Martian Geological Features

High-resolution grayscale images capturing volcanic flows, canyons, and channels on Mars, showcasing diverse geological formations and textures.

This image is located in the Tyrrhena Terra region. The cause of the bright markings/material is unknown. It is possible that the formation of the channels are exposing a series of bright layered material

The volcanic flows in image from NASA's 2001 Mars Odyssey spacecraft are located south of Ascraeus Mons and east of Pavonis Mons.

Today's VIS image shows a section of Ares Vallis. Ares Vallis is a large channel that arises in Iani Chaos, passes through Margaritifer Terra, and then empties into Chryse Planitia. Orbit Number 80624 Latitude 0.445959 Longitude 342.666 Instrument VIS Captured 2020-02-16 21 33

Landslides

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. Landslide deposits, layered materials and sand dunes cover a large portion of the chasma floor. This image is located in eastern Coprates Chasma. The branching features near the bottom of the image are spurs of rock in the cliff face. The rock is more resistant to erosion that fine materials like sand and dust. Those materials are visible below the spurs, and then onto the canyon floor. Unlike the large landslide deposits, these small fans of material build up over time as the material above erodes. There are sand dunes along the edge of the fans in this 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 an

This complex channel is located in the Nili Fossae region as seen by NASA's 2001 Mars Odyssey spacecraft.

This image from NASA's 2001 Mars Odyssey spacecraft shows the floor of an unnamed crater east of Aram Chaos and Ares Vallis. There are two distinct elevations on the crater floor, which may indicate layered fill material.

Candor Chasma Plateau

This image is located in the Tyrrhena Terra region. The cause of the bright markings/material is unknown. It is possible that the formation of the channels are exposing a series of bright layered material

An extensive field of small, dark dunes in located on the floor of the unnamed crater in Arabia Terra

The mitten-shaped feature in Candor Chasma is a landslide deposit in this image from NASA's 2001 Mars Odyssey spacecraft.

This image from NASA's 2001 Mars Odyssey spacecraft shows dune forms on the floor of Orson Welles Crater, an impact crater in the Coprates quadrangle named for the actor.

$This image from NASA's 2001 Mars Odyssey spacecraft shows lava flows terminating at the foot of canyon walls in Echus Chasma. These lava flows are also fractured into large plates in this region.$

Today's VIS image shows the southeastern portion of Micoud Crater. Micoud Crater is located in Vastitas Borealis. A small group of sand dunes is located on the floor of the crater, visible in the upper left portion of the image. Orbit Number 78913 Latitude 50.1533 Longitude 16.7858 Instrument VIS Captured 2019-09-29 00 35

Larger Landslide

Olympus Mons is surrounded by a steep escarpment called Olympus Rupes. This image from NASA's 2001 Mars Odyssey spacecraft shows this escarpment and lava flows that plunged over it.

Shadows cast by the high walls and high hills within Candor Chasma are visible in this image from NASA's 2001 Mars Odyssey spacecraft. The local time is near 5:00 in the afternoon.

Candor Chasma

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. Landslide deposits, layered materials and sand dunes cover a large portion of the chasma floor. This image is located in central Coprates Chasma. The floor of the chasma is covered by a complex deposit of material. This chaotic surface differs from most of the floor of the canyon and indicate a local process, perhaps a very large landslide or failure of the cliff face. 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.

Dunes forms top this sand sheet in the plains of Aonia Terra in this image captured by NASA's Mars Odyssey.

Sulci Collapse Pits

This image from NASA's 2001 Mars Odyssey shows the central portion of the complex caldera at the summit of Olympus Mons.

This image captured by NASA's Mars Odyssey shows a portion of Coprates Chasma.

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 84285 Latitude -44.1162 Longitude 34.3444 Instrument VIS Captured 2020-12-14 07 25

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. Landslide deposits, layered materials and sand dunes cover a large portion of the chasma floor. This image is located on the eastern side of Coprates Chasma, near Capri Chasma. The image shows multiple landslide features, which form lobed shaped deposits at the bottom of the canyon cliff face. Sand dunes are visible both on the landslide deposit and other parts of the canyon floor. 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 ent

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. Landslide deposits, layered materials and sand dunes cover a large portion of the chasma floor. This image is located in eastern Coprates Chasma. The plateau above the chasma is visible in this image. The cliff face is very steep, with the elevation dropping over 3 miles from the plateau to the canyon floor. Craters are relatively rare on the chasma floor, the one in this image is fairly large. The crater rim has affected winds in this region, causing the interior dunes within the crater as well as the dunes outside the crater rim. 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

Sirenum Fossae. Today's VIS image shows a portion of Sirenum 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 Sirenum Fossae graben are 2735km (1700 miles) long and stretch from eastern Terra Sirenum into western Daedalia Planum. Orbit Number 92416 Latitude -39.2691 Longit

This image near Athabasca Valles shows thin plate of lava as seen by NASA's 2001 Mars Odyssey spacecraft. This style of lava flow is very different from other lava flows in the nearby Elysium and Tharsis volcanic complexes.

