Mars Geological Features

Images of Martian landscapes captured by spacecraft, showcasing geological formations such as valleys, ridges, and lava flows on the surface of Mars.

Candor Chasma

The hills and ridges at the top of this image captured by NASA's 2001 Mars Odyssey spacecraft are part of Nilus Mensae, which is part of the complex Kasei Valles channels.

This image from NASA's 2001 Mars Odyssey spacecraft shows a portion of Ma'adim Vallis, which is a large channel that enters Gusev Crater from the south.

The landslide deposits in this image captured by NASA's 2001 Mars Odyssey spacecraft are located in Baetis Chaos.

Dark slope streaks are found throughout Lycus Sulci in this image taken by NASA's 2001 Mars Odyssey spacecraft.

Daedalia Planum is comprised of enormous amounts of lava flows, the majority of which appear to be related to Arsia Mons. In this image from NASA's 2001 Mars Odyssey spacecraft, multiple overlapping flows are evident.

The complex channels in this image from NASA's 2001 Mars Odyssey spacecraft are part of Granicus Valles, located on the western margin of the Elysium volcanic region.

With a diameter of roughly 2,000 km (1,243 miles) and a depth of over 7 km (more than 4 miles), the Hellas Basin, shown in this image from NASA's Mars Odyssey spacecraft, is the largest impact feature on Mars.

Candor Chasma

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 83767 Latitude -25.1526 Longitude 220.709 Instrument VIS Captured 2020-11-01 15 42

This image captured by NASA's 2001 Mars Odyssey spacecraft shows a small portion of the boundary region between Terra Sabaea and Utopia Planitia.

Gusev Crater

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 83606 Latitude -34.6882 Longitude 183.955 Instrument VIS Captured 2020-10-19 09 36

Landslide

A landslide deposit is visible in this VIS image of Coprates Catena. Coprates Catena parallels the much larger Coprates Chasma; both are part of Valles Marineris. Orbit Number 71880 Latitude -14.7075 Longitude 295.237 Instrument VIS Captured 2018-02-26 18 24

$Dust slides are common in the dust covered region called Lycus Sulci. A large fracture is also visible in this image$

Wind Etching in Candor Chasma

Noctis Labyrinthus

Today's VIS image shows part of Solis Planum. Both volcanic and tectonic forces created the features in this image. The linear features that run diagonally across the image are fault features called graben. The rough surfaced regions are volcanic flows. Orbit Number 74613 Latitude -20.2864 Longitude 257.634 Instrument VIS Captured 2018-10-09 21 29

Dark slope streaks are a common feature on the cliff faces of Lycus Sulci as this image from NASA's 2001 Mars Odyssey spacecraft shows.

Arcuate Fractures in Olympus Mons Caldera

The channels in this image captured by NASA's Mars Odyssey spacecraft were created by the flow of lava. This image shows part of the region between Pavonis and Ascraeus Mons.

NASA's 2001 Mars Odyssey spacecraft shows the apparent effects of wind and water mark the surface of this region just northeast of Gusev Crater.

This image captured by NASA's 2001 Mars Odyssey spacecraft shows a portion of Olympus Rupes, part of the steep margin surrounding Olympus Mons. The term rupes means scarp.

This image from NASA's 2001 Mars Odyssey spacecraft shows Asimov Crater is unique in that the crater floor has been completely filled with material to approximately the crater rim and then a series depressions have occurred near the crater rim.

Dark Slope Streaks

A small landslide deposit is visible at the bottom left corner of this VIS image. The landslide is in an unnamed crater in Terra Sirenum. Orbit Number 74477 Latitude -35.232 Longitude 224.63 Instrument VIS Captured 2018-09-28 16 33

This image from NASA's 2001 Mars Odyssey spacecraft of Daedalia Planum shows the termination or end of a single flow. In this case it is the end of the brighter/rougher flow on the right side of the image.

This image captured by NASA's 2001 Mars Odyssey spacecraft shows a portion of Hebes Chasma.

Dark slope steaks mark the ridges of this region in Lycus Sulci in this image from NASA's 2001 Mars Odyssey spacecraft.

A Diminutive Volcano

This NASA 2001 Mars Odyssey spacecraft image shows the western edge of the summit caldera of Ceranus Tholus, one of the smaller volcanic constructs of the Tharsis region. Several channels dissect the western flank of the volcano.

This image from NASA's Mars Odyssey shows a small portion of two landslide deposits within Melas Chasma.

