Mars Geological Features

High-resolution images from Mars showcasing diverse geological formations and textures, offering insights into the planet's surface and history.

Ares Vallis Cataract
Ares Vallis Cataract
305 assets in this story
6145-58971702
Today's VIS image shows part of the floor of Firsoff Crater. Located in Arabia Terra, Firsoff Crater, and the neighboring Crommelin Crater, contain large layered deposits on the crater floor. The north side of the smaller crater at the bottom of the image shows the layering. Wind action has modified the deposit. Firsoff Crater is 90 km in diameter (56 miles). Orbit Number 94812 Latitude 2.77617 Longitude 350.268 Instrument VIS Captured 2023-04-30 02 58
6145-44811022
This image captured by NASA's 2001 Mars Odyssey spacecraft is part of Tithonium Chasma, part of the western side of Valles Marineris.
6145-44622748
Where Ophir Meets Candor
6145-44675635
Ares Vallis Cataract
6145-44493272
Claritas Fossae. Located between the lava plains of Daedalia Planum and Solis Planum, Claritas Fossae is a graben filled highland. Graben are formed by tectonic activity, where extensional forces stretch the surface allowing blocks of material to slide down between paired faults. These linear grabens are termed fossae. This region of Mars had very active tectonism and volcanism, resulting in the huge volcanos like Arsia Mons and deep chasmata of Valles Marineris. Claritas Fossae was formed prior to the large lava flows of the Tharsis region. Orbit Number 91446 Latitude -36.8955 Longitude 262.397 Instrument VIS Captured 2022-07-26 23 05
6145-44975851
This image captured by NASA's 2001 Mars Odyssey spacecraft shows part of the floor of Coprates Chasma, including a large sand sheet and smaller dunes.
6145-44637158
This image captured by NASA's 2001 Mars Odyssey spacecraft shows a small portion of Iani Chaos. The brighter floor material is being covered by sand, probably eroded from the mesas of the Chaos.
6145-44841828
This image captured NASA's Mars Odyssey shows part of a landslide deposit in Melas Chasma.
6145-45122775
This image captured by NASA's 2001 Mars Odyssey spacecraft shows part of the canyon wall of Melas Chasma.
6145-45099279
This image captured by NASA's 2001 Mars Odyssey spacecraft shows part of a complex region of channels which dissect the margin of Arabia Terra where elevations lower into Acidalia Planitia.
6145-45116810
This image captured by NASA's 2001 Mars Odyssey spacecraft shows part of the floor of Gusev Crater.
6145-45258879
This image shows the north central cliff face of Hebes Chasma. The cliff face and downslope movement of material is very different in appearance than the same features of the large mesa in the center of the chasma. Hebes Chasma is an enclosed basin not connected to Valles Marineris. The Odyssey spacecraft has spent over 15 years in orbit around Mars, circling the planet more than 69000 times. It holds the record for longest working spacecraft at Mars. THEMIS, the IR/VIS camera system, has collected data for the entire mission and provides images covering all seasons and lighting conditions. Over the years many features of interest have received repeated imaging, building up a suite of images covering the entire feature. From the deepest chasma to the tallest volcano, individual dunes inside craters and dune fields that encircle the north pole, channels carved by water and lava, and a variety of other feature, THEMIS has imaged them all. For the next several months the image of the day
6145-44484664
This VIS image shows layering of surface materials in Meridiani Planum. TES (Thermal Emission Spectrometer) initially detected hematite in a surface layer, which was confirmed by THEMIS (THrmal EMision Imaging System). These findings supported a water rich origin of the hematite and led to the selection of the site for the Opportunity MER (Mars Exploration Rover). The TES instrument was located on the Mars Global Surveyor spacecraft. THEMIS is onboard the Mars 2001 Odyssey spacecraft. Orbit Number 89658 Latitude 1.83323 Longitude 0.267191 Instrument VIS Captured 2022-03-01 17 54
6145-45261466
This image shows the eastern portion of Hebes Chasma. The ridge that is casting a shadow at the bottom of the image is likely a large tectonic fault. All of the materials on the floor of the chasma are from the cliff faces. The deposition and erosion of the materials in this image are very different from the those of the large central 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 the north pole, channels carved
6145-44795363
This NASA 2001 Mars Odyssey image shows part of the floor of Coprates Chasma.