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. Landslide deposits, layered materials and sand dunes cover a large portion of the chasma floor. This image is located in central Coprates Chasma. The image shows multiple landslide features, which form the bright lobed shaped deposits at the bottom of the canyon cliff face (top of image). The linear grooves on the top of the large landslide deposit were formed as the material came to rest on the canyon floor. The other features on the chasma floor are layered materials that have been weathered. 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

This image from NASA's Mars Odyssey covers a portion of the Medusa Fossae formation, near the equator of Mars. The most characteristic feature of the Medusa Fossae formation is the abundance of 'yardangs,' which are erosional landforms carved by wind.

Today's VIS image shows a small section of Mangala Valles. Mangala Valles is a complex channel more than 900km long (560 miles). The channel system starts near Mangala Fossae, a large tectonic feature that intersects the volcanic plains of Daedalia Planum. Like other channels in the region, Mangala Valles flows northward, eventually emptying into southern Amazonis Planitia. Orbit Number 83062 Latitude -6.77734 Longitude 209.123 Instrument VIS Captured 2020-09-04 15 21

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

The numerous, closely spaced channels in this image from NASA's 2001 Mars Odyssey spacecraft are part of Arda Valles.

This image from NASA's Mars Odyssey shows deposits in a crater located in Arabia Terra. Arabia is generally dust covered and dark streaks or dust avalanches are present in the crater walls.

$The fractures and channel-like features in this image are located in the Elysium Volcanic complex$

This old crater in Terra Sabaea has patterned floor material that is indicative of having a volitile component. At high latitudes the volitile is most likely ice

Tharsis Winds

Today's VIS image shows a portion of the immense volcanic flow fields in the Tharsis region. These flows are northeast of Ascraeus Mons. Orbit Number 81575 Latitude 16.1457 Longitude 264.928 Instrument VIS Captured 2020-05-05 04 57

These lava flows are part of Ascraeus Mons

This image captured by NASA's 2001 Mars Odyssey spacecraft shows part of the southern margin of Juventae Chasma.

The floor of Eos Chasma is composed of thousands of small hills; this type of terrain is called 'chaos.' This image from NASA's Mars Odyssey and shows a small portion of Eos Chaos.

Candor Chasma

his image shows part of the dune field near Meroe Patera. 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

This image from NASA's Mars Odyssey spacecraft shows the beginning of Pavonis Chasma (top of frame) on the northern flank of Pavonis Mons.

Today's VIS image shows a section of Bahram Vallis. This channel is located in northern Lunae Planum, south of Kasei Valles. Bharam Vallis drains from the higher elevations of Lunae Planum towards the Chryse Planitia basin. This channel is over 300km long (186miles). In this image Bahram Vallis enters Waspam Crater (right side of image) and then exits the crater (top right corner). Orbit Number 81374 Latitude 20.3853 Longitude 303.032 Instrument VIS Captured 2020-04-18 15 46

This VIS image covers part of Nilus Mensae. Located in the region where the northward flowing channel from Valles Marineris becomes the eastward flowing Kasei Valles, Nilus Mensae is a complex region of tectonic faulting and fluid flow features. In addition to the scoured surface, sand dunes are visible in depressions throughout the image. Orbit Number 78517 Latitude 21.6368 Longitude 286.455 Instrument VIS Captured 2019-08-27 09 50

$These linear fractures are part of Panchaia Rupes$

Aonia Terra Dunes (VIS)

This image captured by NASA's 2001 Mars Odyssey spacecraft continues to follow the channel seen in the past two images. The rover landing site is at the top margin of this image.

This image captured by NASA's 2001 Mars Odyssey spacecraft shows a small section of Reull Vallis.

This image from NASA's 2001 Mars Odyssey spacecraft shows some of the depressions in the material that fills Asimov Crater.

Tikhonravov Crater is a large, old crater in Terra Sabaea. The crater is pockmarked by numerous younger craters and other features. This image from NASA's Mars Odyssey shows a channel within Tikhonravov Crater.

