Mars Geological Features

Images showcasing various Mars geological features including cross sections, channels, and tectonic structures, depicted in grayscale with scientific annotations.

Dark Dunes in Herschel Crater
Dark Dunes in Herschel Crater
149 assets in this story
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Ius Chasma. Today's VIS image shows a complete cross section of Ius Chasma. Ius Chasma is at the western end of Valles Marineris. Valles Marineris is over 4000 kilometers long, wider than the United States. Ius Chasma is almost 850 kilometers long (528 miles), 120 kilometers wide and over 8 kilometers deep. In comparison, the Grand Canyon in Arizona is about 175 kilometers long, 30 kilometers wide, and only 2 kilometers deep. The canyons of Valles Marineris were formed by extensive fracturing and pulling apart of the crust during the uplift of the vast Tharsis plateau. Landslides have enlarged the canyon walls and created deposits on the canyon floor. Weathering of the surface and influx of dust and sand have modified the canyon floor, both creating and modifying layered materials. There are many features that indicate flowing and standing water played a part in the chasma formation. The rugged floor of Ius Chasma in this image is the result of many large landslides. Orbit Number 92413
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The wind eroded surface in this image from NASA's 2001 Mars Odyssey spacecraft is located in Zephyria Planum.
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. Arabia Terra Channel. Today's VIS image shows part of a large unnamed channel located in northern Arabia Terra. Channels in this region of Arabia Terra typically flow northward into the lower elevations of Acidalia Planitia, however this channel flows east/west over the majority of its length. Orbit Number 94224 Latitude 36.8608 Longitude 28.5773 Instrument VIS Captured 2023-03-12 17 12
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Tempe Fossae. Today's VIS image is shows a portion of Tempe Fossae. The fossae are graben comprised of paired, parallel fractures with a down-dropped block of material between the fracture set. This morphology is created by extensional tectonic stresses. 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 north-northwest/south-southeast direction. This fossae system is located in Tempe Terra, a complexly fractured region bet
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Today's VIS image shows an unnamed channel in Terra Cimmeria. Orbit Number 87308 Latitude 2.36838 Longitude 116.9 Instrument VIS Captured 2021-08-20 05 54
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This VIS image shows a cross section of Pavonis Mons, including part of the summit caldera (circular region in the middle of the image). 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 surface collapses into the void formed by an emptied magma chamber. Pavonis Mons is the smallest of the three volcanoes with a summit of only 14km (8.7 miles) and a width of
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Wind is one of the remaining active processes altering the surface of Mars. In regions of long term unidirectional winds, the dust and sand is winnowed away. In places with poorly cemented surface materials the wind and entrained sand with blast the surface causing linear erosion like that seen in today's VIS image. This image is located at the equator near Gordii Dorsum. Orbit Number 77484 Latitude 5.04807 Longitude 213.038 Instrument VIS Captured 2019-06-03 08 10
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Tyrrhena Patera
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Dark Dunes in Herschel Crater
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This VIS image shows part of Cerunius Fossae. The linear depressions are fault bounded features called graben. These features form from tectonic forces that are pulling apart the surface, created space for material to slide down along the fault. Orbit Number 77308 Latitude 26.9347 Longitude 248.025 Instrument VIS Captured 2019-05-19 20 27
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This image from NASA's 2001 Mars Odyssey spacecraf shows part of the southern flank of Ascraeus Mons. Large collapse features are common in this area.
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Claritas Fossae is the dissected and fractured highland between the volcanic plains of Daedalia and Solis Planums. This image is from NASA's 2001 Mars Odyssey spacecraft.
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The extensive channel system seen is this VIS image include parts of both Sabis Vallis and Minio Vallis. The valles are just two of many channels that flow northward thru Terra Sirenum to empty into Amazonis Planitia. Sabis Vallis is 206km long (128 miles) and Minio Vallis is 88km long (55 miles). Both channels are located west of the much larger Mangala Valles. Orbit Number 81914 Latitude -5.1073 Longitude 207.895 Instrument VIS Captured 2020-06-02 02 44
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This image captured by NASA's 2001 Mars Odyssey spacecraft shows a small portion of the lava flows that make up Daedalia Planum.
