Martian Terrain and Geological Features

This cluster showcases diverse Martian landscapes, including dune fields, craters, and erosion patterns, highlighted by grayscale imagery that emphasizes texture and topography.

Channels

Oudemans Crater Central Uplift: A Sample of Well-Preserved Layering Excavated from Kilometers Below

This image captured by NASA's 2001 Mars Odyssey spacecraft is located in Ravi Vallis, a channel running from the highlands of Xanthe Terra to the complex lower elevation Hydraotes Chaos.

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 89812 Latitude -22.162 Longitude 240.598 Instrument VIS Captured 2022-03-14 10 06

Crater Features

Marte Valles

Kasei Valles

Inverted Topography

Large landslide deposits dominate this image of Ius Chasma captured by NASA's 2001 Mars Odyssey. Dunes are visible at the bottom of the frame.

$The fracture system in this image, captured by NASA's 2001 Mars Odyssey, is part of Galaxias Fossae, a series of fractures on the northern part of the Elysium Mons volcanic complex.$

Huge regions of complex valleys and chaos are located in Xanthe and Margaritifer Terras. Rising from Valles Marineris, outflow channels like Ares, Tiu and Shalbantana valles empty into Chryse Planitia. This VIS image shows part of Chryse Chaos, located within Masursky Crater, along the Tiu Valles channel. Chaos forms from erosion of the surface into mesa features. With time the valleys expand creating the jumble of hills seen in the image. Orbit Number 79152 Latitude 11.5428 Longitude 327.544 Instrument VIS Captured 2019-10-18 16 42

Collapse Features

This image from NASA's 2001 Mars Odyssey spacecraft shows a small portion of Ma'adim Vallis. This channel intersects Gusev Crater, home of the Spirit Rover.

Patapsco Vallis

The narrow volcanic flows in this image captured by NASA's 2001 Mars Odyssey spacecraft are located on the northeastern flank of Olympus Mons.

Gully Grab Bag in Crater Wall in the Terra Sirenum Region

At the southern end of Echus Cansma this dissected surface and mega-gullies occur

Iani Chaos

This image from NASA's Mars Odyssey caputured on July 23, 2010 off the northern flank of Arsia Mons shows collapse/vent features.

Distal Rampart of Crater in Chryse Planitia

These dust slides are located on the wall of Thithonium Chasma

Ius Chasma Ridge

Wind Etching

Channel

Amidst the hummocky topography produced by the ejecta from Lyot crater, smooth patches of material fill shallow depressions in this NASA Mars Odyssey image.

This image shows a small landslide on the northern margin of Tiu Vallis

Numerous gullies are visible in this image captured by NASA's 2001 Mars Odyssey spacecraft of Asimov Crater.

The pits and channels in the VIS image are located along the margin between Arabia Terra and Acidalia Planitia. Arabia Terra is one of the oldest surface regions on Mars and contains a large variety of surface features. Orbit Number 77916 Latitude 30.7624 Longitude 345.182 Instrument VIS Captured 2019-07-08 22 06

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 91585 Latitude -48.766 Longitude 34.0294 Instrument VIS Captured 2022-08-07 09 15

Streamlined islands, like the one shown in this NASA Mars Odyssey image, are one piece of geologic evidence that large quantities of water once flowed across the surface of Mars in the distant past.

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 94829 Latitude 21.9 Longitude 217.227 Instrument VIS Captured 2023-05-01 12 40

Dunes are found on the floor of this unnamed crater located on the margin between Arabia Terra and Terra Sabaea in this image from NASA's 2001 Mars Odyssey spacecraft.

Today's VIS image shows a small part of Daedalia Planum. The lava flows originate from Arsia Mons, one of the large volcanoes in the Tharsis region. The different surface textures are created by differences in the lava viscosity and cooling rates. The lobate margins of each flow can be traced back to the start of each flow or to the point where they are covered by younger flows. Flows in Daedalia Planum can be as long as 180 km. Orbit Number 81888 Latitude -22.8438 Longitude 240.412 Instrument VIS Captured 2020-05-30 23 16

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 82045 Latitude -43.8185 Longitude 34.3876 Instrument VIS Captured 2020-06-12 21 24

The unnamed channel in this image captured by NASA's 2001 Mars Odyssey spacecraft is located in Terra Sabaea.

The linear depressions in this VIS image are part of Sirenum Fossae. These depressions are called graben, which form by the down drop of material between two parallel faults. The faults are caused by extensional tectonic stresses in the region. The fossae are 2735km long (1700 miles). Orbit Number 83511 Latitude -26.424 Longitude 218.759 Instrument VIS Captured 2020-10-11 14 31

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

Today's VIS image shows a small portion of Dao Vallis. Located south of Hadriacus Mons (a volcano), this channel is approximately 1200km (750 miles) long. It has been proposed that heating of the region due to volcanic activity melted subsurface ice which was released to the surface to carve the channel. Dao Vallis empties into the Hellas Planitia basin. Orbit Number 83191 Latitude -34.7957 Longitude 91.6287 Instrument VIS Captured 2020-09-15 06 07

Mangala Vallis

In the bottom half of this image captured by NASA's 2001 Mars Odyssey spacecraft is a line of small volcanic vents.

