Mars Terrain Exploration

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

Channels

Today's VIS image shows dust devil tracks in Utopia Planitia. The tracks occur where dust devils have scoured the fine materials off the underlying surface. In some cases dust devils can create arced tracks. The ones in this image are mostly linear. Orbit Number 72335 Latitude 51.4292 Longitude 112.722 Instrument VIS Captured 2018-04-05 06 20

Today's VIS image shows a section of Mamers Valles. The channel is nearly 1000 km long (600 miles). Mamers Valles originates near Cerulli Crater in northern Arabia Terra, and after a short section near the crater where flow is to the south, flows northward to empty in Deuteronilus Mensae. The steep walls of Mamers Valles can reach heights of 1200 m (4000 feet). This portion of Mamers Valles is part of the southward flowing channel. Orbit Number 89757 Latitude 31.2642 Longitude 20.0676 Instrument VIS Captured 2022-03-09 21 42

Reull Vallis

This VIS image shows a region of chaos near the terminal end of Morava Valles. Located in Margaritifer Terra, Morava Valles is one of several channels that empty northward towards Chryse Planitia. Morava Valles arises from a region of chaos. Chaos terrain is also found along the course of the channel and may occur where the channel flow fluid warmed the subsurface ice creating additional release points for melted subsurface ice. Chaos terrain is typified by regions of blocky, often steep sided, mesas interspersed with deep valleys. With time and erosion the valleys widen and the mesas become smaller. It has been proposed that a catastrophic outflow of subsurface water creates the chaos and provides the surface flow creating the channel. Orbit Number 79002 Latitude -11.1516 Longitude 338.097 Instrument VIS Captured 2019-10-06 08 08

Today's VIS image shows a portion of Nanedi Valles. This channel is over 500 km long (310 miles) and is located in Xanthe Terra. Orbit Number 79240 Latitude 4.57002 Longitude 309.592 Instrument VIS Captured 2019-10-25 22 34

Located north of Olympus Mons and west of Alba Patera, Acheron Fossae, seen in this NASA Mars Odyssey image, provides a record of early tectonic activity in the Tharsis region.

Numerous dark slope streaks are located on the inner rim of this unnamed crater in Terra Sabaea. This image is from NASA's 2001 Mars Odyssey spacecraft.

Proposed MSL site in Meridiani Crater Lake

The small crater in the middle of the image is at the upwind side of the dune field. There is a considerable amount of sand within the crater, with a relatively smooth surface and few dune forms. It is likely that this crater provides a source of available sand for the large dune field. Located in eastern Arabia is an unnamed crater, 120 kilometers (75 miles) across. The floor of this crater contains a large exposure of rocky material, a field of dark sand dunes, and numerous patches of what is probably fine-grain sand. The shape of the dunes indicate that prevailing winds have come from different directions over the years. The Odyssey spacecraft has spent over 15 years in orbit around Mars, circling the planet more than 71,000 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 receive

Channel

This image captured by NASA's 2001 Mars Odyssey spacecraft shows part of the northern flank of Hecates Tholus, which is located on the northern part of the Elysium Volcanic Complex.

The channel-like features in this VIS image are tectonic graben. These graben are called Sirenum Fossae. Graben are created in regions of extensional tectonic stress, where the bedrock is faulted and pulled apart, allowing linear sections of the surface to drop downward along paired faults. The Sirenum Fossae graben are 2735km (1700 miles) long. Orbit Number 84111 Latitude -37.1819 Longitude 191.303 Instrument VIS Captured 2020-11-30 00 06

Hypansis Vallis

Dark Slope Streaks

Dark slope streaks mark many of the hills in this image captured by NASA's 2001 Mars Odyssey spacecraft. This region of hills is called Tartarus Colles. The term colles means small hills or knobs.

Cerberus Fossae

Today's VIS image shows part of Cerberus Fossae. These large graben cut across the Tartarus Montes in Elysium Planitia. A graben is formed when large blocks of material slid downward between paired faults in regions of extensional stresses. Orbit Number 77648 Latitude 10.0918 Longitude 160.48 Instrument VIS Captured 2019-06-16 20 19

This image from NASA's Mars Odyssey is located west of Zephyria Planum. Surfaces in this region have undergone extensive erosion by the wind. Wind is one of the most active processes of erosion on the surface of Mars today.

Wind Power

Bright windstreaks are located around several small craters at the top of this image captured by NASA's 2001 Mars Odyssey spacecraft.

In this NASA Mars Odyssey image of western Acidalia, two craters of similar size dramatically display the effects of geologic activity. The younger one on the left has been left relatively well preserved.

The channel feature in this image from NASA's 2001 Mars Odyssey spacecraft is called Mangala Fossa. This feature was formed by tectonic activity, with the walls being faults that allowed the central portion to slide downward forming a graben.