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Kaiser Crater Dunes (VIS)
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Today's VIS image shows part of the floor of Orson Welles Crater. This region of the crater contains chaos. Chaos is formed where tectonic forces break the surface into blocks. Erosion along the breaks widen and deepen the valleys between creating mesas. There is evidence that this crater may once have held a lake. Orson Welles Crater is 116 km in diameter (72 miles). Orbit Number 94963 Latitude -0.688448 Longitude 314.526 Instrument VIS Captured 2023-05-12 13 20
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Juventae Chasma is an enormous box canyon which opens to the north and forms the outflow channel Maja Vallis. This image from NASA's Mars Odyssey spacecraft captures a portion of the western floor of Juventae Chasma and shows a wide variety of landforms.
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Lycus Sulci. Today's VIS image shows a portion of Lycus Sulci. Lycus Sulci is a low lying area of ridges and valleys found to the northwest of Olympus Mons. It is not yet understood how this feature formed or how it relates to the formation of Olympus Mons itself. Orbit Number 93612 Latitude 32.6141 Longitude 219.235 Instrument VIS Captured 2023-01-21 08 26 https //photojournal.jpl.nasa.gov/catalog/PIA25855
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Tractus Catena. This VIS image shows part of Tractus Catena, just one of many north/south trending tectonic graben located south and east of Alba Mons. The graben with circular pits are part of Tractus Catena. The graben without pits are part of Tractus Fossae. The pits most likely formed as a result of roof collapse into an underlying open space such as a lava tube. Orbit Number 93979 Latitude 28.6599 Longitude 257.766 Instrument VIS Captured 2023-02-20 13 00 https //photojournal.jpl.nasa.gov/catalog/PIA25940
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Kaiser Crater Dunes. This VIS image is located in Kaiser Crater and shows many individual dunes. The crater floor is visible between some of 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 91442 Latitude -46.9786 Longitude 19.5191 Instrument VIS Captured 2022-07-26 15 07
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This VIS image is located in the central 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 south 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. Orbit Number 79159 Latitude 19.0493 Longitude 124.534 Instrument VIS Captured 2019-10-19 06 34
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These clouds formed in the south polar region. The faintness of the cloud system likely indicates that these are mainly ice clouds, with relatively little dust content
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This image captured by NASA's 2001 Mars Odyssey spacecraft was collected simultaneously with yesterday's IR image. It shows part of the dune field on the floor of Rabe Crater.
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This image from NASA's Mars Odyssey spacecraft shows relatively dark coarse grained material forming individual dunes coalescing into a relatively uniform sand sheet.
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Alba Mons Flank. Today's VIS image is located on the western flank of Alba Mons. This region is highly dissected by channels. Alba Mons is a broad volcano, surrounded by graben features created by a huge volcanic eruption followed by the collapse of the volcano into the underlying empty magma chamber. Orbit Number 93786 Latitude 44.5605 Longitude 241.615 Instrument VIS Captured 2023-02-04 16 13 https //photojournal.jpl.nasa.gov/catalog/PIA25878
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This image from NASA's Mars Odyssey spacecraft shows a portion of Arda Valles.
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This image from NASA's 2001 Mars Odyssey spacecraft shows lava flows from Arsia Mons.
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Medusa Fossae Textures
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With all the frost gone, the south polar region is exhibiting more than just layering and surface markings. As this image from NASA's 2001 Mars Odyssey spacecraft shows, the polar surface is not smooth at this resolution.
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This daytime infrared image of Kaiser Crater, taken by NASA's 2001 Mars Odyssey spacecraft, shows the majority of the dune field located on the floor of the crater.
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The volcanic flows in this image from NASA's Mars Odyssey spacecraft are part of Daedalia Planum. The flows originated at Arsia Mons.
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This image from NASA's 2001 Mars Odyssey is located south of Olympus Mons and east of Gordii Dorsum, in a heavily wind eroded region. The winds are predominately east/west in this area.
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Protonilus Mensae. The mesas and valleys in this VIS image are part of Protonilus Mensae. Located between the relative highlands of northern Terra Sabaea and the lowlands of Vastitas Borealis, Protonilus Mensae is region of chaos terrain. 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. It has been proposed that a catastrophic outflow of subsurface water creates the chaos. Protonilus Mensae also shows signs of glacial flows, which would continue to modify the surface. Orbit Number 93930 Latitude 43.4172 Longitude 47.0895 Instrument VIS Captured 2023-02-16 12 47 https //photojournal.jpl.nasa.gov/catalog/PIA25929
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The linear ridges in this image captured by NASA's 2001 Mars Odyssey spacecraft are located near the south polar cap.
