Mars Impact Craters

Images of Mars showcasing various impact craters, with features like ripples, exposed rock, and ancient channels against a rugged Martian landscape.

View taken from the Mars Reconnaissance Orbiter showing part of the floor of a large impact crater in the southern highlands on Mars, north of the giant Hellas impact basin. Most of the crater floor is dark, with abundant small ripples of wind-blown material. A pit in the floor of the crater has exposed light-toned, fractured rock, which appears fractured at several different scales.
View taken from the Mars Reconnaissance Orbiter showing part of the floor of a large impact crater in the southern highlands on Mars, north of the giant Hellas impact basin. Most of the crater floor is dark, with abundant small ripples of wind-blown material. A pit in the floor of the crater has exposed light-toned, fractured rock, which appears fractured at several different scales.
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View taken from the Mars Reconnaissance Orbiter showing part of the floor of a large impact crater in the southern highlands on Mars, north of the giant Hellas impact basin. Most of the crater floor is dark, with abundant small ripples of wind-blown material. A pit in the floor of the crater has exposed light-toned, fractured rock, which appears fractured at several different scales.
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An isolated, elongated mound (about 1 mile wide and 3.75 miles long) rises above the smooth, surrounding plains. Horizontal layers are exposed at the northern end of the mound, and its surface is characterized by a very unusual quasi-circular pattern with varying colors that likely reflect diverse mineral compositions. A closer view shows that the rock has a range of textures, from massive and fractured on the left, to subtle banding or layering on the right. The origin of this mound is unknown, but its formation may be related to the clay-bearing rocks in the nearby Oxia Planum region.
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In this image from NASA's Mars Reconnaissance Orbiter is an old degraded crater that has undergone a complex history of burial and erosion. At least two types of exposed bedroc are shown here.
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This image captured by NASA's Mars Reconnaissance Orbiter shows ancient highland channels in Eridania Valley.
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The largest crater associated with a March 2012 impact on Mars has many smaller craters around it, revealed in this image from the High Resolution Imaging Science Experiment (HiRISE) camera on NASA's Mars Reconnaissance Orbiter.
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This image shows the remains of an ancient delta in Mars' Jezero Crater, which NASA's Perseverance Mars rover will explore for signs of fossilized microbial life. The image was taken by the High Resolution Stereo Camera aboard the ESA (European Space Agency) Mars Express orbiter. The European Space Operations Centre in Darmstadt, Germany, operates the ESA mission. The High Resolution Stereo Camera was developed by a group with leadership at the Freie Universitat Berlin.
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This image from NASA's Mars Reconnaissance Orbiter spacecraft samples the excellent bedrock exposures north of Terby Crater, which lies on the northern rim of the giant Hellas basin.
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Oxia Planum is an ancient (Noachian epoch) terrain situated to the east of Chryse Planitia at about 18 degrees north. This image from NASA's Mars Reconnaissance Orbiteris of a proposed ExoMars Landing Site.
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This is only one of four impact craters on Mars known that possesses intact layers exposed in the central uplift in this image from NASA's Mars Reconnaissance Orbiter.
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Eridania is the name of topographically enclosed basin located in the Southern highlands of Mars that has been suggested to be the site of a large ancient lake or inland sea. This image is from NASA's Mars Reconnaissance Orbiter.
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Imaged by MRO's NASA's Mars Reconnaissance Orbiter Context Camera, this observation shows one of two odd, rounded mesas with a knobby, pitted texture.
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This image from NASA's Mars Reconnaissance Orbiter spacecraft shows an interesting collection of kilometer-scale craters with flat and smooth floors. The craters themselves may be caused by debris from a distant larger impact.
