is a group of sand dunes. With enough wind and sand, sand dunes are formed. Dune morphology typically has a shallow slope on the side the wind is blowing from and a steep face on the other side. The darker part of the dunes in this image are the steep slopes. Wind blows sand particles up the shallow slope and then the particles 'fall' off the crest of the dune down the steep side. With time, the constant wind will move the crest of the dune forward. Depending on the amount of available sand, dunes can grow to large heights and sizes. In the case of this image, the dunes are moving toward the top of the image, which means up the surface slope. In cases like this, the dunes 'climb' up hills. Orbit Number 74955 Latitude -50.2322 Longitude 292.058 Instrument VIS Captured 2018-11-07 00 56
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The THEMIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. This image from NASA's 2001 Mars Odyssey spacecraft shows a part of the large sand sheet on the floor of Proctor Crater.
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The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. This image from NASA's 2001 Mars Odyssey spacecraft shows a crater within a crater on the floor of Hadley Crater.
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Salty Trench
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This VIS image shows part of Ceraunius Fossae. The linear depressions are fault bounded features called graben. Graben form from tectonic forces that are pulling apart the surface, created space for material to slide down along the fault. Alba Mons is surrounded by extensive regions of closely spaced graben. Ceraunius Fossae is located south of Alba Mons. Orbit Number 78406 Latitude 27.7831 Longitude 248.084 Instrument VIS Captured 2019-08-18 06 29
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Mars Orbiter Camera Views the Face
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This VIS image runs from northern Juventae Chasma to just short of the southern canyon wall. Illustrating the variety of landforms within the chasma, this image contains the rough canyon floor at the northern extent of the chasma, layered materials in the center of the image and dunes located in the southern, deepest section of the chasma. Orbit Number 71356 Latitude -3.55335 Longitude 298.389 Instrument VIS Captured 2018-01-14 14 25
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In planetary nomenclature, the descriptor term chaos means distinctive area of broken terrain . The general morphology of chaos is steep-sided mesas in close proximity. This VIS image shows a region of Chryse Chaos where the isolated mesas are beginning to be formed. The interconnected channel forms erode, and mesas are created by erosion of the bounding channels. The bottom of the image shows some of the resultant mesas. Orbit Number 71455 Latitude 13.1491 Longitude 318.592 Instrument VIS Captured 2018-01-22 18 16
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Channels dissect the northern rim of this unnamed crater in Terra Cimmeria.
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Meanders in Nanedi Valles
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Alba Fossae. Alba Fossae is a set of long valleys on the western side of Alba Mons. These valleys are referred to as graben and are formed by extension of the crust and faulting. When large amounts of pressure or tension are applied to rocks on timescales that are fast enough that the rock cannot respond by deforming, the rock breaks along faults. In the case of a graben, two parallel faults are formed by extension of the crust and the rock in between the faults drops downward into the space created by the extension. Numerous sets of graben are visible in this THEMIS image, trending from north-northeast to south-southwest. Because the faults defining the graben are formed perpendicular to the direction of the applied stress, we know that extensional forces were pulling the crust apart in the west-northwest/east-southeast direction. The large number of graben around Alba Mons is generally believed to be the result of extensional forces associated with the uplift of Alba Mons. Orbit Numb
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Microscopic photography of a fragment of wood from the Wierzbięty Epitaph from Branice (II) unknown
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This image captured by NASA's 2001 Mars Odyssey spacecraft looks like a slithering snake on Mars. Orbit Number 61495 Latitude 32.0515 Longitude 152.236 Instrument VIS Captured 2015-10-25 06 21
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. Olympus Mons. Today's VIS image shows part of the lower flank of Olympus Mons. The bright band in the image is an escarpment, where there is a large elevation change over a very short linear range - a cliff. This escarpment is called Olympus Rupes. In 2-D images it is very difficult to interpret the height component. In this case, the elevation change from the highest point (bottom of image) to the lowest point (top of image) is 7757m (25,449 feet). Olympus Mons is 21.9km (13.6 miles, 72,000 feet) tall. For comparison, Mt Everest is only 29,032 feet tall. Orbit Number 94579 Latitude 22.7256 Longitude 229.336 Instrument VIS Captured 2023-04-10 22 38
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Today's VIS image is located on the upper flank of Olympus Mons. Olympus Mons is the largest volcano in the solar system, standing 14 miles high above the surrounding volcanic plains. Orbit Number 77209 Latitude 17.991 Longitude 225.786 Instrument VIS Captured 2019-05-11 16 44
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This image captured by NASA's 2001 Mars Odyssey spacecraft shows part of Boreum Cavus, at the interior end of Chasma Boreale.
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Today's VIS image shows a small section of Shalbatana Vallis. Located in Xanthe Terra, Shalbatana Vallis is an outflow channel carved by massive floods of escaping groundwater whose source lies far to the south of this image. This channel, and all others in this region, drain into Chryse Planitia. Shalbatana Vallis is 1029km long (639 miles). Orbit Number 95150 Latitude 10.3961 Longitude 318.227 Instrument VIS Captured 2023-05-27 22 56
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Pit Craters of Tractus Catena
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Today's VIS image shows a section of Scamander Vallis. Scamander Vallis is located in northern Terra Sabaea. Orbit Number 77403 Latitude 15.79 Longitude 28.6431 Instrument VIS Captured 2019-05-27 16 08
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This image from NASA's 2001 Mars Odyssey spacecraft is of the south pole and shows a surface with numerous oval depressions. This texture has been described as looking like swiss cheese.
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This side-perspective view of Ceres' mysterious mountain Ahuna Mons was made with images from NASA's Dawn spacecraft. Dawn took these images in December 2015.
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Martian Kanji