6145-45077586
Lava flows of Daedalia Planum can be seen at the top and bottom portions of this image from NASA's 2001 Mars Odyssey spacecraft. The ridge and linear depression in the central part of the image are part of Mangala Fossa, a fault bounded graben.
6145-45258373
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 brighter materials at the bottom of the image are layered deposits. It is unknown how deep these canyon deposits were when they formed. The layering is only visible due to erosion, making it difficult to estimate the original thickness. While layered deposits can be found on the floor of Coprates Chasma, they are most commonly found along the lower elevations and at the bottom of the cliff faces in the canyon. 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 pr
6145-44483928
Today's VIS image shows part of Gale Crater, including the large layered deposit on the crater floor. The Curiosity Rover is located in Gale Crater. Gale crater is 150km (90 miles) in diameter. Orbit Number 88942 Latitude -4.53543 Longitude 137.674 Instrument VIS Captured 2022-01-01 18 55
6145-44946742
This image captured by NASA's 2001 Mars Odyssey spacecraft shows a landslide deposit in Ganges Chasma.
6145-44831718
Small unnamed channels drain the surface in this region of Arabia Terra were captured by NASA's Mars Odyssey on August 3, 2010.
6145-44663082
The two landslides in this image are located in Aeolis Mensae
6145-44484668
Today's VIS image shows a small portion of the immense lava flows that originated from Arsia Mons. Arsia Mons is the southernmost of the three large aligned volcanoes in the Tharsis region. Arsia Mons' last eruption was 10s of million years ago. 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 (111 miles). For comparison the longest Hawaiian lava flow is only 51 km (˜31 miles) long. The total area of Daedalia Planum is 2.9 million square km - more than four times the size of Texas. Orbit Number 90723 Latitude -23.0254 Longitude 238.572 Instrument VIS Captured 2022-05-28 10 23
6145-44576471
This image, taken by NASA's Mars Odyssey spacecraft, shows a cratered highland region called Arabia Terra. The center right side of the image shows a branch of the valley network Naktong Vallis cutting into the eastern rim of an unnamed crater.
6145-45263587
Multiple gullies dissect the rim of this unnamed crater in Terra Cimmeria. Orbit Number 74480 Latitude -49.7019 Longitude 140.533 Instrument VIS Captured 2018-09-28 22 24
6145-44663903
This images shows part of the main channel of Mamers Vallis as well as one of it's tributaries
6145-44622760
Ophir Chasma Etched Rock
6145-44892293
This image from NASA's 2001 Mars Odyssey spacecraft is of Lycus Sulci, located on the western side of Olympus Mons and dominated by multi-direction ridges which contains material less resistant than the ridges to the effects of wind.
6145-44988247
The arcuate or curved fractures in this image are located on the eastern margin of Elysium Planitia as seen by NASA's 2001 Mars Odyssey spacecraft.
6145-44672076
Melas Chasma
6145-45035312
A small section of Dao Vallis in shown in this image from NASA's 2001 Mars Odyssey spacecraft. Dao Vallis is a major channel that drains into Hellas Planitia.
6145-44656113
This interesting tributary channel is located in the Deuteronilus region of Mars
6145-44666265
These large landslides are located in Ganges Chasma
6145-44925419
This image shows numerous gullies that dissect the rim of Bunge Crater as seen by NASA's 2001 Mars Odyssey spacecraft.
6145-44607017
Meridiani Planum
6145-44512192
This VIS image shows several channels located in Terra Sabaea. The flow was from the top of the image towards the bottom. These channels are located north of Hellas Planum and are following the topographic gradient down into the Hellas basin. None of these channels have been named. Orbit Number 81919 Latitude -17.5776 Longitude 65.3522 Instrument VIS Captured 2020-06-02 12 33
6145-44597419
Lycus Sulci
6145-45080155
Numerous channels dissect the rim of Lohse Crater, as shown in this image captured by NASA's 2001 Mars Odyssey spacecraft.
