Mars Terrain Exploration

High-resolution images from Mars showcasing diverse geological features like valleys, craters, and chaotic terrains captured by spacecraft.

Channels

Dark dunes on the floor of an interior crater in Becquerel, imaged here by NASA's Mars Odyssey spacecraft, supply the sand responsible for the erosion of the remarkable, layered deposit to the south.

These lava flows are associated with Ascraeus Mons

This crater and surrounding channels are part of Kasei Vallis

The linear depression in this VIS image is part of Sirenum Fossae. Depressions of this type are called graben, which form by the down drop of material between two parallel faults. The faults are caused by tectonic stresses in the region. The Sirenum Fossae graben are 2735km (1700 miles) long. Orbit Number 84067 Latitude -32.5029 Longitude 205.188 Instrument VIS Captured 2020-11-26 08 34

These streamers of clouds cross over a small crater without deflection

Showing the area just slightly west of the previous image, the large region of sand and sand dunes are the dark area that dominates this image captured by NASA's 2001 Mars Odyssey spacecraft.

This image shows a section of Nirgal Vallis. In this image a crater has been formed across the vallis. The crater formation postdates the channel formation.

This VIS image shows lava flows from Alba Mons, and a tectonic graben called Cyane Fossae. It is thought that the linear depressions that surround Alba Mons were created by a huge volcanic eruption followed by the collapse of the volcano into the underlying empty magma chamber. Orbit Number 77146 Latitude 31.4715 Longitude 241.52 Instrument VIS Captured 2019-05-06 12 18

Only a portion of a large landslide deposit is shown in this image taken by NASA's 2001 Mars Odyssey spacecraft. The landslide occurred on the rim of an unnamed crater southwest of Holden Crater.

This VIS image is located in Terra Cimmeria, near the margin with Nepenthes Mensae. The highlands of Terra Cimmeria are at the bottom of the image. Tectonic activity has created fault blocked regions along the highland boundary. With time and erosion, the blocks become isolated mesas, and then the low hills of Nepenthes Mensae. Orbit Number 78685 Latitude 1.97703 Longitude 122.103 Instrument VIS Captured 2019-09-10 05 44

Multiple overlapping lobes of ejecta are visible in this image of an unnamed crater in Chryse Planitia as seen by NASA's 2001 Mars Odyssey spacecraft.

This VIS image shows Gasa Crater located on the floor of a larger unnamed crater Eridania Planitia. Gullies dissect the rims of both craters. Orbit Number 76121 Latitude -35.639 Longitude 129.538 Instrument VIS Captured 2019-02-11 01 31

This image of the flank of Ascraeus Mons shows several individual flows where the sides are higher than the center. These are called leveed flows, as the outer margin acts as a levee containing the flow as it continues downslope. Levees grow as the flow margins start to cool. The hotter liquid lava continues as long as the source flows. 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

These lava flows originated at Arsia Mons. This image is from NASA's 2001 Mars Odyssey spacecraft.

Reull Vallis. This VIS image shows a short section of Reull Vallis. Reull Vallis starts in Promethei Terra and empties into Hellas Plainitia. Reull Vallis is 1051km (653 miles) long. Orbit Number 92169 Latitude -41.0221 Longitude 107.284 Instrument VIS Captured 2022-09-24 11 18 https //photojournal.jpl.nasa.gov/catalog/PIA25750

This VIS image is located in Melas Chasma. The linear and arcuate features are on the surface of a large landslide. This region of Melas Chasma is covered by several very large landslide deposits. Melas Chasma is part of the largest canyon system on Mars, Valles Marineris. At only 563 km long (349 miles) Melas is not the longest canyon, but it is the widest. Located in the center of Valles Marineris, it has depths up to 9,000 meters (30,000 feet) from the surrounding plains. In addition to landslide deposits, there are 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 78255 Latitude -10.9711 Longitude 290.017 Instrument VIS Captured 2019-08-05 19 51