Today's VIS image shows part of northern Arabia Terra. Arabia Terra is one of the oldest surface regions on Mars and contains a large variety of surface features. The region is dissected with numerous unnamed channels of all sizes and complexities, as well as numerous pits of unknown origin. The majority of channels in this region flow north into Acidalia Planitia. The western rim of Sinton Crater is visible at the top of the image. Sinton Crater is 62km in diameter (39 miles). Orbit Number 89794 Latitude 39.9655 Longitude 31.1803 Instrument VIS Captured 2022-03-12 22 52

The floor of a 75 km diameter crater in the Amenthes region of Mars displays lobate flow features in the center of this image from NASA's Mars Odyssey spacecraft.

The downdropped block of surface seen in this image captured by NASA's 2001 Mars Odyssey spacecraft is called a graben. The graben is younger than the crater, since the crater is cut by the graben.

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). Orbit Number 79487 Latitude 31.1242 Longitude 19.9702 Instrument VIS Captured 2019-11-15 06 50

This image captured by NASA's 2001 Mars Odyssey spacecraft shows where Patapsco Vallis enters the largest depression of Elysium Fossae. Patapsco Vallis, on the Elysium Mons volcanic complex, was likely formed by the flow of lava rather than water.

NASA's 2001 Mars Odyssey spies what looks like a praying mantis looking back at the spacecraft.

This NASA Mars Odyssey image captures a portion of several lava flows in Daedalia Planum southwest of the Arsia Mons shield volcano. Textures characteristic of the variable surface roughness associated with different lava flows in this region are easily s

Destination: Meridiani

Hebes Chasma Mosaic

The interconnected collapse pits at the top of this image, taken by NASA's 2001 Mars Odyssey spacecraft, are part of Coprates Catena. Notice the dunes in the bottom of each pit.

Freedom crater, located in Acidalia Planitia, exhibits a concentric ring pattern in its interior as seen in this image from NASA's Mars Odyssey spacecraft, suggesting that there has been some movement of these materials towards the center of the crater.

Today's VIS image shows several unnamed channels located in northern Arabia Terra. Channels in this region of Arabia Terra are flowing northward into the lower elevations of Acidalia Planitia. Orbit Number 89794 Latitude 39.9655 Longitude 31.1803 Instrument VIS Captured 2022-03-12 22 52

Located in Arabia Terra, the crater shown in this image from NASA's Mars Odyssey spacecraft is known as Henry Crater. Like many other craters on Mars, the interior of Henry Crater is filled with a layered deposit.

Newton Crater

Today's VIS image shows part of Maja Valles, a large channel system in Lunae Planum. The main part of the channel is visible at the upper left in this image. The lower part of the image is located within an old crater called Stege Crater. The channel in the central part of the image is flowing along the inner rim of the crater and into the main Maja Valles channel just off the image to the left. Maja Valles in 1600 km (1000 miles) long. Like most outflow channels in the region, Maja Valles arises from Valles Marineris and drains into Chryse Planitia. Maja Valles starts in Juventae Chasma. Orbit Number 89111 Latitude 4.27445 Longitude 300.886 Instrument VIS Captured 2022-01-15 16 56

This image from NASA's Mars Odyssey shows the northern sidewall of Melas Chasma.

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 79215 Latitude 5.581 Longitude 310.73 Instrument VIS Captured 2019-10-23 21 10

Tharsis Collapse Pits

Ius Chasma

Impact Crater Filled With Layered Deposits

This image shows part of Coprates Chasma as seen by NASA's 2001 Mars Odyssey spacecraft.

$The fractures in this image captured by NASA's 2001 Mars Odyssey spacecraft are aligned with most of the fractures in Tempe Terra, but are some distance from the bulk of the fracturing.$

This image of the east end of Coprates Chasma contains several dune fields. The dunes in the center of the image are larger and darker than the dunes at the bottom

This image shows a portion of the summit caldera of Olympus Mons

Western Meridiani

Milankovic Crater is located in central Arcadia Planitia. This VIS image shows small sand dunes on the crater floor, and larger dunes within the central crater peak/pit feature. With a diameter of just under 120km, Milankovic Crater is the largest crater in the region. Orbit Number 71870 Latitude 54.2312 Longitude 213.365 Instrument VIS Captured 2018-02-25 23 00

The many small channels in this image are part of the larger Sabis Vallis

The lava flows in this image from NASA's 2001 Mars Odyssey spacecraft are located east of Olympus Mons.