This windstreak is located on the volcanic plains of Daedalia Planum as seen by NASA's Mars Odyssey. The dark outer margin is the region of dust being removed from the surface. The inner bright part is where dust is being deposited.

Multiple slope streaks are visible on the rim of Henry Crater

This VIS image shows a section of Granicus Valles, one of several channel systems that originate near the western margin of the Elysium Mons volcanic complex. The channel system is approximately 750 km (466 miles) long. It is likely that both water and lava played a part in creating the channel. Orbit Number 80107 Latitude 26.9142 Longitude 133.873 Instrument VIS Captured 2020-01-05 08 02

Dark Slope Streaks

Dao Vallis

Landslide

THEMIS ART #91

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

Small Features

This image of Ganges Chasma, captured by NASA's 2001 Mars Odyssey spacecraft, contains both landslide deposits and dunes.

This image captured by NASA's 2001 Mars Odyssey spacecraft shows numerous dark streaks on the inner rim of this unnamed crater.

Infilled Crater

The odd pattern on the floor of this channel suggests that a volitile such as ice played a part in its formation

This ridged and pockmarked surface is located west of Phlegra Montes in the northern plains

The small channels in this image of Utopia Planitia are south of Granicus Valles were captured by NASA's Mars Odyssey on July 23, 2010.

The collapse features in this images are related to lava tubes that likely originated at Elysium volcanic complex

This image from NASA's 2001 Mars Odyssey spacecraft shows a channel carved by lava. This channel is located northeast of Olympus Mons.

This VIS image shows part of Albor Fossae. These fossae (graben) are located on the southeastern flank of Albor Tholus, one of the volcanoes of the Elysium volcanic complex. Orbit Number 81529 Latitude 18.2534 Longitude 151.75 Instrument VIS Captured 2020-05-01 10 03

Deposition + Erosion = Textures

Many small channels dissect the rim of Martz Crater, as shown in this image captured by NASA's 2001 Mars Odyssey spacecraft.

Located on the northern margin of Aonia Terra, this unnamed crater interacts with one of the fossa, also called a graben. In this image, it is apparent that the tectonic depression crosses the crater, which means the crater was created before the depression. The ability to relatively date the different features allows for interpretations of the series of events that created the features in this image. Orbit Number 74806 Latitude -42.6506 Longitude 273.295 Instrument VIS Captured 2018-10-25 18 22

This image from NASA's 2001 Mars Odyssey spacecraft shows different surface textures in some of the lava flows of Daedalia Planum.

The linear depressions in this image captured by NASA's 2001 Mars Odyssey spacecraft are part of Memnonia Foassae.

The hills in this image captured by NASA's 2001 Mars Odyssey spacecraft are part of a large region of hills located north of Hecates Tholus.

This image from NASA's 2001 Mars Odyssey spacecraft shows a portion of the floor of Crommelin Crater. This crater contains a large mound of material that filled a large part of the crater and has been subsequently eroded.

This VIS image shows a section of Nanedi Valles. Located In Xanthe Terra, the channel system is more than 500 km (310 miles) long. Orbit Number 79527 Latitude 4.41081 Longitude 309.635 Instrument VIS Captured 2019-11-18 13 44

This VIS image shows a section of Her Desher Vallis. This channel is located in Noachis Terra. Orbit Number 74923 Latitude -25.1336 Longitude 312.258 Instrument VIS Captured 2018-11-04 10 15

The rounded hills in this VIS image are located in Arcadia Planitia. Broad linear ridges and groups of hills in this region are part of Phlegra Dorsa (ridges) and Phlegra Montes (hills). Orbit Number 71248 Latitude 30.6712 Longitude 171.018 Instrument VIS Captured 2018-01-05 17 05

This sand sheet and dune field occurs on the floor of Candor Chasma

This image from NASA's Mars Odyssey spacecraft shows the cratered highlands of Terra Sirenum in Mars' southern hemisphere. Near the center of the image running from left to right one can see long parallel to semi-parallel troughs called graben.

The two depression crossing this image are called Pavonis Fossae and are located just north of the volcano in this image captured by NASA's 2001 Mars Odyssey spacecraft.