6145-44656611
These ridges and channeled lows are part of Sulci Gordii
6145-44484412
Today's VIS image shows part of the large hill near the eastern edge of Candor Chasma. Layering is visible toward the bottom of the image. The sides of the hill are deeply incised by erosion, probably including both wind and water processes. 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. 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 88687 Latitude -7.91852 Longitude 294.829 Instrument VIS Captured 2021-12-11 18 58
6145-45027089
A large sandsheet with surface dune forms is shown in this image of Aonia Terra captured by NASA's 2001 Mars Odyssey spacecraft.
6145-44640690
This interesting deposit is located on the floor of Becquerel Crater
6145-44605646
Hematite Outlier and Sand Dunes
6145-45292206
Today's VIS image shows a small portion of the immense lava flows that originated from Arsia Mons. Arsia Mons is the southernmost of the three large aligned volcanoes in the Tharsis region. Arsia Mons' last eruption was 10s of million years ago. 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 84016 Latitude -23.1326 Longitude 237.739 Instrument VIS Captured 2020-11-22 03 44
6145-45263328
This VIS image shows part of the wall and floor of Coprates Chasma. Several landslide deposits are visible as well as small regions of sand dunes. Orbit Number 71992 Latitude -14.4199 Longitude 302.56 Instrument VIS Captured 2018-03-07 23 50
6145-45260408
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. Today's image of the southern section of the canyon shows a large region of sand dunes. The presence of dunes indicates wind action as the most recent geologic process modifying 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 i
6145-45292210
Today's VIS image shows part of Ariadnes Colles. The term colles means hills or knobs. The hills appear brighter than the surrounding lowlands, likely due to relatively less dust cover. Ariadnes Colles is located in Terra Cimmeria. Orbit Number 84305 Latitude -36.9669 Longitude 178.644 Instrument VIS Captured 2020-12-15 22 54
6145-44821011
Located near Amazonis Mensa, this region of Mars has undergone erosion by wind. Long linear hills being created by the wind are called yardangs in this image from NASA's 2001 Mars Odyssey.
6145-44685152
Candor Chasma
6145-45265408
This VIS image shows a small portion of Daedalia Planum. The lava flows in this image originated at Arsia Mons. Individual flows have lengths up to almost 180km (~111 miles). The longest Hawaiian lava flow is only 51km (~31 miles). The area of Daedalia Planum is 2.9 million square km - more than 4 times the size of Texas. Orbit Number 75431 Latitude -18.9209 Longitude 241.546 Instrument VIS Captured 2018-12-16 05 39
6145-44483814
The three large aligned Tharsis volcanoes are Arsia Mons, Pavonis Mons and Ascreaus Mons (from south to north). There are collapse features on all three volcanoes, on the southwestern and northeastern flanks. This alignment may indicate a large fracture/vent system was responsible for the eruptions that formed all three volcanoes. This VIS image shows part of the southern flank of Arsia Mons, along the center of the aligned fracture system. The scalloped depressions are most likely created by collapse of the roof of lava tubes. Lava tubes originate during eruption event, when the margins of a flow harden around a still flowing lava stream. When an eruption ends these can become hollow tubes within the flow. With time, the roof of the tube may collapse into the empty space below. The tubes are linear, so the collapse of the roof creates a linear depression. In this region, the complexity of the collapse and faulting has created a unique surface. This region has collapse depressions with
6145-44981543
This image captured by NASA's 2001 Mars Odyssey spacecraft shows a small portion of the lava flows that comprise Daedalia Planum.
6145-44973791
This image from NASA's 2001 Mars Odyssey spacecraft shows part of Coprates Chasma, which is just one part of the extensive Valles Marineris canyon system.