The floor of the crater at the top of this image from NASA's 2001 Mars Odyssey spacecraft is completely covered by a large sand sheet with surface dune forms. Now that is it near the end of northern spring all the frost has disappeared from the sand.

The jumbled, chaotic terrain in this NASA Mars Odyssey image may represent a source region for the Reull Vallis, one of the larger channel systems in the southern hemisphere of Mars.

Small, dark sand dunes are located on the floor of Moreux Crater.

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). Orbit Number 94876 Latitude 21.1353 Longitude 301.426 Instrument VIS Captured 2023-05-05 09 33

$Paired fractures with a downdropped block between them are termed graben. Graben are common on Alba Patera, where this image is located$

Olympica Fossae is a complex channel located on the volcanic plains between Alba Mons and Olympus Mons. It contains both linear sections that appear to be tectonic in origin and sinuous sections that were more likely created by liquid flow. There are several streamlined islands in this image, indicating a fluvial origin in this section of the fossae. Given the location it appears that lava, rather than water, was the fluid. Olympica Fossae 420km long (261 miles). Orbit Number 95165 Latitude 23.3032 Longitude 243.696 Instrument VIS Captured 2023-05-29 04 39

Linear Ridges

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 19 46

The dunes shown in this image from NASA's 2001 Mars Odyssey are located on the floor of Hussey Crater in Terra Sirenum.

This image captured by NASA's 2001 Mars Odyssey spacecraft shows a portion of the northern cliff face and complex floor deposits of Ophir Chasma.

Crater Floor in Arabia Terra Region

Dusty Volcanic Vent in Syria Planum

Melas Chasma is part of the largest canyon system on Mars, Valles Marineris. At only 563 km long (349 miles) it is not the longest canyon, but it is the widest. Located in the center of Valles Marineris, it has depths up to 9 km below the surrounding plains, and is the location of many large landslide deposits, as will as layered materials and sand dunes. There is evidence of both water and wind action as modes of formation for many of the interior deposits. This VIS image highlights the extent of layered materials within the canyon. 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 imagin

The smooth plains of Elysium embay the blocky broken up highlands of Aeolis in this image from NASA's Mars Odyssey spacecraft. The plains have been interpreted by researchers to be possibly mudflows or lava flows.

Reull Vallis

A small channel system dissects the rim of this unnamed crater in Terra Sirenum. Orbit Number 74466 Latitude -39.9359 Longitude 182.762 Instrument VIS Captured 2018-09-27 18 47

The dark windstreaks in this image are located on volcanic flows northwest of Ascraeus Mons

Eroded Ejecta

This image captured by NASA's 2001 Mars Odyssey spacecraft shows several windstreaks located on the volcanic flows west of Ceraunius Tholus.

. Elyisum Fossae. Today's VIS image contains sections of two of the many channel forms found radial to the Elysium Mons volcanic complex. In this case the fossae are located to the west of Elysium Mons. Elysium Fossae are comprised of both linear and sinuous channels, usually interpreted to have both fluid and tectonic forces playing a part in the formation. The linear depression resembles a graben (formed by tectonic forces) and sinuous channel more closely resembles features caused by fluid flow - either lava or water created by melting subsurface ice due to volcanic heating. The Elysium Fossae system is 1044 km (649 miles) in length. Orbit Number 94395 Latitude 25.0308 Longitude 137.23 Instrument VIS Captured 2023-03-26 19 03

This image from NASA's 2001 Mars Odyssey spacecraft shows sand dunes on the floor of an unnamed crater near Meridiani Planum.

Layers in Olympus Mons Basal Scarp

Joint Observation of the Isidis Basin with the Rosetta Mission

These clouds are located near the edge of the south polar region. The cloud tops are the puffy white features in the bottom half of the image

The gullies at the top of the image captured by NASA's 2001 Mars Odyssey spacecraft occur on the rim of an unnamed crater on the larger rim of the Argyre Basin. It has been postulated that this type of gully may form due to the melting of a snow/ice cover

This 2001 Mars Odyssey image shows dark dunes on the floor of Lamont Crater.

Sirenum Fossae

The smaller crater within the larger crater is called Gasa Crater, as shown in this image from NASA's 2001 Mars Odyssey spacecraft.

These lava flows occur on the flank of Olympus Mons

This image from NASA's 2001 Mars Odyssey spacecraft shows a region of the south pole where the surface has developed linear markings, a pattern not unlike a thumbprint.

Southern Kasei Vallis

The channels in this image, taken by NASA's 2001 Mars Odyssey spacecraft, are called Hephaestus Fossae and were most likely formed by lava flow and erosion rather than being eroded by water.

Daedalia Planum. 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 92152 Latitude -22.9243 Longitude 240.536 Instrument VIS Captured 2022-09-23 01 36 https //photojournal.jpl.nasa.gov/catalog/PIA25748

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