This VIS image shows part of the rim of an unnamed crater in Terra Cimmeria. A group of channels dissect the rim near to upper left of the image. These channels are called gullies due to being on a steep slope rather than a flat river plain. With careful examination, it is possible to see a boundary layer between the upper incised gully and a lower deposition region. The boundary marks a change in slope, the steep upper portion supports fast moving fluid that carves into the rim eroding materials. The change to a flatter slope causes the fluid to slow down and as it slows the materials carried by the fluid a deposited. Orbit Number 75452 Latitude -47.6995 Longitude 170.871 Instrument VIS Captured 2018-12-17 23 46

This VIS image shows the region where flank flows from Olympus Mons (top of image) meet the surrounding lava plains. Orbit Number 80678 Latitude 12.5468 Longitude 223.171 Instrument VIS Captured 2020-02-21 08 19

Everywhere Dunes

Numerous channels dissect the higher elevation material at the top of this image. This image captured by NASA's 2001 Mars Odyssey spacecraft is located in Noachis Terra.

This image captured by NASA's 2001 Mars Odyssey shows just one of many lava channels located on the Elysium Mons volcanic complex.

Rugged Crater Floor. Today's VIS image shows part of an unnamed crater located in Noachis Terra. Unlike most Martian craters, this one has a very rugged floor. Most craters have flat floors, having been filled with materials such as sand blown into the crater, layered deposits from short term lakes, and volcanic materials from nearby flows. The morphology of the crater floor indicates that this is a relatively young crater, with the original floor created during the impact event. Orbit Number 93133 Latitude -41.7607 Longitude 16.3316 Instrument VIS Captured 2022-12-12 20 18 https //photojournal.jpl.nasa.gov/catalog/PIA25841

Today's VIS image shows a very small portion of the extensive lava flows of the Tharsis volcanic complex. These flows are located southwest of Ascraeus Mons. Orbit Number 81900 Latitude 6.11029 Longitude 250.287 Instrument VIS Captured 2020-05-31 23 08

This image from NASA's 2001 Mars Odyssey spacecraft shows two channels. The channel in the center of the image ends in a crater, where it has created a delta deposit. These craters and channels are located on the northeastern margin of Icaria Planum.

This image from NASA's 2001 Mars Odyssey shows the eastern flank of Pavonis Mons.

This VIS image shows a section of the tributary channel between Aram Chaos and Ares Vallis. A small landslide deposit is visible in the middle of the image. Orbit Number 79763 Latitude 2.95902 Longitude 341.373 Instrument VIS Captured 2019-12-08 00 06

The ancient, catastrophic floods on Mars, whose origins remain a mystery, produced a channeled and scoured landscape like this one, which is called Tiu Valles and was imaged by NASA's Mars Odyssey spacecraft.

Crater Delta. Today's VIS image shows two unnamed channels on the western edge of Claritas Fossae. The small channel joins the larger one close the the crater rim. The main channel has formed a delta in the crater. Deltas are formed when sediment laden rivers slow down - either due to a flattening of topography, or entering a standing body of water. The reduction in velocity causes the sediments to be deposited. The main channel often diverges into numerous smaller channel that spread apart to form the typical fan shape of a delta. Orbit Number 92145 Latitude -39.0947 Longitude 256.903 Instrument VIS Captured 2022-09-22 12 24 https //photojournal.jpl.nasa.gov/catalog/PIA25747

This is an image from NASA's Mars Odyssey spacecraft of an area within Acidalia Planitia that contains patterned ground (near the top of the image). This type of surface is likely related to subsurface ice.

In this image from NASA's Mars Odyssey spacecraft, bizarre textures cover the surface of eastern Utopia Planitia, where there is a high probability that ground ice has played a role in the formation of this unusual landscape.

Erosion and what it Reveals

This VIS image shows two of the channel segments of Granicus Valles. Granicus Valles is a complex channel system located west of Elysium Mons. The system is approximately 750km long. It is likely that both water and lava played a part in creation of the feature. Orbit Number 88156 Latitude 28.6099 Longitude 129.149 Instrument VIS Captured 2021-10-29 01 49

The depressions in the rim of this unnamed crater in Terra Sabaea are being filled with new material. The surface texture of the new material is different from the surrounding older material

This image shows a portion of Auqakuh Vallis

This image from NASA's 2001 Mars Odyssey is of an unnamed channel located in Xanthe Terra.

Image captured by NASA's 2001 Mars Odyssey spacecraft shows the eastern flank of Arsia Mons midway between the summit of the volcano and the surrounding plains.

This VIS image shows much of the same location as yesterday's image. Gale Crater is the home of the Curiosity Rover. The rover landed in August of 2012 and has been exploring the crater for the past 6 Earth years (3 Mars years). The goal of the mission is to climb onto the layered deposit in the center of the crater to assess it's possible origins. Orbit Number 71424 Latitude -4.66294 Longitude 137.356 Instrument VIS Captured 2018-01-20 04 52

The windstreaks in this image captured by NASA's Mars Odyssey are located on lava flows from Arsia Mons.