6145-44531802
Today's VIS image shows a small section of Nirgal Valles. Located in Noachis Terra, Nirgal Valles is 610km long (379 miles). Orbit Number 83302 Latitude -27.1434 Longitude 315.095 Instrument VIS Captured 2020-09-24 08 50
6145-44864828
This image from NASA's 2001 Mars Odyssey shows a few of the many channels named (in this case Arda Valles) and unnamed that empty into a large low in Margaritifer Terra.
6145-52930336
Crater Dunes. This VIS image shows a large sand sheet with surface dune forms as well as smaller sand dunes within an unnamed crater in Noachis Terra. These dunes are composed of basaltic sand that has collected in the bottom of the crater. The topographic depression of the crater forms a sand trap that prevents the sand from escaping. Dune fields are common in the bottoms of craters on Mars and appear as dark splotches that often lean up against the downwind walls of the craters. Dunes are useful for studying both the geology and meteorology of Mars. The sand forms by erosion of larger rocks, but it is unclear when and where this erosion took place on Mars or how such large volumes of sand could be formed. The dunes also indicate the local wind directions by their morphology. Orbit Number 92028 Latitude -48.9171 Longitude 34.0952 Instrument VIS Captured 2022-09-12 21 08 https //photojournal.jpl.nasa.gov/catalog/PIA25742
6145-45092601
This image captured by NASA's 2001 Mars Odyssey spacecraft shows part of the dune field on the floor of Proctor Crater.
6145-44672293
Layered Deposits in Aureum Chaos
6145-44965131
This image from NASA's Mars Odyssey spacecraft shows a small section of Samara Valles.
6145-44812841
The lava flows in this image taken by NASA's 2001 Mars Odyssey spacecraft are part of the extensive flow field of Arsia Mons.
6145-44484710
Today's VIS image is located between the main part of Coprates Chasma (north) and Coprates Catena (south). The canyon in this area is much shallower than the main canyon. Coprates Chasma is one of the numerous canyons that make up Valles Marineris. The chasma stretches for 960 km (600 miles) from Melas Chasma to the west and Capri Chasma to the east. Orbit Number 90883 Latitude -15.0445 Longitude 301.518 Instrument VIS Captured 2022-06-10 14 37
6145-44913454
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.
6145-44834779
This image from NASA's Mars Odyssey shows a region on the north end of Gordii Dorsum. Wind is the main source of erosion in this region, so the unusual texture may indicate that the surface material in this region is different from nearby regions.
6145-45260704
This image shows the part of the northern cliff face of Hebes Chasma at the top of the image. The linear features aligned diagonally across the top of the image are large faults. These faults may have been created at the same time that the chasma formed. The materials seen at the bottom half of this image are part of the erosion of the central mesa. The layered material of the mesa appear to have been eroded by both wind and water action. 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 vol
6145-44962219
This image from NASA's Mars Odyssey spacecraft shows some of the extensive lava flows that originate at Arsia Mons.
6145-58965922
Elator Vallis, the channel shown in image from NASA's Mars Odyssey, runs on the plains of Aurorae Planum. This portion of Elator Vallis parallels Ganges Chasma (shown in the top of the image).
6145-44967364
Do you see what I see this image from NASA's Mars Odyssey spacecraft Turn your head to the left and look at the crater at the top of the image - a smiley face will be gazing at you.
6145-45297730
This VIS image shows part of the Tharsis lava plains between Sulci Gordii and Ulysses Fossae. While large volcanoes and huge lava flow sheets dominate the Tharsis region, extensive tectonic features are also present. The entire Tharsis region forms a bulge on the equatorial part of Mars, generated by the uplift of magma rising through the crust. The motion of subsurface magma created extensional forces, tearing the surface apart releasing the magma in floods of lava and volcano building events. At the same time the extension cracked the surface creating the faults and graben also seen in the region. In this image, the linear graben post-date the lava flows. Orbit Number 78394 Latitude 17.6427 Longitude 235.778 Instrument VIS Captured 2019-08-17 06 43
6145-52930290
Kaiser Crater Dunes. This VIS image is located in Kaiser Crater and shows many individual dunes. This sand dune field is one of several regions of sand dunes located on the southern part of the crater floor. The crater floor is visible between the dunes, indicating that there is a limited sand supply creating the dunes. These dunes are composed of basaltic sand that has collected in the bottom of the crater. The topographic depression of the crater forms a sand trap that prevents the sand from escaping. Dune fields are common in the bottoms of craters on Mars and appear as dark splotches that often lean up against the downwind walls of the craters. Dunes are useful for studying both the geology and meteorology of Mars. The sand forms by erosion of larger rocks, but it is unclear when and where this erosion took place on Mars or how such large volumes of sand could be formed. Local winds continue to move the sand dunes across the crater floor. There are two sides to a dune, the low angl
6145-44679935
Huygens Crater
6145-44965968
This image from NASA's Mars Odyssey spacecraft shows the eastern part of Hydrae Chasma.
