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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Today's VIS image shows a small section of Nirgal Valles. Located in Noachis Terra, Nirgal Valles is 610km long (379 miles). Orbit Number 83308 Latitude -27.164 Longitude 315.114 Instrument VIS Captured 2020-09-24 21 22
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The pristine nature of this crater and its ejecta indicate that it is younger than the outflow channel where it is located. This image is from NASA's 2001 Mars Odyssey.
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. Cerberus Fossae. 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 channe
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This image from NASA's 2001 Mars Odyssey spacecraft of the Tharsis region illustrates relative age relations. Fractures occurred in old lava flows and then younger lava flows covered the fractures.
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This VIS image captured by NASA's 2001 Mars Odyssey spacecraft of Iani Chaos shows the layered deposit that occurs on the floor. It appears that the layers were deposited after the chaos was formed.
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Mangala Fossae. Mangala Fossae is a long linear depression called a graben and was 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. At the right side of the image the graben enters an impact crater, and creates a complex group of tectonic fractures and depressions. Mangala Fossae is 828 km long (514 miles). Orbit Number 91061 Latitude -19.2481 Longitude 206.825 Instrument VIS Captured 2022-06-25 06 21
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This image shows part of the Nili Patera dune field. High resolution imaging by other spacecraft has revealed that the dunes in this region are moving. Winds are blowing the dunes across a rough surface of regional volcanic lava flows. The paterae are calderas on the volcanic complex called Syrtis Major Planum. Dunes are found in both Nili and Meroe Paterae and in the region between the two calderas. The Odyssey spacecraft has spent over 15 years in orbit around Mars, circling the planet more than 69000 times. It holds the record for longest working spacecraft at Mars. THEMIS, the IR/VIS camera system, has collected data for the entire mission and provides images covering all seasons and lighting conditions. Over the years many features of interest have received repeated imaging, building up a suite of images covering the entire feature. From the deepest chasma to the tallest volcano, individual dunes inside craters and dune fields that encircle the north pole, channels carved by water
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Clear to Hazy
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Candor Chasma
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The lava flows in this image from NASA's 2001 Mars Odyssey spacecraft are part of Ascraeus Mons.
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The channels and depressions seen in this image from NASA's 2001 Mars Odyssey spacecraft are part of Gordii Fossae, located on the volcanic plains between Olympus Mons and Gigas Sulci.
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Located on the extensive lava plains between Olympus Mons and Alba Mons, this image from NASA's 2001 Mars Odyssey spacecraft shows complex intersecting valleys, which were created by lava flow.
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Lycus Sulci
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This VIS image shows part of the eastern end of Candor Chasma. The edge of the canyon is at the bottom of the image. The slopes of the chasma a eroded into a series of ridges and valleys. Winnowing of unconsolidated sediments by long term unidirectional winds can create these features. The ridge and valley system is called a yardang. Orbit Number 74936 Latitude -8.6632 Longitude 294.841 Instrument VIS Captured 2018-11-05 12 02
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These fractures and graben are part of Gordii Fossae, a large region that has undergone stresses which have cracked the surface as seen by NASA's 2001 Mars Odyssey spacecraft.
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This image from NASA's 2001 Mars Odyssey shows a complex tributary channel and its entry to the main channel of Shalbatana Vallis.
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The dunes seen in this VIS image are located on the complex floor of Rabe Crater. The sand is likely derived by erosion into the deposit that fills most of the crater floor, creating a pit which hosts the dunes. Rabe Crater is located in Noachis Terra and is 108km in diameter (67 miles). Orbit Number 82906 Latitude -43.447 Longitude 35.0145 Instrument VIS Captured 2020-08-22 18 52
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This VIS image shows part of the northwestern 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 in the image are concentric faults. Pavonis means peacock in Latin, making the name peacock mountain. Orbit Number 88202 Latitude 0.534605 Longitude 245.963 Instrument VIS Captured 2021-11-01 20 33
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This image captured by NASA's 2001 Mars Odyssey spacecraft shows sand dunes on the floor of Sumgin Crater.
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This image captured by NASA's 2001 Mars Odyssey spacecraft shows dunes on the floor of an unnamed crater in Noachis Terra.
