Martian Crater Topography

Images of various Martian craters showing intricate landscapes, including gullies, landslides, and channel formations as captured by NASA's Mars Odyssey.

This unnamed crater near Timoshenko Crater has been breached by a channel
This unnamed crater near Timoshenko Crater has been breached by a channel
291 assets in this story
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Herschel Dunes
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Aeolis Landslides
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This image from NASA's 2001 Mars Odyssey spacecraft shows several channels dissecting the rim of Semeykin Crater.
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Slope Streaks
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This image captured by NASA's 2001 Mars Odyssey spacecraft shows the interior of an unnamed crater near Nili Fossae.
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Crater Ejecta
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THEMIS ART #96
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An unnamed channel dissects the surface of Terra Cimmeria as seen by NASA's 2001 Mars Odyssey spacecraft.
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With its rim eroded off by catastrophic floods in Tiu Vallis and its strangely angular shape, this 12 km (about 7.5 mile) diameter crater imaged by NASA's Mars Odyssey spacecraft looks vaguely like a stop sign.
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The ejecta materials of this crater are more resistant to erosion than the surrounding materials. The wind has eroded pits and other features around the crater causing it to become a topographic high. This image is from NASA's Mars Odyssey.
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The floor of this crater near its southwestern rim is rougher that the rest of the crater floor. Some process of change is working only in this area
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Dark slope streaks mark the rim of this unnamed crater in Terra Sabaea captured by NASA's Mars Odyssey.
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This image from NASA's 2001 Mars Odyssey spacecraft shows the northwestern floor and rim of Gale crater. A channel dissects the rim, and the edge of the central mound is visible in the bottom right corner. This is the landing site of NASA's rover, Curiosi
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Apollinaris Patera
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The rim and floor of this southern crater are relatively unmodified, indicating that this crater is younger than its more weathered neighbors
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This image of Terra Cimmeria captured by NASA's 2001 Mars Odyssey spacecraft shows two channels intersecting to become one larger channel.
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This image from NASA's 2001 Mars Odyssey spacecraft shows some of the extensive volcanic flows east of the large Tharsis volcanoes.
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This VIS image shows a linear depression in Syria Planum. Volcanic activity, including broad shield volcanoes and extensive volcanic plains created this region of the Tharsis system south of Noctis Labyrinthus. Linear features, like the one in this image, can be caused by several different processes. In this case a combination of tectonic forces and lava emplacement created the depression. Orbit Number 74800 Latitude -14.4492 Longitude 260.323 Instrument VIS Captured 2018-10-25 07 10
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The 'tail' behind the crater at the top of this image from NASA's 2001 Mars Odyssey spacecraft is called a windstreak. This feature is formed by winds blowing over/in and around the crater.
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This VIS image shows a small section on Margaritifer Chaos. The term chaos is applied to regions where the surface is being eroded to form mesas. As the surface processes continue individual mesas become more isolated and take on the appearance of regions of hills. At the top of the image is Margaritifer Terra, which is being dissected into large mesas. Towards the bottom of the image the mesas have been eroded into smaller hills. Orbit Number 72315 Latitude -8.86121 Longitude 339.105 Instrument VIS Captured 2018-04-03 14 28
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The linear depressions in this VIS image are part of Sirenum Fossae. These depressions are called graben, which form by the down drop of material between two parallel faults. The faults are caused by extensional tectonic stresses in the region. The fossae are 2735km long (1700 miles). Orbit Number 81265 Latitude -28.9299 Longitude 214.351 Instrument VIS Captured 2020-04-09 16 06
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These arcuate fractures are located on the margin between Memnonia Fossae and Elysium Planitia
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Today's VIS image shows some of the ejecta from Bacolor Crater in Utopia Planitia. There are several layers of ejecta visible in the image. The crater itself is just off the image to the lower right. Orbit Number 68581 Latitude 33.2419 Longitude 118.099 Instrument VIS Captured 2017-05-30 23 30
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Today's VIS image shows an unnamed crater in Tartarus Colles. The crater floor has been modified by several processes, creating the mounded and fractured features. Layering in the small upper crater suggested that standing water played a part in the modifications. Orbit Number 95130 Latitude 12.8101 Longitude 174.875 Instrument VIS Captured 2023-05-26 07 26
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Mantled Surface of Ascraeus Mons
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This image from NASA's Mars Odyssey spacecraft shows crater wall dust avalanches in southern Arabia Terra.