6145-44493007
Kaiser Crater Dunes. This VIS image shows part of the floor of Kaiser Crater. Kaiser Crater is 207 km (129 miles) in diameter and is located in Noachis Terra west of Hellas Planitia. This sand dune field is one of several regions of sand dunes located on the southern part of the crater floor. The image also shows the complex crater floor beneath the dunes. Orbit Number 91155 Latitude -46.9828 Longitude 19.3481 Instrument VIS Captured 2022-07-02 23 58
6145-45262500
This VIS image is located near Zephyria Planum. Winds of two different directions have excavated a poorly cemented surface into linear ridge features called yardangs. Examining the structure of the ridges, it appears that winds first blew from the upper left of the image. Then perhaps after a change in climate, winds blew toward the upper right, carving a new pattern on top of the older one. The ridges are not perpendicular, but intersect at a wider angle. Orbit Number 72496 Latitude -4.75332 Longitude 154.461 Instrument VIS Captured 2018-04-18 12 20
6145-44658150
Aram Chaos contains several layers of fill material
6145-44585228
The jumble of eroded ridges and mesas seen in this NASA Mars Odyssey image occurs within Ares Vallis, one of the largest catastrophic outflow channels on the planet. Floods raged through this channel, pouring out into the Chryse Basin to the north.
6145-44594953
Volcano Vents
6145-44702002
Hellas Basin
6145-44769642
Dark slope streaks are common in Lycus Sulci in this 2001 Mars Odyssey THEMIS VIS image.
6145-45091515
This image captured by NASA's 2001 Mars Odyssey spacecraft shows gullies on the inner rim of an unnamed crater in Noachis Terra.
6145-44982416
Several different surface textures are present on the lower elevations of Iani Chaos in this image from NASA's 2001 Mars Odyssey spacecraft.
6145-45260179
This image shows the northern side of Hebes Chasma. The large central layered mesa is just off the bottom of the image. Meeting in approximately the center of the image are materials eroded from the cliff face and mesa. The appearance of the material differs. Both the floor and central mesa are very complex features in this canyon. Hebes Chasma is an enclosed basin not connected to Valles Marineris. The Odyssey spacecraft has spent over 15 years in orbit around Mars, circling the planet more than 69000 times. It holds the record for longest working spacecraft at Mars. THEMIS, the IR/VIS camera system, has collected data for the entire mission and provides images covering all seasons and lighting conditions. Over the years many features of interest have received repeated imaging, building up a suite of images covering the entire feature. From the deepest chasma to the tallest volcano, individual dunes inside craters and dune fields that encircle the north pole, channels carved by water
6145-45266688
This fracture system is called Elysium Chasma. Located west of Elysium Mons, it is just one of many large fractures in the Elysium volcanic complex. Orbit Number 77711 Latitude 23.285 Longitude 140.982 Instrument VIS Captured 2019-06-22 00 54
6145-45047437
This image captured by NASA's 2001 Mars Odyssey spacecraft shows dust devil tracks covering most of the surface in this region of Utopia Planitia.
6145-44844204
Constant sand-blasting by the winds on Mars have eroded and sculpted the surface in the equatorial region around Medusae Fossae in this image captured by NASA's Mars Odyssey.