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Like yesterday's image, this image from NASA's Mars Odyssey spacecraft shows lava flows from Arsia Mons.
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This image from NASA's 2001 Mars Odyssey spacecraft shows part of the mesa and valley terrain called 'chaos.' This region of chaos is near the far eastern end of Valles Marineris.
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Today's VIS image shows part of the eastern flank of Arsia Mons, including part of Oti Fossae (bottom of image). Arsia Mons is the southernmost and youngest of the three large, aligned Tharsis volcanoes. Oti Fossae - linear graben - follow the major northeast/southwest trend of the volcanoes. Orbit Number 81526 Latitude -9.5484 Longitude 242.037 Instrument VIS Captured 2020-05-01 03 58
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Lava Flows and Surface Textures
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Today's VIS image shows more of the south polar cap at the end of summer. Orbit Number 67907 Latitude -85.55 Longitude 285.999 Instrument VIS Captured 2017-04-05 09 59
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This image captured by NASA's 2001 Mars Odyssey spacecraft shows part of the large sand sheet within Proctor Crater.
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Kaiser Dunes
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This image captured by NASA's 2001 Mars Odyssey spacecraft spans Candor Chasma.
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This VIS image shows a cross section of the eastern flank of Ascraeus Mons. Ascreaus Mons is the northernmost 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, collapse 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, Ascraeus 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 surface collapses into the void formed by an emptied magma chamber. Ascraeus Mons is the largest of the three volcanoes with a summit of 18km (11 miles) and a width of 460 km (286 miles). For comparison Maun
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This image captured by NASA's 2001 Mars Odyssey spacecraft shows part of the dune field on the floor of Rabe Crater.
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. Oti Fossae. The linear features in the bottom half of this VIS image are called Oti Fossae. Oti Fossae is located on the eastern flank of Arsia Mons and aligns with the regional northeast/southwest trend of the major Tharsis volcanoes. Fossae are typically tectonic features termed 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 crustal deformation in this region was from the inflation of the surface by the rise of magma that created the Tharsis volcanoes. Arsia Mons is the southernmost and youngest of the three large, aligned Tharsis volcanoes Arsia Mons, Pavonis Mons and Ascreaus Mons, from south to north. This alignment
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This image shows part of the complex caldera at the summit of the volcano. Calderas are found at the tops of volcanoes and are the source region for magma that rises from an underground lava source to erupt at the surface. Volcanoes are formed by repeated flows from the central caldera. The final eruptions can pool within the summit caldera, leaving a flat surface as they cool. Calderas are also a location of collapse, creating rings of tectonic faults that form the caldera rim. Ascraeus Mons has several caldera features at its summit. 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 dee
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This image from NASA's 2001 Mars Odyssey spacecraft shows part of the large sand sheet and surface dune forms on the floor of Proctor Crater.
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Adamas Labyrinthus. Today's VIS image shows part of southern Utopia Planitia. The irregular channel features are called Adamas Labyrinthus. Adamas Labyrinthus is approximately 853km (530 miles) along it's widest part. Orbit Number 93897 Latitude 35.6024 Longitude 102.309 Instrument VIS Captured 2023-02-13 19 00 https //photojournal.jpl.nasa.gov/catalog/PIA25905
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Eos Chasma Mensa
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Atlantis Chaos. Today's VIS image shows part of Atlantis 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. The mesas in this image appear brighter than the surrounding lowlands, likely due to relatively less dust cover. Atlantis Chaos is located in Terra Sirenum. Orbit Number 92160 Latitude -34.9498 Longitude 183.405 Instrument VIS Captured 2022-09-23 18 04 https //photojournal.jpl.nasa.gov/catalog/PIA25749
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This VIS image shows a cross section of Pavonis Mons. 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 surface collapses into the void formed by an emptied magma chamber. Pavonis Mons is the smallest of the three volcanoes with a summit of only 14km (8.7 miles) and a width of 375 km (233 miles). Like most shield volcanoes the surface has a low profile. In t
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The lineations seen in this NASA Mars Odyssey image occur in Acidalia Planitia. These fissures, or cracks in the ground, are possibly evidence that there was once subsurface ice or water in the region.