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Meridiani Planum
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Hummocky, textured terrain within lava flows northwest of Pavonis Mons, one of the Tharsis volcanoes, is shown in this image from NASA's Mars Odyssey spacecraft.
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Today's VIS image shows part of Claritas Fossae. The linear features (fossae) are graben, a tectonic feature created when blocks of material subside between paired faults. These graben filled highlands are bounded by Solis Planum to the northeast and Icaria Planum to the southwest. Extensional tectonic forces are responsible for graben formation. While close to the Tharsis region, it is thought that Claritas Fossae formed prior to the large lava flows located north of this image. The large, deepest depression is younger than the other graben of Claritas Fossae. It is not known if it formed just after the other graben, or at a much later time. Orbit Number 90760 Latitude -12.0301 Longitude 249.617 Instrument VIS Captured 2022-05-31 11 34
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The Medusae Fossae Formation, shown in this image from NASA's Mars Odyssey spacecraft, is a large region of material that is easily eroded by the wind. The work of the wind has produced a variety of surface textures.
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The channels in this image captured by NASA's 2001 Mars Odyssey spacecraft dissect the far western flank of the Elysium Mons highland.
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Parts of Meridiani Planum have a surface that appears to be composed of different layers of material. In this image taken by NASA's Mars Odyssey the contrast of bright and dark materials indicates the different layers.
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Located on the margin of Zephyria Planum, this image from NASA's 2001 Mars Odyssey shows the effect the wind has had on the surface of Mars. Loose materials have been removed and semi-consolidated materials have been eroded into narrow hill forms.
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Olympus Rupes is the name of the large escarpment surrounding Olympus Mons. The escarpment is a cliff where there is a large elevation change over a short distance. This VIS image is located along the southeastern margin of Olympus Mons, the largest Martian volcano. Orbit Number 72406 Latitude 14.4639 Longitude 229.509 Instrument VIS Captured 2018-04-11 02 30
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This VIS image shows a region of plains to the west of Alba Mons. Numerous windstreaks are visible. The bright material forming tails behind the craters were created by surface winds funneled over and around the crater. The raised rims and bowls of impact craters causes a complex interaction such that the wind vortex in the lee of the crater can both scour away the surface dust and deposit it back in the center of the lee. The tail shows the direction of the wind, in this case blowing from the lower right to the upper left or from southeast to northwest. Also visible in this image are lava flows from Alba Mons and linear graben. Orbit Number 81738 Latitude 38.9682 Longitude 239.118 Instrument VIS Captured 2020-05-18 15 10
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This VIS image shows sand dunes on the floor of an unnamed crater located between Terra Sabaea and Utopia Planitia. The inner crater rim seen in the bottom half of the image has flow-like features. This morphology is usually indicative of material containing a volatile such as ice moving downslope. Orbit Number 79947 Latitude 42.4781 Longitude 67.2101 Instrument VIS Captured 2019-12-23 03 56
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This image shows part of the Nili Patera dune field. High resolution imaging by other spacecraft has revealed that the dunes in this region are moving. Winds are blowing the dunes across a rough surface of regional volcanic lava flows. The paterae are calderas on the volcanic complex called Syrtis Major Planum. Dunes are found in both Nili and Meroe Paterae and in the region between the two calderas. The Odyssey spacecraft has spent over 15 years in orbit around Mars, circling the planet more than 69000 times. It holds the record for longest working spacecraft at Mars. THEMIS, the IR/VIS camera system, has collected data for the entire mission and provides images covering all seasons and lighting conditions. Over the years many features of interest have received repeated imaging, building up a suite of images covering the entire feature. From the deepest chasma to the tallest volcano, individual dunes inside craters and dune fields that encircle the north pole, channels carved by water
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Liu Hsin Crater
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Scalloped Depressions with Layers in the Northern Plains
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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.
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NASA's Mars Odyssey spacecraft captured this image of dunes located in Aonia Terra.
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This image shows part of the flank and margin of Ascraeus Mons
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Medusa Fossae
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Old Landslide In Ius Chasma
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Dark Sand and Bright Bedrock in Terra Meridiani
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The unusual surface texture seen in the image from NASA's 2001 Mars Odyssey spacecraft reflects the resistance of the surface rocks to erosion by the wind. This image shows part of the northern end of Gordii Dorsum.