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Interesting textures on lava flows in Daedalia Planum, southwest of the Tharsis volcanoes, can by observed in this image from NASA's Mars Odyssey spacecraft.
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This image from NASA's Mars Odyssey shows part of the eastern flank of Ascraeus Mons, one of the large Tharsis Volcanoes. The circular pits all aligned in a row mark the collapse of the roof of a lava tube.
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The narrow lava flows in this image from NASA's 2001 Mars Odyssey spacecraft are located on the northeastern flank of Olympus Mons.
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This VIS image shows a small section of an unnamed channel in Arabia Terra. This is just one of many channels dissecting the region. Orbit Number 78702 Latitude -4.98861 Longitude 352.581 Instrument VIS Captured 2019-09-11 15 18
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Accumulations of thick dust give way down slopes, crater walls, and other steep terrain in this image from NASA's Mars Odyssey, leaving the dark streaks that are common in the dusty region of Arabia Terra.
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Channel
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Moreux Crater is located in the northern part of Terra Sabaea. The crater has a region of sand dunes on the crater floor, as well as features that are similar to glacial topography on Earth. The glacial flows occur from both the crater rim and the central crater peak. Glacial activity creates fine scale materials, which means the source of the dune sands may be local, rather than materials blown in from outside of the crater. Orbit Number 71851 Latitude 41.908 Longitude 44.2358 Instrument VIS Captured 2018-02-24 09 22
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Isolated hills and a small channel are visible in this image of Gigas Sulci captured by NASA's 2001 Mars Odyssey spacecraft . Gigas Sulci is located southeast of Olympus Mons.
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Uranius Patera
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MSIP: Elysium Mons Lava Flow
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This VIS image shows part of Medusa Fossae. Winds have eroded materials in this region, creating ridges and valleys aligned with the direction of the wind. Orbit Number 72008 Latitude -3.47752 Longitude 199.295 Instrument VIS Captured 2018-03-09 07 31
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The ridges and infilling lava flows make up the region termed Gordii Sulci
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This image captured by NASA's 2001 Mars Odyssey spacecraft is located near Memnonia Sulci, on the edge of Lucus Planum.
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This image from NASA's 2001 Mars Odyssey spacecraft shows a landslide occurred on the rim of Fesenkov Crater, creating the deposit visible in this image.
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Channel and Graben
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Fractures
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This image captured by NASA's 2001 Mars Odyssey spacecraft shows a small portion of Yuty Crater's ejecta blanket.
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'Butterfly' ejecta is the name given when a crater has two lobes of ejecta on opposite sides, with little or no ejecta between the lobes. This image is from NASA's 2001 Mars Odyssey spacecraft.
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The discontinuous channels in this image are collapsed lava tubes
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Old Geology and New Geology
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This NASA Mars Odyssey image covers a large area over the summit of Ulysses Patera, one of the many volcanoes that make up the giant Tharsis volcanic province, although Ulysses itself is fairly small in comparison to the other volcanoes in this area.
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Today's VIS image shows a field of dunes on the floor of an unnamed crater near Schiaparelli Crater in Noachis Terra. Orbit Number 79163 Latitude -3.81259 Longitude 12.247 Instrument VIS Captured 2019-10-19 14 21
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This VIS image is located on the margin of Arabia Terra and Acidalia Planitia. The channel features were created by fluids running from the highland of Arabia Terra into the lower elevations of Acidalia Planitia. Orbit Number 77367 Latitude 31.0987 Longitude 345.16 Instrument VIS Captured 2019-05-24 17 05
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The southern Amazonis Planitia shows two craters with ejecta that stand out above the surrounding surface. The ejecta has remained in place while the surrounding material was removed. This image is from NASA's 2001 Mars Odyssey spacecraft.
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The floor of Coprates Chasma contains many different geologic landforms. This image, taken by NASA's 2001 Mars Odyssey spacecraft, shows the effects of wind and landslides.
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Today's VIS image shows part of the lowland plains north of the Elysium volcanic complex. Right angles are almost always created by tectonic forces. These linear depressions and the right angle intersections most likely were created in response to the volcanic activity that resulted in the uplifted surface and volcanoes of Elysium. Orbit Number 88717 Latitude 37.1901 Longitude 143.037 Instrument VIS Captured 2021-12-14 06 30
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This complexly eroded region is part of Aeolis Planum with portions that appear to be layered material that has been eroded by wind action. This image is from NASA's 2001 Mars Odyssey spacecraft.