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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 channels
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This VIS image shows part of Tractus Fossae, a region of north/south trending tectonic graben located south of Alba Mons. 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 north/south. Because the faults defining the graben are formed parallel to the direction of the applied stress, we know that extensional forces were pulling the crust apart in the east/west direction. The large number of graben around Alba Mons is generally believed to be the result of extensional forces associated with the uplift of the volcano. Orbit Number 87590 Latitude 25.9931 Longitude 258.163 Instru
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This image of the southern flank of Ascraeus Mons, taken by NASA's 2001 Mars Odyssey spacecraft, shows a small sample of collapse features that are common in the area.
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Today's VIS image shows a portion of Tantalus Fossae. The linear features 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-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 the volcano. Tantalus Fossae is 2361 km (1467 m
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Dark Slope Streak with Streak-Generated Topography
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Sand Dune Field in Richardson Crater
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This channel feature in Ceraunius Fossae looks like a hooded cobra spitting venom
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Arcadia Planitia, shown in this NASA Mars Odyssey image, occupies a region just north of Amazonis Planitia, one of the brightest and dustiest regions on Mars.
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This VIS image of Olympia Undae was collected at the middle of north polar summer. The density of dunes and the alignments of the dune crests varies with location, controlled by the amount of available sand and the predominant winds over time. Olympia Undae is a vast dune field in the north polar region of Mars. It consists of a broad sand sea or erg that partly rings the north polar cap from about 120° to 240°E longitude and 78° to 83°N latitude. The dune field covers an area of approximately 470,000 km2 (bigger than California, smaller than Texas). Olympia Undae is the largest continuous dune field on Mars. Olympia Undae is not the only dune field near the north polar cap, several other smaller fields exist in the same latitude, but in other ranges of longitude, e.g. Abolos and Siton Undae. Barchan and transverse dune forms are the most common. In regions with limited available sand individual barchan dunes will form, the surface beneath and between the dunes is visible. In regions w
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Cydonia Region
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Coprates Chasma. Today's VIS image shows a cross section of Coprates Chasma. The floor of the 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. Paralleling the chasma to the south runs a narrower and shallower chain of linked pits and depressions called Coprates Catena. Orbit Number 93011 Latitude -14.3186 Longitude 299.989 Instrument VIS Captured 2022-12-02 19 04 https //photojournal.jpl.nasa.gov/catalog/PIA25811
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This image captured by NASA's 2001 Mars Odyssey spacecraft shows several of the graben that make up Ceraunius Fossae.
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This image captured by NASA's Mars Odyssey shows one edge of the complex caldera at the summit of Olympus Mons.
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Today's VIS image shows part a section of a mega gully. Located on the plains of Sinai Planum, it is just one of a number of huge channels that line the cliff face of Ius Chasma. The linear sides of the channel indicate that the formation of these features included tectonic activity. Ius Chasma is on the western end of Valles Marineris. Orbit Number 77719 Latitude -8.12758 Longitude 274.408 Instrument VIS Captured 2019-06-22 16 33
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This linear features near the South Polar Cap appeared during the height of southern summer
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Hematite Outlier
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Olympia Undae
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This mosaic is composed of the sharpest views of Pluto that NASA's New Horizons spacecraft obtained during its flyby of the distant planet on July 14, 2015.
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On Earth, these wind-derived features are called 'blowouts,' where the force of the wind has carved out a crescent-shaped depression in soft, uncemented material like glacial loess. This image is from NASA's Mars Odyssey.
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Heavy Cratering near Callisto's South Pole
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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 83387 Latitude -46.8031 Longitude 19.7369 Instrument VIS Captured 2020-10-01 08 54
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The dunes in Richardson crater, located at 72 degrees south latitude, are still covered in frost as seen by NASA's Mars Odyssey. The small dark spots are where the sun is beginning to remove the ice and reveal the darker dune materials below.