Today's VIS image shows a portion of Kasei Valles, just at the region where the northward flow of the channel turns eastward towards it's eventual end in Chryse Planitia. Kasei Valles is one of the largest outflow channel systems on Mars, in places up to 482 km (300 miles) wide and 1580 km (982 miles) long. For comparison, the Grand Canyon in Arizona is is only 29 km (18 miles) at its widest and only 446 km (277 miles) long. Orbit Number 79952 Latitude 20.11 Longitude 286.449 Instrument VIS Captured 2019-12-23 13 42

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. This VIS image is located along the northern cliff face of the chasma. The linear features are large landslide surfaces. A region of sand dunes is located along the change in elevation from the cliff face at the top of the image and the floor of the canyon at the bottom of the image. 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

Landslide

This image captured by NASA's 2001 Mars Odyssey spacecraft shows a portion of Nirgal Vallis.

The dunes in this image captured by NASA's 2001 Mars Odyssey spacecraft are located in an unnamed crater on the eastern margin of Tempe Terra.

Today's VIS image shows a section of a graben that is part of Nili Fossae. Graben are formed when a block of material drops downward between paired tectonic faults. Graben usually have straight sides with little sinuosity, whereas fluvial channels typically have large amounts of sinuosity along the length of the depression. Nili Fossae is located northeast of the large volcano Syrtis Major and northwest of the ancient impact basin Isidis Planitia. The graben, which can be about 500 meters (1,600 feet) deep, make concentric curves that follow the outline of Isidis Planitia. The faults likely formed as the crust sagged under the weight of lava flows filling Isidis Planitia. Orbit Number 79198 Latitude 23.3881 Longitude 78.7422 Instrument VIS Captured 2019-10-22 11 40

A network of small channels is visible in image from NASA's 2001 Mars Odyssey spacecraft.

This image captured by NASA's 2001 Mars Odyssey spacecraft shows lava channels in the Tharsis plains.

The linear depressions in the middle of this VIS image are graben called Cerberus Fossae. Graben form where extensional tectonic forces allows blocks of material to subside between paired faults. Cerberus Fossae are located in Elysium Planitia, southeast of the Elysium Mons volcanic complex. Orbit Number 87793 Latitude 15.3137 Longitude 163.349 Instrument VIS Captured 2021-09-29 04 24

The alluvial fans on the north side of this channel possibly represent the most recent activity in Kasei Valles

The isolated mesas in this image from NASA's 2001 Mars Odyssey spacecraft are part of Arsinoes Chaos. There is a material that differs from the rest of the chaos visible at the bottom of the image.

This image from NASA's Mars Odyssey shows Bahram Vallis where it enters Waspam Crater. Bahram Vallis exits the crater to the north a short distance from this location along the rim of Waspam Crater.

Meridiani Planum

Today's VIS image shows part of the southern margin of Candor Chasma. While not as deep as the northern regions of eastern Candor Chasma, the southern region contains all the features seen at the lower elevations to the north. Candor Chasma is one of the largest canyons that make up Valles Marineris. It is approximately 810 km long (503 miles) and is divided into two regions - eastern and western Candor. Candor is located south of Ophir Chasma and north of Melas Chasma. The border with Melas Chasma contains many large landslide deposits. The floor of Candor Chasma includes a variety of landforms, including layered deposits, dunes, landslide deposits and steep sided cliffs and mesas. Many forms of erosion have shaped Candor Chasma. There is evidence of wind and water erosion, as well as significant gravity driven mass wasting (landslides). Orbit Number 89860 Latitude -8.00834 Longitude 293.829 Instrument VIS Captured 2022-03-18 09 02

Olympus Mons

This image captured by NASA's 2001 Mars Odyssey spacecraft of Eumenides Dorsum shows erosion of the surface material by wind action.

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

Northern Hemisphere Gullies with Layers

This VIS image shows a section of Shalbatana Vallis. Shalbatana Vallis is located in Xanthe Terra and is one of many channels that empty into Chryse Planitia. Orbit Number 79639 Latitude 8.5729 Longitude 317.92 Instrument VIS Captured 2019-11-27 19 06

Russell Crater Dunes. This VIS image shows part of the floor of Russell Crater. Dunes of different shapes and sizes are located on the floor of this 135 km (22 miles) diameter crater. Russell Crater is located in Noachis Terra. Orbit Number 92871 Latitude -54.1627 Longitude 12.4699 Instrument VIS Captured 2022-11-21 06 37 https //photojournal.jpl.nasa.gov/catalog/PIA25806

Nili Fossae is a large band of parallel graben located to the northeast of Syrtis Major. The graben in this image from NASA's 2001 Mars Odyssey spacecraft were formed by tectonic activity.