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Today's VIS image shows part of Ceti Mensa. This mesa feature is located in western Candor Chasma and is composed of layered deposits and sand dunes. Orbit Number 88887 Latitude -5.94433 Longitude 284.64 Instrument VIS Captured 2021-12-28 06 13
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This image captured by NASA's 2001 Mars Odyssey spacecraft shows a small portion of Daedalia Planun, the result of vast eruptions of Arsia Mons.
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This VIS image shows a portion of eastern Terra Cimmeria. The image contains from bottom to top a region of hills, part of Sirenum Fossae, channels dissecting a ridge, and a region of linear erosion. The top of the image is higher in elevation than the bottom. Orbit Number 81703 Latitude -36.0913 Longitude 179.445 Instrument VIS Captured 2020-05-15 17 36
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Ripple bedforms fill large fractures near the southern rim of Holden Crater in this image from NASA's Mars Odyssey spacecraft.
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This image captured by NASA's 2001 Mars Odyssey spacecraft shows part of Candor Chasma.
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The unusual and apparently layered surface in this image from NASA's 2001 Mars Odyssey spacecraft is located in Aureum Chaos.
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Noctis Labyrinthus
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Daedalia Planum was created by extensive lava flows from Arsia Mons. This image from NASA's Mars Odyssey shows a small portion of those flows.
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The multiple trends of yardangs in this image indicate that the winds in the Elysium region have changed direction several times
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This dune field is located on the floor of a crater located southeast of Mutch Crater
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This canyon system imaged here by NASA's Mars Odyssey was named Valles Marineris in honor of its discoverer, NASA's Mariner 9 spacecraft. The image covers a portion of the canyon system called Melas Chasma.
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Coprates Chasma. Today's VIS image shows a cross section of Coprates Chasma. In this region the chasma has two sections - a deep, flat floored canyon at the top of the image, and a shallower section in the lower part of the image. The sections are divided by a large ridge. The floor of the bottom canyon is covered by large landslide deposits. Coprates Chasma is one of the numerous canyons that make up Valles Marineris. The chasma stretches for 960 km (600 miles) from Melas Chasma to the west and Capri Chasma to the east. Orbit Number 91988 Latitude -12.6995 Longitude 293.287 Instrument VIS Captured 2022-09-09 13 27 https //photojournal.jpl.nasa.gov/catalog/PIA25717
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This image displays sand dunes within Proctor Crater. These dunes are composed of basaltic sand that has collected in the bottom of the crater. The topographic depression of the crater forms a sand trap that prevents the sand from escaping. Dune fields are common in the bottoms of craters on Mars and appear as dark splotches that lean up against the downwind walls of the craters. Dunes are useful for studying both the geology and meteorology of Mars. The sand forms by erosion of larger rocks, but it is unclear when and where this erosion took place on Mars or how such large volumes of sand could be formed. The dunes also indicate the local wind directions by their morphology. In this case, there are few clear slipfaces that would indicate the downwind direction. The crests of the dunes also typically run north-south in the image. This dune form indicates that there are probably two prevailing wind directions that run east and west (left to right and right to left). Orbit Number 83605 L
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The linear depressions in this VIS image are part of Idaeus Fossae. These features are located on the margin of Tempe Terra and the lowlands of Acidalia Planitia. Orbit Number 88025 Latitude 36.6727 Longitude 307.238 Instrument VIS Captured 2021-10-18 06 59
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This image from NASA's Mars Odyssey shows a portion of Tithonium Chasma, part of western Valles Marineris.