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The Tale of a Retreating Scarp. This scene on the north rim of Secchi Crater shows a curious depression with zig-zag walls. Some of the linear ridges on the floor of this feature are aligned with them. In some places on Mars, the dust and dirt is mixed with ice that covers a rocky surface. When the Sun shines, the ice can sublimate (turn directly into a vapor) and the dust and dirt collapse. This can form pits and depressions with a linear wall that is frequently parallel to the equator, and that wall retreats towards the equator. This retreat most likely started at the southern end and grew to a stable width. At some point it became wider, stopped, and then grew wider again. Linear ridges on the floor that parallel the top edge are deposits that show where the wall stopped during its long retreat northwards. There is also one long ridge that parallels the eastern wall. Researchers think that the area east of the ridge formed after the main depression. It again started at the south and
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This intriguing surface texture is the result of rock interacting with water, as observed by NASA's Mars Reconnaissance Orbiter. The rock was then eroded and later exposed to the surface. The pinkish, almost dragon-like scaled texture represents Martian bedrock that has specifically altered into a clay-bearing rock. The nature of the water responsible for the alteration, and how it interacted with the rock to form the clay remains poorly understood. Not surprisingly, the study of such altered rocks on Mars is an area of active investigation by the Mars science community. Understanding such interactions, and how they happened, help scientists to understand the past climate on Mars, and if the red planet ever harbored life. Recent studies indicate that the early Martian climate may not have been as warm, wet, and Earth-like, as previously suggested. This is not a problem for finding life on Mars as one might think. Ongoing studies of dry and cold environments on Earth shows that life fin
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McLaughlin Crater (21.9 N, 337.6 E) is a large, approximately 95-kilometer diameter impact crater located north of Mawrth Vallis, in Arabia Terra, seen here by NASA's Mars Reconnaissance Orbiter spacecraft.
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Hellas is an ancient impact structure and is the deepest and broadest enclosed basin on Mars as seen by NASA's Mars Reconnaissance Orbiter.
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Algal-bacterial mats and mineral deposits at a hot spring, Upper Geyser Basin, Yellowstone National Park, Wyoming, USA, North America
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Sometimes a central pit forms inside some Martian craters, especially when there's substantial ground ice. Such is the case in this observation from NASA's Mars Reconnaissance Orbiter spacecraft.
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The layered bedrock in this image was brought from several kilometers of depth during the formation of this 44 kilometer wide crater in the volcanic plains of Lunae Planum as seen by NASA's Mars Reconnaissance Orbiter.
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The Eridania Basin is thought to have once contained a large sea. This image from NASA's Mars Reconnaissance Orbiter spacecraft shows the Gorgonum Basin, which lies along the eastern edge of Eridania.
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NASA's Curiosity Mars rover can be seen in this image taken from space on May 31, 2019, by the High Resolution Imaging Science Experiment (HiRISE) camera aboard the Mars Reconnaissance Orbiter (MRO). In the image, Curiosity appears as a bluish speck. The image shows Curiosity at a location called Woodland Bay. It's just one of many stops the rover has made in an area referred to as the clay-bearing unit on the side of Mount Sharp, a 3-mile-tall (5-kilometer-tall) mountain inside of Gale Crater. Look carefully, and you can make out what it is likely Curiosity's head, technically known as the remote sensing mast. A bright spot appears in the upper-left corner of the rover. At the time this image was acquired, the rover was facing 65 degrees counterclockwise from north, which would put the mast in about the right location to produce this bright spot.
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This particular area, called Mangala Valles and located near the Tharsis region, may be an example of the action of liquid water in the ancient Martian past. This image is from NASA's Mars Reconnaissance Orbiter.
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This beautiful image shows terrific layers and exposed bedrock along a cliff in west Candor Chasma, which is part of the extensive Valles Marineris canyon system as seen by NASA's Mars Reconnaissance Orbiter.
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This image captured by NASA's Mars Reconnaissance Orbiter shows a transition from depressed to inverted channels in the Gorgonum Basin.
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This image from NASA's Mars Reconnaissance Orbiter shows the southwestern floor of a 50-kilometer diameter unnamed crater, about 100 kilometers northeast of Hellas Basin.
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Chryse Outflow Channel
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This image captured by NASA's Mars Reconnaissance Orbiter from the Gordii Dorsum region of Mars shows a large area covered with polygonal ridges in an almost geometric pattern.
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Large impacts produce uplifted central structures, either peaks, or pits, or an uplifted peak with a central pit. This crater south of Aurorae Chaos has a central pit exposing bedrock units with diverse colors, indicating diverse rock compositions. This crater includes clay-rich minerals identified by the CRISM instrument on MRO. See this enhanced-color cutout over the eastern half of the central pit.
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This impact crater in the region of Mars called Libya Montes, observed by NASA's Mars Reconnaissance Orbiter, shows typical gullies with alcoves at the top, channels, and depositional fans at the bottom.