These wind eroded hills are located on the southwest margin of Lycus Sulci

This image from NASA's 2001 Mars Odyssey spacecraft shows numerous large gullies dissect the inner rim of this unnamed crater in Noachis Terra.

This images shows part of the northeastern flank and margin of Pavonis Mons. Collapse features are common on the the margins of the Tharsis volcanoes along the vent axis

This VIS image shows a small section of Ma'adim Valles. Ma'adim Valles is an outflow channel that starts in the southern lowlands and flows northward into Gusev crater, the home of the MER Spirit rover. Located in Terra Cimmeria, the channel is 700km (435 miles) long, with widths up to 20 km (12 miles) and depths to 2 km (1.2 miles) in places. Orbit Number 82901 Latitude -24.5592 Longitude 176.226 Instrument VIS Captured 2020-08-22 09 06

Candor Chasma

The two depression crossing this image are called Pavonis Fossae and are located on the northern lower flank of Pavonis Mons. These linear features are most likely created by a combination of both tectonic and volcanic forces. The top feature has several narrow 'walls' within the depression, indicating a collapse of the roof of an empty lava tube. 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 (8.7 miles). Orbit Number 90136 Latitude 3.50046 Longitude 249.786 Instrument VIS Captured 2022-04-10 02 31

This VIS image shows part of the extensive volcanic flows in the Tharsis region. These flows are east of Ascraeus Mons. Orbit Number 81076 Latitude 11.2203 Longitude 261.313 Instrument VIS Captured 2020-03-25 02 50

This image shows the part of the southern cliff face of Hebes Chasma a the bottom of the image. At the top of the image is part of the large mesa located in the center of the chasma. Hebes Chasma is an enclosed basin not connected to Valles Marineris. The cliff faces of the chasma itself and the interior mesa appear quite different, which may provided information on how the chasma and the mesa formed. 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 wate

Landslide in a Crater

Ejecta Modification

This image captured by NASA's 2001 Mars Odyssey spacecraft shows a portion of Auqakuh Vallis, which dissects the northern margin of Terra Sabaea.

This image from NASA's 2001 Mars Odyssey spacecraft shows lava flows which have plunged over the steep escarpment marking the edge of Olympus Mons into the surrounding plains.

This image from NASA's 2001 Mars Odyssey shows a landslide deposit in Ophir Chasma.

Today's VIS image shows a portion of Shalbatana Vallis. Located in Xanthe Terra, Shalbatana Vallis is an outflow channel carved by massive floods of escaping groundwater whose source lies far to the south of this image. Shalbatana Vallis is over 1300 km long (808 miles). This channel, and all others in this region, drain into Chryse Planitia. A small landslide deposit is visible at the bottom of the image. Orbit Number 88187 Latitude 6.89989 Longitude 317.849 Instrument VIS Captured 2021-10-31 14 58

Orson Welles Crater Dunes

This image from NASA's 2001 Mars Odyssey spacecraft shows the complex surface on the northeastern flank of Arsia Mons. The channel-like features and collapse pits are likely all due to subsurface lava tubes.

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. Landslide deposits, layered materials and sand dunes cover a large portion of the chasma floor. This image is located in eastern Coprates Chasma, just east of the previous image. In this image, the lobate margins of several landslide deposits are easy to identify. This indicates the chaotic surface in yesterday's image are materials emplaced by landslides. The brighter features at the bottom of the image are layered materials. There are also dunes in the region with the layered deposits. 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 ye

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 landslide deposits in this VIS image from NASA's 2001 Mars Odyssey spacecraft are located in Valles Marineris and are called Coprates Labes.

The dune field in this image taken by NASA's 2001 Mars Odyssey is located on the floor of an unnamed crater east of Proctor Crater.

This image taken by NASA's 2001 Mars Odyssey spacecraft shows a landslide deposit on the southern rim of Candor Chasma.

Today's VIS image shows part of Clasia Vallis, located in Terra Sabaea. Clasia Vallis is 125km long (77 miles). Orbit Number 88720 Latitude 33.6222 Longitude 57.0277 Instrument VIS Captured 2021-12-14 12 25

It is sometimes difficult to figure out the history of the surface of Mars as seen in visible wavelength images. This image from NASA's 2001 Mars Odyssey is located on the northern margin of Hellas Basin and hints at a layered surface.