The layered deposits in this Valles Marineris canyon imaged by NASA's Mars Odyssey spacecraft are heavily eroded by the wind into an impressive array of yardangs and swirling patterns of layers. The origin of the deposits remains a mystery.

A beautiful delta deposit in Harris Crater is the highlighted feature in this image captured by NASA's 2001 Mars Odyssey.

This image captured by NASA's 2001 Mars Odyssey shows a portion of Iani Chaos.

Tractus Catena Collapse Pits

Today's VIS image shows part of an unnamed crater in Terra Sirenum. The inner crater rim is dissected by numerous small channels. Orbit Number 82888 Latitude -44.1271 Longitude 194.346 Instrument VIS Captured 2020-08-21 07 18

Maunder Crater

Eroded Mesas

Today's VIS image shows a portion of the floor of an unnamed crater in Arabia Terra. Like several other craters on Mars, including the nearby Henry Crater, this crater contains a large mound of material that filled a large part of the crater floor. This mound has been subsequently eroded by the wind. These materials were brought into the crater sometime after the impact that formed the crater. Orbit Number 95048 Latitude 8.48497 Longitude 21.1439 Instrument VIS Captured 2023-05-19 13 22

This image from NASA's Mars Odyssey is located in Meroe Patera, which is a small region within Syrtis Major Planitia. Syrtis Major is a low-relief shield volcano whose lava flows make up a plateau more than 1,000 km (about 620 miles) across.

Today's VIS image shows part of Louros Valles on the southern part of Ius Chasma. Louros Valles is a region of mega gullies the empty into Ius Chasma. Ius Chasma is unique from the other chasmata of Valles Marineris in possessing mega gullies on both sides of the chasma. The largest mega gullies are located in Sinai Planum, dissecting those plains and emptying into the canyon. Mega gullies are thought to be sapping channels caused by groundwater flow and erosion. The Earth analog is springs - water that flows underground and then breaches the surface creating channels. The morphology of the Mars gullies mirrors terrestrial springs. The channel is fairly uniform in width and the head of the channel is rounded like an amphiteater. The channel lengthens by erosion at the head backwards as the surface where the spring emerges is undercut. For Mars it is theorized that subsurface water would stay liquid due to underground heating. Ius Chasma is at the western end of Valles Marineris, south

Dune forms cover the top of this sand sheet on the floor of Juventae Chasma, a chasma north of the Valles Marineris canyon system in this image from NASA's Mars Odyssey.

Located west of the Elysium Volcanic complex, Hebrus Valles is a complex channel system that flowed to the north. In this VIS image the channel features have the appearance of a channel formed by liquid flow. In other portions of the valles, there are pits and collapse features which appear to have formed by material falling into subsurface voids. This is a common feature in regions of volcanic activity where lava tubes run below the surface. Both water and lava probably contributed to the formation of Hebrus Valles. Orbit Number 71499 Latitude 17.8884 Longitude 127.923 Instrument VIS Captured 2018-01-26 09 17

This image captured by NASA's 2001 Mars Odyssey spacecraft shows a number of unnamed channels located on the northeastern margin of Terra Sabaea.

This unnamed channel complex in nothern Arabia Terra contains several different surface textures on the channel floor. The parallel ridges are unusally indicative of materials which contain volatiles

This image from NASA's 2001 Mars Odyssey spacecraft shows the dunes located on the floor of Brashear Crater.

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

The two linear depressions crossing this VIS image are graben created by tectonic activity. Orbit Number 77201 Latitude 4.92604 Longitude 98.3657 Instrument VIS Captured 2019-05-11 00 51

Spurs and gullies form the cliff sides of the Vallis Marineris chasmata at top of this image captured by NASA's 2001 Mars Odyssey spacecraft. Sand dunes at the bottom of image are a common feature on the floors of the chasmata.

The lava flows in this image from NASA's 2001 Mars Odyssey spacecraft most likely originated from Ascraeus Mons, one of the large Tharsis volcanos.

The unnamed channels in this image from NASA's 2001 Mars Odyssey spacecraft are located southeast of Albor Tholus.

Today's VIS image shows part of the northern cliff face of Melas Chasma and the large landslide deposits at the base of the cliff face. The landslide deposits are called Ophir Labes. The descriptor term labes means landslide. Orbit Number 74275 Latitude -9.66666 Longitude 290.547 Instrument VIS Captured 2018-09-12 01 22

This image captured by NASA's 2001 Mars Odyssey spacecraft shows a portion of Lycus Sulci, a complex region of ridges located on the northern side of Olympus Mons. The term sulci means subparallel furrows and ridges.