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Sand dunes cover part of the floor of this unnamed crater in Terra Cimmeria. Orbit Number 75321 Latitude -57.5486 Longitude 169.005 Instrument VIS Captured 2018-12-07 04 26
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This image shows the western section of the large sand ridge on the floor of Russell Crater. This is also the northern extent of the dune field. The crest of the large ridge runs from lower right to upper left. Smaller dune ridges intersect the large ridge perpendicular to the crest. Russell Crater is located in Noachis Terra. A spectacular dune ridge and other dune forms on the crater floor have caused extensive imaging. The Odyssey spacecraft has spent over 15 years in orbit around Mars, circling the planet more than 69000 times. It holds the record for longest working spacecraft at Mars. THEMIS, the IR/VIS camera system, has collected data for the entire mission and provides images covering all seasons and lighting conditions. Over the years many features of interest have received repeated imaging, building up a suite of images covering the entire feature. From the deepest chasma to the tallest volcano, individual dunes inside craters and dune fields that encircle the north pole, ch
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Today's VIS image is located in Gale Crater. Home to the Curiosity Rover since August of 2012, Gale crater is 154km in diameter (96 miles). Multiple features within the crater are visible in this image, including dunes, wind and water etched rock, layered central mound (Aeolis Mons common name Mount Sharp), and small channels. Aeolis Mons rises 18,000 ft (5,500 m) from the crater floor, higher than Mount Rainier rises above Seattle. Orbit Number 81879 Latitude -4.7719 Longitude 137.564 Instrument VIS Captured 2020-05-30 05 35
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These lava flows and channels are part of Alba Patera, a large collapsed volcano in the Tharsis region
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Looking again at the southeastern flank of the volcano the narrow nature of the flows are visible. Given the steep sides of the volcano, flows from the summit run as narrow rivers down the flank. The flows spread out into wider units when they encounter the flatter plains surrounding the volcano. The Odyssey spacecraft has spent over 15 years in orbit around Mars, circling the planet more than 69000 times. It holds the record for longest working spacecraft at Mars. THEMIS, the IR/VIS camera system, has collected data for the entire mission and provides images covering all seasons and lighting conditions. Over the years many features of interest have received repeated imaging, building up a suite of images covering the entire feature. From the deepest chasma to the tallest volcano, individual dunes inside craters and dune fields that encircle the north pole, channels carved by water and lava, and a variety of other feature, THEMIS has imaged them all. For the next several months the ima
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Candor Chasma Landslides
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This picture of Triton is a mosaic of the highest resolution images taken by NASA's Voyager 2 on Aug. 25, 1989 from a distance of about 40,000 kilometers (24,800 miles).
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Gale Crater. Today's VIS image shows part of Gale Crater, including the large layered deposit on the crater floor. This deposit has been heavily eroded, which exposed the layering. The Curiosity Rover is located in Gale Crater. Gale crater is 150km (90 miles) in diameter. Orbit Number 92243 Latitude -4.91547 Longitude 137.678 Instrument VIS Captured 2022-09-30 13 20 https //photojournal.jpl.nasa.gov/catalog/PIA25756
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This image shows part of Utopia Plainitia. The dark markings are dust devil tracks and possibly fractures
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A field of sand dunes is visible on the floor of this unnamed crater in Terra Sabaea. Orbit Number 88046 Latitude 26.5457 Longitude 62.9214 Instrument VIS Captured 2021-10-20 00 25
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This image captured by NASA's 2001 Mars Odyssey spacecraft shows several of the graben (fault bounded depression) that are part of Acheron Catena.
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This image shows the part of the southern cliff face of Hebes Chasma at the bottom of the image. The materials seen in the majority of this image are part of the erosion of the central mesa, perhaps created by a massive landslide. Hebes Chasma is an enclosed basin not connected to Valles Marineris. The Odyssey spacecraft has spent over 15 years in orbit around Mars, circling the planet more than 69000 times. It holds the record for longest working spacecraft at Mars. THEMIS, the IR/VIS camera system, has collected data for the entire mission and provides images covering all seasons and lighting conditions. Over the years many features of interest have received repeated imaging, building up a suite of images covering the entire feature. From the deepest chasma to the tallest volcano, individual dunes inside craters and dune fields that encircle the north pole, channels carved by water and lava, and a variety of other feature, THEMIS has imaged them all. For the next several months the i
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Daedalia Planum
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These dunes occur on the floor of Holden Crater as seen by NASA's 2001 Mars Odyssey spacecraft.
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Northern Meridiani Etched Terrain and Hematite Plains Contact
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This closed depression is located in Noachis Terra. To the south a channel leads to second region of erosion
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The small parallel ridges in this image captured by NASA's 2001 Mars Odyssey spacecraft were created by the erosive power of wind blown particles.