This crater is located on the flank of Ascraeus Mons

The channel in this image is called Apsus Vallis and it is located near the Elysium volcanic complex. Lava may have played a part in the formation of Apsus Vallis

Gullies

The diffuse streaks of white in this VIS image are clouds. These are high altitude winter clouds over Melas Chasma. Streamers of clouds like this are moving very quickly in high altitude winds. Orbit Number 88213 Latitude -11.5665 Longitude 290.207 Instrument VIS Captured 2021-11-02 18 14

This VIS image shows part of an unnamed crater on the northwest margin of Daedaia Planum. Lava flows are visible around the crater rim. The interior of the crater has been filled by a material that is now being eroded to create the ridge and valley formation at the upper left part of the image. Orbit Number 72793 Latitude -4.58437 Longitude 222.433 Instrument VIS Captured 2018-05-12 23 30

Deuteronlius Mensae Central Peak

Moving further east, we see more dunes. This image captured by NASA's 2001 Mars Odyssey spacecraft shows more of the crater rim and the crater floor seen in the image is not as smooth as in other parts of the crater.

Marte Vallis

A small delta is located in this unnamed crater near Nili Fossae.

Hebes ILD

This image shows a portion of the southern flank of Olympus Mons

Crater Dunes

Crater Dunes

Meridiani Craters

This image from NASA's Mars Odyssey spacecraft shows the westward continuation of the channel from yesterday's image. Note how the channel widens as it moves downslope (to the west).

The lava flows in this image captured by NASA's 2001 Mars Odyssey spacecraft are located on the northeastern margin of Daedalia Planum. Wind deposits are visible in the lee of the flow fronts.

Today's VIS image shows a small section on Margaritifer Chaos. The term chaos is applied to regions where the surface is being eroded to form mesas. As the surface processes continue individual mesas become more isolated and take on the appearance of regions of hills. At the top of the image is Margaritifer Terra, which is being dissected into large mesas. Towards the bottom of the image the mesas have been eroded into smaller hills. Orbit Number 89010 Latitude -7.22948 Longitude 336.24 Instrument VIS Captured 2022-01-07 09 17

The small channel in this image captured by is located in volcanic flows in the northern part of Tractus Fossae.

Arsia Mons Flows

Hole-y Smokes!

This VIS image is located in Utopia Planitia and shows part of Hephaestus Fossae. Hephaestus Fossae is a complex channel system. It has been proposed that the channel formed by the release of melted subsurface ice during the impact event that created a large crater in the center 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 81767 Latitude 17.6969 Longitude 125.709 Instrument VIS Captured 2020-05-21 00 22

Lava Tube Collapse Pits

The channel in this VIS image is located on the western margin of Medusae Fossae. Orbit Number 78907 Latitude -5.87425 Longitude 198.259 Instrument VIS Captured 2019-09-28 12 25

Today's VIS image shows a portion of the northern flank of Ascraeus Mons. Ascraeus Mons is the northernmost of the three large aligned Tharsis volcanoes. All three have extensive flank deposits along the northeast/southwest trend connecting the volcanoes. In today's image volcanic lava flows are visible along with tectonic features and collapse features. Collapse into underlying lava tubes will create a what looks like a series of craters along a tectonic trend. Orbit Number 79404 Latitude 15.2404 Longitude 256.725 Instrument VIS Captured 2019-11-08 10 44

Streamlined Hills of Maja Vallis

This image by NASA's Mars Odyssey spacecraft shows Utopia Planitia, a large plain in the northern hemisphere of Mars. It is believed that this basin is the result of a large impact.

This image captured by NASA's 2001 Mars Odyssey spacecraft shows a portion of Hebrus Valles. This channel system was formed by liquid flow of either water or lava, or a combination of both.