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The complex channel in this image is a small section of Reull Vallis as seen by NASA's 2001 Mars Odyssey spacecraft.
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Fans of Lava Flows on the Flanks of Olympus Mons
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Continuing eastward, this image of Gale captured by NASA's 2001 Mars Odyssey spacecraft shows the reappearance of dunes on the crater floor near the margin of Mt. Sharp.
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Windstreak
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The ridge in this image captured by NASA's 2001 Mars Odyssey spacecraft shows the Tharsis region (called Uranius Dorsum) reminds one of a skeletal spine.
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The linear feature in this VIS image is part of Labeatis Fossae. Fossae are linear depressions, most often caused by extensional tectonic forces pulling the crust apart and allowing material to slide downward between bounding faults. This type of feature is called a graben. In this image, the feature as numerous circular features within the fossae. In regions of volcanic flows, the depression may be caused by roof collapse into an underlying void left by a lava tube. As this feature is located in the Tharsis volcanic region, it is likely that this feature was primarily created by volcanic collapse rather tectonic stress. Orbit Number 79516 Latitude 21.1075 Longitude 264.698 Instrument VIS Captured 2019-11-17 16 06
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Two Craters
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This image from NASA's Mars Odyssey is of a doublet crater located in Utopia Planitia, near the Elysium Volcanic region. Doublet craters are formed by simultaneous impact of a meteor that broke into two pieces prior to hitting the surface.
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The ejecta of the impact crater shown in this image from NASA's Mars Odyssey spacecraft appears to have been modified after it was emplaced. This modification may be due to the presence of subsurface ground ice.
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Platy Lava Flow
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Nirgal Vallis
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Today's VIS image shows part of the inner rim of Kaiser Crater. The rim has been dissected by numerous gullies. Kaiser Crater is located in Noachis Terra. Orbit Number 74952 Latitude -44.6907 Longitude 19.7647 Instrument VIS Captured 2018-11-06 18 59
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The linear features in this VIS image are called Mareotis Fossae. They are part of a huge region of graben that comprise Tempe Terra. The graben of Mareotis Fossae trend to the northeast, parallel to the fossae of Alba Mons located just to the west of Tempe Terra. 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 northeast to 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 northwest/southeast direction. Mareotis Fossae is 1907km long
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Crater Dunes
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This VIS image is located in the southeastern portion of Hephaestus Fossae. Hephaestus Fossae is a complex channel system in Utopia Planitia near Elysium Mons. It has been proposed that the channel formed by the release of melted subsurface ice during the impact event that created a large crater west of this image. Additionally, the nearby Elysium volcanic center created subsurface heating that may have played a part in creating both Hephaestus Fossae and Hebrus Valles to the north. Hephaestus Fossae are over 600km long (373 miles). Orbit Number 78847 Latitude 17.5748 Longitude 126.158 Instrument VIS Captured 2019-09-23 13 59
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Landslides
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In this image the action of the wind is forming yardangs. The top layer of material is being removed by the wind, revealing an older surface below -- like the crater at the bottom of the frame
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This image captured by NASA's 2001 Mars Odyssey spacecraft shows two circular features. The flat floored feature is the summit caldera of Elysium Mons and the bowl-shaped feature next to the caldera is an impact crater.
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Today's VIS image shows a small part of Daedalia Planum. The lava flows originate from Arsia Mons, one of the large volcanoes in the Tharsis region. The different surface textures are created by differences in the lava viscosity and cooling rates. The lobate margins of each flow can be traced back to the start of each flow or to the point where they are covered by younger flows. Flows in Daedalia Planum can be as long as 180 km. Orbit Number 82038 Latitude -14.622 Longitude 231.902 Instrument VIS Captured 2020-06-12 07 44
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Texture
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This VIS image shows part of the floor of Spallanzani Crater. At some point after the crater was created the floor was covered by a fill material. The material was laid down in layers, which are easily identifiable at the eroded margins of the desposit. Spallanzani Crater is located near the southeast margin of Hellas Planitia in Promethei Terra. Orbit Number 75249 Latitude -58.0904 Longitude 86.3064 Instrument VIS Captured 2018-12-01 06 07
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This VIS image shows part of a complex channel system located in northern Arabia Terra. While there are many unnamed channels in region, this one is very long and substantial in width. The uniform width over much of the length of the feature, and the straightness of the channel sections may indicate these are tectonic features rather than channels caused by fluid action. The fact that this feature is not called a vallis or valles (fluid flow channels) indicates that those who have studied this feature lean towards the tectonic origin for the channels. Orbit Number 87261 Latitude 36.7761 Longitude 27.9326 Instrument VIS Captured 2021-08-16 09 13
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This image captured by NASA's 2001 Mars Odyssey spacecraft shows part of the sand sheet and dunes on the floor of Rabe Crater.