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This VIS image shows part of the floor of Russell Crater, including sand dunes of mulitple sizes. Russell Crater is located in Noachis Terra. Orbit Number 74472 Latitude -54.048 Longitude 12.3835 Instrument VIS Captured 2018-09-28 06 34
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The wind eroded material in this image from NASA's 2001 Mars Odyssey spacecraft are located just north of Amazonis Mensa.
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Biblis Patera
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At the base of this slope is a fan-shaped deposit of the slope forming material. The channel that the fan rests upon is Kasei Valles in this image as seen by NASA's 2001 Mars Odyssey spacecraft.
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Proposed MSL Site in Juventae Chasma
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Dunes cover the majority of this image of Rabe Crater. As the dunes are created by wind action the forms of the dunes record the wind direction. Dunes will have a long low angle component and a short high angle side. The steep side is called the slip face. The wind blows up the long side of the dune. In this VIS image the slip faces are illuminated more than the longer side. In this part of the crater the winds were generally moving from the lower right corner of the image towards the upper left. Rabe Crater is 108 km (67 miles) across. Craters of similar size often have flat floors. Rabe Crater has some areas of flat floor, but also has a large complex pit occupying a substantial part of the floor. The interior fill of the crater is thought to be layered sediments created by wind and or water action. The pit is eroded into this material. The eroded materials appear to have stayed within the crater forming a large sand sheet with surface dune forms as well as individual dunes where the
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. Terra Sabaea Channels. Today's VIS image shows part of the northeastern margin of Terra Sabaea. This regional boundary between the highlands of Terra Sabaea and lowlands of Utopia Planitia is heavily dissected by both fluid flow channels and extensive faulting. While many of the channels are unnamed, this image has three named channels Clasia Vallis (center of image with ridge in the middle of the channel), Hypsas Vallis (the next channel below Clasia Vallis) and Clanis Valles (the very shallow channel at the bottom of the image). Clasia Vallis is 147km (91 miles) long, Hypsas Vallis is 33km (20 miles) long. and Clanis Valles is 58km (36 miles) long. Orbit Number 94223 Latitude 34.7195 Longitude 57.7232 Instrument VIS Captured 2023-03-12 15 13
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This image from NASA's Mars Odyssey spacecraft shows the eastern portion of a region on Mars called Hesperia Planum. Immediately visible in the image is the dark barchan type dunes that are being blown against the southeast wall of the crater.
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This image from NASA's Mars Odyssey spacecraft shows grooves within channels of Kasei Valles that can be interpreted as evidence for fluvial activity.
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This image captured by NASA's 2001 Mars Odyssey spacecraft shows part of the South Polar cap.
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These dark sand dunes are located in an unnamed crater in Noachis Terra
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Olympus Mons
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Proctor Crater Dunes. This VIS image shows sand dunes within Proctor Crater. These dunes are composed of basaltic sand that has collected in the bottom of the crater. The topographic depression of the crater forms a sand trap that prevents the sand from escaping. Dune fields are common in the bottoms of craters on Mars and appear as dark splotches that often lean up against the downwind walls of the craters. Dunes are useful for studying both the geology and meteorology of Mars. The sand forms by erosion of larger rocks, but it is unclear when and where this erosion took place on Mars or how such large volumes of sand could be formed. The dunes also indicate the local wind directions by their morphology. In this case, there are few clear slipfaces that would indicate the downwind direction. The crests of the dunes also typically run north-south in the image. This dune form indicates that there are probably two prevailing wind directions that run east and west (left to right and right t
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Dark slope streaks marking the walls in this image of Noctis Labyrinthus captured 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. It contains both linear sections that appear to be tectonic in origin and sinuous sections that were more likely created by liquid flow. Given the location it appears that lava, rather than water, was the fluid. Olympica Fossae 420km long (261 miles). Orbit Number 94828 Latitude 24.6519 Longitude 245.654 Instrument VIS Captured 2023-05-01 10 42
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This image captured by NASA's 2001 Mars Odyssey spacecraft is further west from yesterday's image, near the margin between Coprates Chasma and Melas Chasma.
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These windstreaks are located on the downwind side of impact craters located in Syrtis Major as seen by NASA's 2001 Mars Odyssey spacecraft.