$This image from NASA's Mars Odyssey shows the cratered highlands of Terra Cimmeria. The image contains several long troughs of Sirenum Fossae running primarily from left to right. These features are parallel to semi-parallel fractures called graben.$

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. This VIS image shows the ridge forms that are typical of this region. Orbit Number 94904 Latitude 19.3247 Longitude 213.937 Instrument VIS Captured 2023-05-07 16 52

Today's VIS image shows a single linear depression, most likely a graben. This region is located just south of Cerberus Fossae, so it may have formed at the same time. Several Cerberus Fossae graben have also been source regions for flow features. Orbit Number 94756 Latitude 7.92391 Longitude 165.118 Instrument VIS Captured 2023-04-25 12 20

This image captured by NASA's 2001 Mars Odyssey spacecraft shows lava flows near the eastern flank of Pavonis Mons.

Floor of Becquerel Crater

Channels

Rayed Gratteri Crater

This 2001 Mars Odyssey THEMIS VIS image shows a portion of Nirgal Vallis and a scalloped tributary channel.

$The northern margin of Terra Sabaea is a complex area between a cratered highland and complexly eroded lower plains. This VIS image of the region shows just one of the numerous unnamed channels. The 90 degree bends indicate tectonic fractures have played a part in the channel formation. Orbit Number 71863 Latitude 32.1944 Longitude 59.4512 Instrument VIS Captured 2018-02-25 09 02$

Floor of Chia Crater

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

Terra Sabaea

Today's VIS image shows a crater on Hephaestus Fossae. The crater is fairly young, as there is only minimal modification of the crater floor. While it appears that the crater sits of top of the channel, the creation of the crater may have also created the channel. The impact event would have caused subsurface heating, melting any subsurface ice in the region which would have created surface flow to form the channel. Orbit Number 72447 Latitude 17.8067 Longitude 125.698 Instrument VIS Captured 2018-04-14 11 35

Arabia Terra Crater

The windstreak in this image from NASA's 2001 Mars Odyssey is located on lava flows from Arsia Mons.

Today's VIS image shows a small section of Nirgal Valles. Located in Noachis Terra, Nirgal Valles is 610km long (379 miles). Orbit Number 83514 Latitude -28.1171 Longitude 319.016 Instrument VIS Captured 2020-10-11 16 26

This image from NASA's 2001 Mars Odyssey spacecraft shows two craters located in the northern lowlands.

These yardangs are being formed by wind erosion of the Memnonia Sulci deposits

This image captured by NASA's 2001 Mars Odyssey shows a portion of the northeastern flank of Ascraeus Mons.

Multidepth Channels

Infilled Crater

Flow Complexity

Gullies in Trough near Gorgonum Chaos

Just north of the hematite deposit in Meridiani Planum, the remnants of a formerly extensive layer of material remain as isolated knobs and buttes in this image from NASA's Mars Odyssey spacecraft.

Meridiani Planum

This image shows a different portion of the collapse features located on the northern flank of Ascraeus Mons as seen by NASA's 2001 Mars Odyssey spacecraft.

The fill material on the floor of this crater looks a bit like a flower

Today's VIS image shows a portion of the flank of Albor Tholus, a volcano found in the Elysium volcanic complex. The caldera of the volcano is very deep compared to it's height. The top elevation of Albor Tholus is approximately 4.5km, the deepest part of the caldera measures 3km below this an elevation of only 1.5km. Orbit Number 77798 Latitude 18.4758 Longitude 151.507 Instrument VIS Captured 2019-06-29 04 49

This image captured by NASA's 2001 Mars Odyssey spacecraft shows part of Cyane Fossae, located near Alba Mons.

Orthogonal Ridges

This image, taken by NASA's 2001 Mars Odyssey spacecraft, shows a small section of Nirgal Vallis.