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This wind eroded crater is located between Eumenides and Gordii Dorsa. The ejecta of the crater is more resistant to the wind than the surrounding materials in this image from NASA's Mars Odyssey.
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This image captured by NASA's 2001 Mars Odyssey spacecraft shows part of the extensive flow field called Daedalia Planum. The lava flows originated at Arsia Mons.
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This image shows part of the summit caldera of Ceraunius Tholus. Channels are common on the flanks of this volcano
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Dark slope streaks are visible in this image of Amazonis Planitia captured by NASA's 2001 Mars Odyssey spacecraft.
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The craters in this image from NASA's 2001 Mars Odyssey spacecraft are located in a region of prolonged wind action. The ejecta of the craters is more resistant to the wind than the materials around it.
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Dark slope streaks are common throughout the ridges that comprise Lycus Sulci in this image captured by NASA's 2001 Mars Odyssey spacecraft.
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Taken by one of the Mars Student Imaging Project (MSIP) teams, these are the unusual floor deposits in Spallanzani Crater. The wind may have affected the surface of the layered deposit. Small dunes have formed near the southern margin
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The large crater in this image is called Gandzani Crater. The crater is not circular, but appears to have corners . This crater is located in Mareotis Fossae, a huge complex of graben that make up part of Tempe Terra. The tectonic activity would include subsurface fracturing, which would have deflected impact pressures along fault faces. Meteor Crater in Arizona has corners due to the same tectonic forcing of impact pressures. Orbit Number 79104 Latitude 34.6565 Longitude 268.965 Instrument VIS Captured 2019-10-14 17 58
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Located in Noachis Terra, Asimov Crater has an unusual crater floor morphology. At some point after the crater formed, the interior was filled by materials that reached almost to the top of the crater rim. At some later point, deep depressions formed along the inner crater rim. Channels dissect both sides of these depressions. The mechanism of both the filling of the crater and the formation of the depressions is not known. Two other nearby craters also have filled floors and interior depressions. This VIS image shows the southwestern section of the interior depression. Orbit Number 74834 Latitude -47.6066 Longitude 4.28931 Instrument VIS Captured 2018-10-28 02 12
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The dissected surface seen in this image from NASA's 2001 Mars Odyssey spacecraft is near Warrego Valles.
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Channel
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Today's VIS image shows an unnamed channel in northern Terra Sabaea. The regional boundary between the highlands of Terra Sabaea and lowlands of Utopia Planitia is heavily dissected by both fluid flow channels and extensive faulting. Orbit Number 79922 Latitude 28.8312 Longitude 70.6552 Instrument VIS Captured 2019-12-21 02 28
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Light Outcrop on Crater Floor
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The channels in this VIS image are part of Clanis Valles. Clanis Valles is on the eastern margin of Terra Sabaea. The channel system is 58km long (36 miles). Orbit Number 86948 Latitude 33.549 Longitude 58.0713 Instrument VIS Captured 2021-07-21 14 41
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Martian Dichotomy Boundary
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A multitude of dark slope streaks mark the inner rim of this unnamed crater in Terra Sabaea. This image is from NASA's 2001 Mars Odyssey spacecraft.
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Craters and Grabens: Circles and Lines
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Volcanic Vent
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Hebrus Vallis
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This image captured by NASA's 2001 Mars Odyssey spacecraft shows a small unnamed channel in Terra Sabaea.
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Gullies are visible in this image of the northern rim of Holden Crater as seen by NASA's 2001 Mars Odyssey spacecraft.
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Hecates Channels
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The channel crossing this image from NASA's 2001 Mars Odyssey spacecraft is called Ma'adim Valles.
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This image from NASA's 2001 Mars Odyssey spacecraft shows an unnamed crater in Chryse Planitia. There are several concentric ridges visible on the right side of this image.