Maunder Crater. One of the most interesting features of Maunder Crater is the large trough seen in this image. The floor of Maunder Crater has been filled by a significant amount of material. At some time after the filling event, the large trough developed. The depression is located on the east side of the crater and parallels the crater rim. How and why the trough came to be is unknown. Orbit Number 91505 Latitude -49.2071 Longitude 2.39522 Instrument VIS Captured 2022-07-31 19 36

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 covers part of the floor of the canyon. At the top of the image is one of the many hills found on the floor in this region. The linear grooved surface is part of a landslide deposit. Melas Chasma has many large landslide regions. Landslide deposits often have grooved surfaces with the grooves parallel to the direction of movement as the slide occurred. The ends of the landslide typically have a lobate edge, and will flow around large preexisting landforms. The Odyssey spacecraft has spent over 15 years in orbit around

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. Orbit Number 88761 Latitude 8.29946 Longitude 317.817 Instrument VIS Captured 2021-12-17 21 18

This image shows several wind streaks in Syrtis Major Planum as seen by NASA's 2001 Mars Odyssey spacecraft.

Kasei Channels

Fine-scale Textures

Today's VIS image shows an unnamed crater in southern Acidalia Planitia. The ejecta blanket has radial grooves, and the inner crater rim is dissected by numerous gullies. Orbit Number 95137 Latitude 36.2589 Longitude 329.564 Instrument VIS Captured 2023-05-26 21 24

$The Kasei Valles region is very complex. This image captured by NASA's Mars Odyssey illustrates that complexity with features created by fluvial action (channels) and tectonic processes (fractures).$

The ridges on the floor of this crater are made of a more resistant material that their surroundings. Erosion is removing the less resistant material

$The fractures in this image from NASA's 2001 Mars Odyssey spacecraft are part of Labeatis Fossae.$

Today's VIS image shows part of the northeastern portion of Jezero Crater. The Perserverance Rover is located on the northwestern part of the crater - near a delta deposit formed by the influx of silt laden water into the crater at a time during Mars' past that was wetter. The crater most likely hosted a lake for a period of time. The channel at the top of this image was formed by the flow of water exiting the crater. Orbit Number 89206 Latitude 18.3845 Longitude 78.1952 Instrument VIS Captured 2022-01-23 12 45

Small ripple-like dunes surround hills in the region of Elysium Planitia in this image from NASA's Mars Odyssey spacecraft.

Today's VIS image shows the western rim of Bamberg Crater. The complex nature of the rim is one indication of the relative youth of this crater in relation to it's surrounding. Many gullies dissect this rim. Orbit Number 71254 Latitude 39.6224 Longitude 356.451 Instrument VIS Captured 2018-01-06 05 00

The linear feature in this image captured by NASA's 2001 Mars Odyssey spacecraft is part of Cyane Fossae. The circular collapse features are bounded by linear faults.

This heavily dissected surface is located within the Acheron Fossae region

This image captured by NASA's 2001 Mars Odyssey shows unnamed channel flows northward in Margaritifer Terra.

Deposits in Electris Region

This image from NASA's Mars Odyssey shows part of the floor of Ganges Chasma. Deposits of fine surface materials and bright layered deposits are visible in this image.

This image shows a small portion of the floor deposits within Melas Chasma.

This unnamed crater in Terra Cimmeria is not as round in shape as other craters. Major landslides have occurred on the crater rim, resulting in the final shape as seen by NASA's 2001 Mars Odyssey spacecraft.

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

Today's VIS image is of a group of craters in Solis Planum. Because three of the craters are overlapping it is possible to determine the order in which those three were created. While we can not say exactly when in Martian history these craters formed, we can delineate the relative order of formation. Since impacts create circular craters, a recently formed crater will create a crescent into the crater it impacts. So the order of impact in this image is 1) the crater at the bottom, 2) the large crater in the middle of the image, and 3) the small crater mostly off this image to the right. Orbit Number 67865 Latitude -30.7955 Longitude 276.931 Instrument VIS Captured 2017-04-01 23 16

This image from NASA's 2001 Mars Odyssey spacecraft shows a portion of Dittaino Valles.

Wrinkle Ridges in Solis Planum

Today's VIS image shows a section of Mamers Valles. The channel is nearly 1000 km long (600 miles). Mamers Valles originates near Cerulli Crater in northern Arabia Terra, and after a short section near the crater where flow is to the south, flows northward to empty in Deuteronilus Mensae. This image is located where the channel changes from southward flow to northward. On the right side of the image the channel cuts from one crater into a lower one. The channel hugs the wall of the second crater and then exits to the top of the image. The steep walls of Mamers Valles can reach heights of 1200 m (4000 feet). Orbit Number 80086 Latitude 30.9514 Longitude 19.1598 Instrument VIS Captured 2020-01-03 14 34

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