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Gullies and Boulder Tracks. The formation of gullies on Martian slopes is still under debate. Potential mechanisms include the melting of surface water ice, groundwater outbursts, or dry mass wasting processes (landslides). This image shows several shallow gully channels with associated debris aprons emanating from a buried layer on the interior of a crater wall. Also visible are many boulders of varying sizes along the wall, with several exhibiting clear tracks from their journey downslope. These tracks can be used to better understand the mass wasting environment on the hill slope and whether there is any connection between the boulders and the gullies.
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Known since at least 2003, this is a wonderful case of aeolian sandstone that preserves its original sand dune bedform shapes and lies unconformably over a previously-eroded surface of layered sedimentary rock. MRO.
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Flying through the canyons and over the ridges of Valles Marineris, viewers can experience some of the thrills that gripped explorers who pushed into unknown regions on Earth
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This image of the Nili Fossae region, to the west of the great Isidis basin, shows layered bedrock with many impact craters. Nili Fossae is one of the most mineralogically important sites on Mars. Remote observations by the infrared spectrometer onboard MRO (called CRISM) suggest the layers in the ancient craters contain clays, carbonates, and iron oxides, perhaps due to hydrothermal alteration of the crust. However, the impact craters have been degraded by many millions of years of erosion so the original sedimentary, impact ejecta, or lava flows are hard to distinguish. The bright linear features are sand dunes, also known as transverse aeolian dunes, because the wind direction is at ninety degrees to their elongated orientation. This shows that the erosion of Nili Fossae continues to the present day with sand-sized particles broken off from the local rocks mobilized within the dunes.
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This image shows a crater on the floor of Eos Chasma, part of the Valles Marineris canyon system. Craters on Mars are useful for geologists because they provide cross-sections into the subsurface. The south wall of this crater shows evidence of several different types of rock, with diverse colors. In the black and white parts of the image, it appears that there are two types of rock one relatively light and one dark. However, in the 1.1 kilometer-wide color swath we can see that the dark rocks are more complicated, as some have a greenish tint and others are purple. Note that these are not the colors your eyes would see if you were there! In enhanced color, the HiRISE near-infrared data appears as red, the red is shown as green, and the blue-green data is shown as blue, allowing us to see more information at once.
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Amphitrites Patera
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Looking at the Crater Half Full. Planetary scientists look for targets that help them better understand the area they are interested in. In this particular image, there is a small (1 kilometer, or 0.6 mile, wide) crater that appears to be partly-filled by deposits that have flowed into, and around it. With this observation, scientists can learn more about the nature of these deposits. The crater offers an opportunity to gain more information about the flowing behavior of these deposits and their thickness given that the crater size can be used to estimate its depth. This provides insight into the thickness of the deposits partly filling it. https //photojournal.jpl.nasa.gov/catalog/PIA25897
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Mars digital-image mosaic merged with color of the MC-25 quadrangle, Thaumasia region of Mars. This image is from NASA's Viking Orbiter 1.
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The objective of this observation from NASA's Mars Reconnaissance Orbiter is to examine a light-toned deposit in a region of what is called 'chaotic terrain.' Some shapes suggest erosion by a fluid moving north and south.
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This image shows part of the steep wall of the caldera (a large volcanic crater) at the top of Ascraeus Mons, one of Mars' giant volcanoes. We can see chutes carved into the soft dust that has built up on the slope, with some similarities to gully landforms elsewhere on the planet.
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This image from NASA's Mars Reconnaissance Orbiter shows an arcuate ridge in Terra Meridiani.The ridge is most likely a former streambed, now exposed in inverted relief.
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NASA's Mars Reconnaissance Orbite observed this image of an isolated mountain in the Southern highlands reveals a large exposure of 'purplish' bedrock.
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This image, acquired by NASA's Mars Reconnaissance Orbiter, shows there are a few more fans on the ridge as spring activity progresses in Inca City.
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This HiRISE image shows a flat plain with various low, lumpy mounds. Some of them have distinct colors and tones unlike the surrounding plains, suggesting that they are made up of a different type of material. While the origin of these mounds is not certain, one idea that seems to fit best is that they are deposits left after eruptions of wet sediments onto the surface. This can happen when thick deposits of wet sand and mud are shaken, say from a meteorite impact, and the ground briefly loses its strength, allowing dirty water to be expelled from the deposit. On Earth, this process of liquefaction can happen during earthquakes. If this hypothesis is correct, it means that these mounds provide samples of a potentially habitable environment that we would otherwise need massive drills to reach.