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. This image shows part of two of the summit calderas, each with a floor at different elevations. 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 re

Ophir Chasma Dunes

Reull Vallis

Aonia Terra Dunes

The linear features in this VIS image are graben called Sirenum Fossae. Graben are formed when blocks of material move downward between parallel faults. The faults were created by tectonic stresses in this region. The ground is pulling apart and breaks into faults, continued stress moves the sides of the faults further apart and form the graben. Orbit Number 75220 Latitude -31.3869 Longitude 208.356 Instrument VIS Captured 2018-11-28 20 39

The large mesa in the center of Hebes Chasma dominates this image. The top of the mesa is at the center of the image, with the cliff faces to the top and bottom of the image. The layering of the mesa is most easily identified in the lower part of the image. The long linear depression on the northern face indicate that wind action played a large part in eroding the mesa. 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 th

This VIS image is located on the western margin of Orcus Patera. Dark slope streaks are present on most ridges in the image. Formation of these features is linked to a change in the surface, either removal of the dusty surface revealing darker rock beneath the dust, or a volatile flow along the cliff face. Orbit Number 72545 Latitude 14.6915 Longitude 177.62 Instrument VIS Captured 2018-04-22 13 19

Gigas Sulci

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 from 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 layered materials and sand dunes. The image is located on the mid elevations on the south side of the canyon. 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

These sand dunes are located on the floor of an unnamed crater west of Hellas Basin

Located east of Eumenides Dorsum, this VIS image contains evidence of long term wind action and erosion. This area of Mars is dominated by poorly cemented surface material that is easily eroded by the wind. Unidirectional winds have created the linear ridge/valley system at the top half of this image. These features are called yardangs. Studies of this area propose volcanic ash eruptions from nearby volcanoes are the source of the surface material. Orbit Number 81078 Latitude -2.2665 Longitude 205.439 Instrument VIS Captured 2020-03-25 04 51

This image from NASA's Mars Odyssey spacecraft shows the western rim of Gale Crater. Several channels dissect the rim of the crater.

Dark slope streaks are common on the ridges of Lycus Sulci. These markings are thought to be formed by the removal of the brighter dust when material is shed from the top of the ridge. This image is from NASA's 2001 Mars Odyssey spacecraft.

This image shows the massive Olympus Mons flows at the basal escarpment

Sirenum Fossae. Today's VIS image shows a portion of Sirenum 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 Sirenum Fossae graben are 2735km (1700 miles) long and stretch from eastern Terra Sirenum into western Daedalia Planum. Orbit Number 92627 Latitude -27.7786 Longit

This image captured by NASA's 2001 Mars Odyssey spacecraft shows a small portion of Daedalia Planum.

Today's VIS image shows a section of Bahram Vallis. This channel is located in northern Lunae Planum, south of Kasei Valles. Orbit Number 71256 Latitude 21.0762 Longitude 301.486 Instrument VIS Captured 2018-01-06 08 51

This VIS image shows the intersection of Mangala Fossae and an impact crater. Mangal Fossae is a long linear depression called a graben, and was formed due to extensional tectonic stresses. In this image the graben crosses through a crater. Impact crater formation changes the surface and near surface materials, usually creating much stronger rocks due to the melting of the preexisting surface. The extensional stresses forming the graben interacted with this material and produced the jumble of depressions we see today within the crater. Orbit Number 82251 Latitude -19.3232 Longitude 207.574 Instrument VIS Captured 2020-06-29 20 38

Taken by NASA's 2001 Mars Odyssey spacecraft, this image shows a small portion of the floor of Capri Chasma. Bright layered deposits and dunes are visible.

Layers in Meridiani Planum

Today's VIS image shows a section of Labou Vallis. Labou Vallis is located south of Eumenides Dorsum and is 258 kilometers (160 miles) long. The 'tail' of the tear-dropped shaped island in the center of the channel points downstream, indicating the liquid flow was towards the top of this image. Orbit Number 90200 Latitude -7.83684 Longitude 204.926 Instrument VIS Captured 2022-04-15 08 56

Dark slope streaks are common throughout Lycus Sulci as seen by NASA's 2001 Mars Odyssey spacecraft.

This image of Moreux Crater is dominated by the central peak. There are sand dunes on the right side of the image. The part of the peak with a pitted surface texture and curvilinear ridges has been interpreted to be created by glacial flows. Moreux Crater is located in northern Arabia Terra and has a diameter of 138 kilometers. 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

$The fractures in this image taken by NASA's 2001 Mars Odyssey spacecraft are part of Cerberus Fossae.$

This image NASA's 2001 Mars Odyssey spacecraft shows part of the dune field on the floor of Brashear Crater.

Kasei Vallis Erosion

of 3