6145-44619143
Yardang Development
6145-45264104
This VIS image shows a small portion of the floor of Galle Crater. This large crater is located on the eastern side of Argyre Planitia. The floor of Galle Crater contains many different features, including fluvial, glacial and aeolian derived products. The steep crater rim is toward the bottom of the image. The incised, flat laying materials at the top of the image are probably eroded layered deposits. Orbit Number 74804 Latitude -52.1339 Longitude 329.267 Instrument VIS Captured 2018-10-25 14 28
6145-44626729
Platy Lava Surface
6145-45057348
The complex channel in this image captured by NASA's 2001 Mars Odyssey spacecraft is part of Olympica Fossae, and was most likely formed by the flow of lava.
6145-44665354
This image shows part of one of the many mesas that comprise Deuteronilus Mensae as well as the surrounding debris slope and plains surface
6145-44601422
Central Peak
6145-45299046
This VIS image shows part of the southern 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 81537 Latitude -11.3482 Longitude 284.901 Instrument VIS Captured 2020-05-02 01 42
6145-45112898
This image captured by NASA's 2001 Mars Odyssey spacecraft is located in a region that has been heavily modified by wind action.
6145-45298265
Today's VIS image shows one of several craters located on the floor of the much larger Tikhonravov Crater in Terra Sabaea. Named for Russian rocket scientist, Mikhail Tikhonravov, the crater is thought to have been the location of a large lake, which may have laid down layers of material now exposed on the margins of this pedestal crater. A pedestal crater is formed by removal of surface materials around a resistant layer of ejecta, eventually leaving the crater and ejecta as a mesa or plateau on the lower elevation base surface. Orbit Number 78401 Latitude 12.9296 Longitude 34.4892 Instrument VIS Captured 2019-08-17 20 32
6145-45258176
The interior layered mesa in Hebes Chasma is visible at the top of this image. The southern cliff face is at the bottom. A landslide deposit is visible originating from the southern cliff face. Hebes Chasma is an enclosed basin not connected to Valles Marineris. The Odyssey spacecraft has spent over 15 years in orbit around Mars, circling the planet more than 69000 times. It holds the record for longest working spacecraft at Mars. THEMIS, the IR/VIS camera system, has collected data for the entire mission and provides images covering all seasons and lighting conditions. Over the years many features of interest have received repeated imaging, building up a suite of images covering the entire feature. From the deepest chasma to the tallest volcano, individual dunes inside craters and dune fields that encircle the north pole, channels carved by water and lava, and a variety of other feature, THEMIS has imaged them all. For the next several months the image of the day will focus on the Tha
6145-44860155
This image from NASA's 2001 Mars Odyssey shows a huge ridge of sand in Russell Crater that makes its dune field one of the most unusual on Mars.
6145-44685129
Another Noctis
6145-44623829
Candor Chasma
6145-58971862
The large sand sheet with surface dune forms seen in this VIS image is 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. This crater morphology is unique to Rabe Crater. Rabe Crater is located in Noachis Terra and is 108km in diameter (67 miles). Orbit Number 83505 Latitude -43.6272 Longitude 34.5903 Instrument VIS Captured 2020-10-11 02 34
6145-45264071
This VIS image shows part of Ares Vallis, one of the large channels in Margaritfer Terra that empty into Chryse Planitia. Orbit Number 72477 Latitude 5.49596 Longitude 341.524 Instrument VIS Captured 2018-04-16 22 49
6145-45297726
The lower elevation on the left side of this VIS image is part of Memnonia Sucli. The higher elevations to the right are on the upper part of a mesa that bounds the sulci. The image shows some of the extensive wind etched terrain in Memnonia Sulci, located south west of Olympus Mons. The linear ridges are called yardangs and form by wind removal of semi-cemented material. The ridges are parallel to wind direction, so the predominate winds that created the yardangs in this image blew NE/SW. Orbit Number 78296 Latitude -7.8302 Longitude 186.694 Instrument VIS Captured 2019-08-09 04 54
6145-44644086
These linear clouds are just one of many storm fronts that occurred near the south pole during the late southern summer season