Today's VIS image shows a section of Scamander Vallis. Scamander Vallis is located in northern Terra Sabaea. The channel is 269km (167 miles) long. Orbit Number 94873 Latitude 15.4254 Longitude 28.7992 Instrument VIS Captured 2023-05-05 03 35

This VIS image shows the confluence of the two main channels of Nanedi Valles. Nanedi Valles is 508 km long (315 miles) and is located in Xanthe Terra. Orbit Number 81224 Latitude 6.88707 Longitude 312.284 Instrument VIS Captured 2020-04-06 07 16

This 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 captured by NASA's 2001 Mars Odyssey spacecraft shows Ross Crater in Aonia Terra.

Fine Layered Deposits Near Capri Mensa

The linear and circular features in this image from NASA's Mars Odyssey spacecraft are all volcanic and are located at the base of the southern flank of Ascraeus Mons.

Warrego Valles

Termed both 'catena' and 'fossae,' long linear depressions created by tectonic forces are a dominate surface feature of Alba Mons in this image captured by NASA's Mars Odyssey spacecraft.

The impact crater in this NASA Mars Odyssey image is a model illustration of the effects of erosion on Mars. The degraded crater rim and several landslides observed in crater walls are evidence of the mass wasting of materials.

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 features running vertically in the image are part of Tractus Catena. While other graben in the area are identified as fossae (defined as a long, narrow depression), the circular depressions within this graben lead to the descriptor name catena (defined as a chain of craters). In this case the craters are a result of roof collapse into an underlying open space such as a lava tube. Orbit Number 79329 Latitude 31.4358 Longitude 258.102 Instrument VIS Captured 2019-11-02 06 36

This image from NASA's 2001 Mars Odyssey shows a small portion of the complex channel system, Kasei Valles. In this image, secondary channeling has cut down deeper into the main channel.

Elysium Windstreaks

This lava channel is part of the Elysium Mons flows

Crater Dust Avalanches

This image shows part of the southeastern flank of Pavonis Mons. Surface lava flows run down hill from the top left of the image to the bottom right. Perpendicular to that trend are several linear features. These are faults that encircle the volcano and also run along the linear trend through the three Tharsis volcanoes. This image illustrates how subsurface lava tubes collapse into the free space of the empty tube. Just to the top of the deepest depression are a series of circular pits. The pits coalesce into a linear feature near the left side of the deepest depression. The mode of formation of a lava tube starts with a surface lava flow. The sides and top of the flow cool faster than the center, eventually forming a solid, non-flowing cover of the still flowing lava. The surface flow may have followed the deeper fault block graben (a lower surface than the surroundings). Once the flow stops there remains the empty space lower than the surroundings, and collapse of the top of the tub

THEMIS Images as Art #35

This VIS image shows part of the floor of Moreux Crater. Sand dunes are found in this region of the crater floor. Moreux Crater is located on the northern margin of Terra Sabaea. Orbit Number 72774 Latitude 42.2007 Longitude 44.0537 Instrument VIS Captured 2018-05-11 10 12

This image shows a portion of the flank of Pavonis Mons as seen by NASA's 2001 Mars Odyssey spacecraft. The collapse features at the bottom of the image are related to subsurface tubes that once contained lava.

Sharp Scarp and Varied Features

Multiple channels dissect the northwestern flank of Hecates Tholus in this image as seen by NASA's 2001 Mars Odyssey spacecraft.

This image from NASA's 2001 Mars Odyssey spacecraft shows the complex collapse features on the southern flank of Ascraeus Mons.

Do you see what I see in this image from NASA's Mars Odyssey spacecraft The multiple craters that cross the center of this image resemble a baby bug following the larger mama bug.

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 92253 Latitude -32.4503 Longit

The linear depression in this VIS image is part of Idaeus Fossae. Idaeus Fossae is a complex set of channels on the margin of Tempe Terra and Acidalia Planitia. Orbit Number 78903 Latitude 37.553 Longitude 307.559 Instrument VIS Captured 2019-09-28 04 45

Giant Polygon Troughs, Elysium Planitia at Full Resolution

This image captured by NASA's 2001 Mars Odyssey spacecraft shows some the sand dunes on the floor of Danielson Crater.

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