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Wind Action
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Opportunity's View After Sol 321 Drive
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The slope streaks and small, dark landslides are located in Noctus Labyrinthus
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Today's VIS image shows part of Aram Chaos. Aram Chaos was initially formed by a large impact. Over time the crater interior was modified by several different processes, including liquid water. Chaos forms from erosion of the surface into mesa features. With time the valleys expand creating the jumble of hills seen in the image. Orbit Number 80125 Latitude 1.19021 Longitude 338.127 Instrument VIS Captured 2020-01-06 19 28
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This image captured by NASA's 2001 Mars Odyssey spacecraft shows gullies on the northern face of one of the large depressions that mark the inner rim of Asimov Crater.
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This image to the east of Tharsis Tholus from NASA's Mars Odyssey spacecraft shows one of many vast fields of lava flows produced by the great Tharsis volcanoes.
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THEMIS Images as Art #6
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Today's VIS image is located just east of Arsia Mons. Numerous volcanic flows are visible, flowing downhill to the lower right side of the image. Several tectonic graben are present, generally trending perpendicular to the flows. A small channel feature and a discontinuous channel follow the flow trend. These features are likely lava channels and lava tube traces. Orbit Number 81763 Latitude -7.28995 Longitude 244.476 Instrument VIS Captured 2020-05-20 16 20
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The wind-sculpted yardangs in this scene from NASA's Mars Odyssey spacecraft are part of the Medusae Fossae Formation, a regionally extensive geologic unit that probably was produced from the accumulation of volcanic ash.
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Exposed Layers in Central Valles Marineris
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This image captured by NASA's 2001 Mars Odyssey spacecraft shows a landslide deposit from the cliffside along Tiu Valles.
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. South Polar Clouds. Today's VIS image shows a line of clouds over the south polar cap. These clouds are at an altitude above the surface where they are not directly interacting with the surface topography of the ice. During seasonal changes surface winds will sweep along the cap and create clouds where the winds dip into the troughs of the ice. Orbit Number 91751 Latitude -86.915 Longitude 182.233 Instrument VIS Captured 2022-08-21 01 31
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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. Subtle dark slope streaks are visible both in the channel walls and in the small crater at the bottom of the image. These features are thought to form by downslope movement of material which either reveals the darker rock beneath the dust coating, or creates the darker surface by flow of a volatile just beneath the dust coating. Orbit Number 81875 Latitude 25.8728 Longitude 248.783 Instrument VIS Captured 2020-05-29 21 51
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This image shows half of a crater on the polar cap as seen by NASA's 2001 Mars Odyssey spacecraft.
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This VIS image shows part of the southwestern cliffside of Melas Chasma. Melas Chasma is part of the largest canyon system on Mars, Valles Marineris. At only 563 km long (349 miles) it is not the longest canyon, but it is the widest. Located in the center of Valles Marineris, it has depths up to 9 km below the surrounding plains, and is the location of many large landslide deposits, as will as layered materials and sand dunes. There is evidence of both water and wind action as modes of formation for many of the interior deposits. Orbit Number 90921 Latitude -11.3343 Longitude 284.714 Instrument VIS Captured 2022-06-13 17 44
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This 2001 Mars Odyssey daytime infrared image shows dunes found in craters and on the plains of Terra Cimmeria.
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Spirit's View on Sol 124
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Channels and Erosion
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Dao and Niger Valles. Today's VIS image shows a small portion of both Dao Vallis (middle of image) and Niger Vallis (bottom of image). Arising from the volcano Hadriacus Mons (top of image), Dao Vallis is approximately 1200km (750 miles) long. Niger Vallis is 333 km (207 miles) long. It has been proposed that heating of the region due to volcanic activity melted subsurface ice which was released to the surface to carve the two channels. Niger Vallis merges with Dao Vallis south of this image and then flow southwestward into the Hellas Planitia basin. Orbit Number 93355 Latitude -33.4749 Longitude 93.0394 Instrument VIS Captured 2022-12-31 02 58 https //photojournal.jpl.nasa.gov/catalog/PIA25852
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At the top right of this NASA Mars Odyssey image, the rim of the caldera of Pavonis Mons, one of four exceptionally large volcanoes in the Tharsis region, is barely visible with steep cliffs formed by the collapse of a portion of the volcano's summit.
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Track of Right-Wheel Drag
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Scarp within Chasma Boreale
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This large dune field is located on the floor of Proctor Crater
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Cydonia Region - Detail
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Meandering Tracks on Husband
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Slope Streak South of Olympus Mons