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This VIS image is located in Kaiser Crater and shows many individual dunes. The crater floor is visible between the dunes, indicating that there is a limited sand supply creating the dunes. Local winds continue to move the sand dunes across the crater floor. There are two sides to a dune, the low angle slope of the windward face and the high angle slope of the leeward side. The steep side is called the slip face. Wind blows sand grains up the low angle slope of the dunes which then fall down the slip face. In this way the whole dune moves towards the slip face. The winds blow from the windward to the leeward side of the dunes. In this image the slip faces are on the left side of the dune, so the dunes are slowly moving to the left side of this image. Kaiser Crater is located in Noachis Terra. Orbit Number 89982 Latitude -46.6859 Longitude 20.0452 Instrument VIS Captured 2022-03-28 09 55
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Arabia Terra Craters. Today's VIS image shows three craters located in northern Arabia Terra. The top two have material deposits on the crater floors that postdate the formation of the impact crater. A large channel dissects the rim of the crater at the top of the image. The central crater is named Focas Crater. Orbit Number 93975 Latitude 33.8015 Longitude 12.4675 Instrument VIS Captured 2023-02-20 05 08 https //photojournal.jpl.nasa.gov/catalog/PIA25938
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NASA's 2001 Mars Odyssey image shows a portion of Nirgal Vallis.
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This image captured by NASA's 2001 Mars Odyssey spacecraft shows a portion of the dune sheet and other dune forms on the floor of Proctor Crater.
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Coprates Chasma. Today's VIS image shows a cross section of Coprates Chasma. In this region the chasma has two sections - a deep, flat floored canyon at the top of the image (the northern cliff face is not visible in this image), and the second section below that separated by a large ridge. Paralleling it to the south runs a narrower and shallower chain of linked pits and depressions called Coprates Catena. Landslide deposits, layered materials and sand dunes cover a large portion of the chasma floor. The brighter materials at the top of the image are layered deposits. It is unknown how deep these canyon deposits were when they formed. The layering is only visible due to erosion, making it difficult to estimate the original thickness. While layered deposits can be found on the floor of Coprates Chasma, they are most commonly found along the lower elevations and at the bottom of the cliff faces in the canyon. Coprates Chasma is one of the numerous canyons that make up Valles Marineris.
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Today's VIS image shows part of Hydaspis Chaos, one of many regions of chaos in Margaritifer Terra. Chaos terrain is typified by mesas and valleys. The initial breakup of the surface can be due to tectonic forces, although on Mars it is thought that the mode of formation involves release of melted subsurface ice. With time and erosion the valleys widen and the mesas grow smaller. Hydaspis Chaos is is part of the huge outflow system flowing from Valles Marineris to Chryse Planitia. The channel in the center of the image becomes part of the larger Tiu Valles channel. Orbit Number 87600 Latitude 3.42796 Longitude 332.822 Instrument VIS Captured 2021-09-13 06 56
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Brashear Crater Dunes
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Located in the center of Hebes Chasma is a large deposit of layered material called Hebes Mensa. Extensive erosion has created gullies in the mensa and distributed fine sand size materials to create dunes and sand drifts within the chasma. Orbit Number 72030 Latitude -1.0854 Longitude 283.966 Instrument VIS Captured 2018-03-11 03 02
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This image shows individual dunes on the floor of Russell Crater, as well as larger dunes created by individual dunes coalescing . These dunes are in the western part of the dune field. Russell Crater is located in Noachis Terra. A spectacular dune ridge and other dune forms on the crater floor have caused extensive imaging. The Odyssey spacecraft has spent over 15 years in orbit around Mars, circling the planet more than 69000 times. It holds the record for longest working spacecraft at Mars. THEMIS, the IR/VIS camera system, has collected data for the entire mission and provides images covering all seasons and lighting conditions. Over the years many features of interest have received repeated imaging, building up a suite of images covering the entire feature. From the deepest chasma to the tallest volcano, individual dunes inside craters and dune fields that encircle the north pole, channels carved by water and lava, and a variety of other feature, THEMIS has imaged them all. For th
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The intersecting ridges in this image captured by NASA's 2001 Mars Odyssey spacecraft are called Angustus Labyrinthus. They were formed due to tectonic activity.
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Devil's Den in Terra Sirenum