Today's VIS image shows part of Candor Chasma. Candor Chasma is one of the largest canyons that make up Valles Marineris. It is approximately 810 km long (503 miles) and has is divided into two regions - eastern and western Candor Chasma. Candor Chasma is located south of Ophir Chasma and north of Melas Chasma. The border with Melas Chasma contains many large landslide deposits. The floor of Candor Chasma includes a variety of landforms, including layered deposits, dunes, landslide deposits and steep sided cliffs and mesas. Many forms of erosion have shaped Candor Chasma. There is evidence of wind and water erosion, as well as significant gravity driven mass wasting (landslides). The bright features in this image are layered deposits that have been eroded by wind, and possible water. Orbit Number 89623 Latitude -6.93421 Longitude 291.118 Instrument VIS Captured 2022-02-26 20 41

Small gullies captured in this image from NASA's 2001 Mars Odyssey are located on the north and south sides of this hill. The hill is part of the mountainous region that borders the northeastern side of Argyre Planitia.

Arcuate Fractures

This image from NASA's Mars Reconnaissance Orbiter shows a sample of the variety and complexity of processes that may occur on the walls of Martian craters, well after the impact crater formed.

This image from NASA's Mars Odyssey of the floor of Ganges Chasma shows eroded fill material and extensive sand deposits.

This image captured by NASA's 2001 Mars Odyssey spacecraft shows a small portion of the lava flows of Solis Planum.

Today's VIS image shows a small portion of the extensive volcanic plains of Daedalia Planum. These lava flows originated from Arsia Mons, the southernmost of the three large Tharsis volcanoes. Orbit Number 75250 Latitude -13.305 Longitude 234.502 Instrument VIS Captured 2018-12-01 08 41

$Several fractures cross through Gorgonum Chaos in this image captured by NASA's 2001 Mars Odyssey spacecraft.$

Daedalia Planum is comprised of lava flows from Arsia Mons. This image was captured by NASA's 2001 Mars Odyssey spacecraft.

This image from NASA's Mars Odyssey spacecraft shows the major channel that started near the top of Mt. Sharp. Near the top of this image is a wide valley that reaches to the crater floor and the nearby dunes.

$Tempe Terra is criss-crossed with numerous fracture systems. This image from NASA's Mars Odyssey shows a region where the fractures are intersecting,$

Continuing westward, this image from NASA's Mars Odyssey spacecraft shows Mt. Sharp just east of the highest peak of the deposit. The dark material near the top of the image is likely sand. This image shows the dark material on the floor and on Mt. Sharp.

This image from NASA's Mars Odyssey spacecraft covers part of Tithonium Chasma, which is part of the Valles Marineris system of canyons that stretch for thousands of kilometers.

Small dunes are located on the floor of this unnamed crater in Terra Cimmeria as seen by NASA's 2001 Mars Odyssey spacecraft.

This image from NASA's Mars Odyssey shows multiple landslide deposits within Ganges Chasma.

Aurorae Chaos is located at the eastern end of the chasmata forming Vallis Marineris. This image from NASA's 2001 Mars Odyssey spacecraft is very close to the chasmata and at a higher elevation than the floor of the chasmata.

Today's VIS image shows a region of wind etched materials. In regions of poorly cemented surface materials it is possible to create large features due to just the action of the wind. The equatorial region between Olympus Mons and Apollinaris Mons is dominated by wind etched regions. The direction of the wind aligns with the ridges and valleys. The dominant wind direction in this region is southeast to northwest; however, the wind direction for the upper right of the image is to the other direction. The long linear wind etched valleys are called yardangs. These features are created by long term winds scouring a poor cemented surface material into linear ridges and valleys. These yardangs are part of the Medusa Fossae Formation. It has been suggested that this region of Mars provides a large percentage of the surface dust seen around the planet. Ash falls from nearby volcanoes may have been the source of the surface materials eroded into these and other wind eroded landforms. Orbit Numbe

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. This VIS image shows part of a large ridge of material near the south central part the canyon. The roughest looking material is the top of the ridge. 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,

$This image captured by NASA's 2001 Mars Odyssey shows a small portion of the large fracture called Cerberus Fossae.$

Water Flow Evidence in Kasei Vallis

Do you see what I see in this image captured by NASA's 2001 Mars Odyssey spacecraft One of the mesas in this image is heart shaped.

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 75325 Latitude -18.8135 Longitude 231.098 Instrument VIS Captured 2018-12-07 12 54

Proposed MSL Site in Nili Fossae Crater

Olympus Mons

This image captured by NASA's Mars Odyssey shows a portion of the dunes located in the floor of Kaiser Crater.

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