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HiRISE commonly takes images of recent craters on Mars, which are usually found by the MRO Context Camera where they disturb surface dust. An impact site in this area was first imaged in December 2017. A year and a half later, the scene looks totally different! Dust has eroded from the surface, probably due to the planet-encircling dust storm from 2018. The dark spots around the fresh craters have vanished because they only affected the dust that has since disappeared. See if you can find the craters in the new image by comparing with the old one.
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The pits visible in this image from NASA's Mars Reconnaissance Orbiter aren't impact craters. The material they are embedded into is ejecta (stuff thrown out of an impact crater when it forms) from a large crater called Hale not seen in this image.
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This image from NASA's Mars Reconnaissance Orbiter captures light-toned ridges found in a large fracture located east of Holden Crater forming a curious box-like pattern.
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This picture of the rim of Eos Chasma in Valles Marineris, captured by NASA's Mars Reconnaissance Orbiter, shows active erosion of the Martian surface.
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This image from NASA's Mars Reconnaissance Orbiter shows a portion of a long valley system in northern Arabia Terra.
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Most of the oldest terrains on Mars have eroded into branching valleys, as seen here in by NASA's Mars Reconnaisance Orbiter, much like many land regions of Earth are eroded by rain and snowmelt runoff.
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Mars digital-image mosaic merged with color of the MC-22 quadrangle, Mare Tyrrhenum region of Mars. This image is from NASA's Viking Orbiter 1.
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This observation from NASA's Mars Reconnaissance Orbiter spacecraft shows a terrain of relatively smooth region that transitions into sharp ridges called yardangs on Apollonaris Patera.
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NASA's Curiosity Mars Rover drilled this hole to collect sample material from a rock target called 'Buckskin' on July 30, 2015, during the 1060th Martian day, or sol, of the rover's work on Mars. The diameter is slightly smaller than a U.S. dime.
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Impact craters form when an asteroid, meteoroid, or comet crashes into a planet's surface, causing an explosion. This impact crater is a little less than 3 kilometers in diameter as seen by NASA's Mars Reconnaissance Orbiter.
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Dunes in Holden Crater as Seen by Mars Reconnaissance Orbiter
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Chryse Outflow Channel, Mars, from Viking Orbiter
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The view of 'Chester Lake' from NASA's Mars rover Opportunity is presented in approximate true color. This 'natural color' is the rover team's best estimate of what the scene would look like if humans were there and able to see it with their own eyes.
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This false color image from NASA's Mars Reconnaissance Orbiter indicates that the volcanic cone in the Nili Patera caldera on Mars has hydrothermal mineral deposits on the southern flanks and nearby terrains.
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The High Resolution Imaging Science Experiment (HiRISE) camera aboard NASA's Mars Reconnaissance Orbiter captured these sand ripples and the large dune (at center) on Feb. 9, 2009. Color has been added to make textures easier to see. This area is in Proctor Crater at 47.8 degrees south latitude and 30.7 degrees east longitude.
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Ridges and Dark Patches Seen by Mars Reconnaissance Orbiter
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Volcanoes Ceraunius Tholus and Uranius Tholus
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This image hows the funnel-shaped terminus of Lethe Vallis, a winding channel in the Elysium Planitia region of Mars. MRO.
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Transverse aeolian ridges (TARs) are commonly found throughout the Martian tropics, including rocky regions such as Syrtis Major that are largely devoid of dust as seen by NASA's Mars Reconnaissance Orbiter.
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This image from NASA's Mars Reconnaissance Orbiter shows blocks of bright, layered rock embedded in darker material that are thought to have been deposited by a giant flood that occurred when Uzboi Valles breached the rim of Holden Crater.
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Ius Chasma is one of several canyons that make up Valles Marineris, the largest canyon system in the Solar System.
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This image from NASA's Mars Reconnaissance Orbiter shows the edge of the Martian South Polar layered deposit. The stack of fine layering is highlighted by the rays of the polar sun.
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In this complex crater (about 44-kilometers in diameter), we see bedrock in several locations from different depths in the crust. The central uplift exposes large fragments of green-toned bedrock that possibly originated from several kilometers beneath the surface. To the south of the crater, we see more of this bedrock along with material that was excavated and thrown out after the impact. In craters of this size, the rim is unstable and collapses inwards forming terraces, which occasionally exposes more bedrock that would have originated from close to the surface than the rocks exposed within the uplift itself. Central uplifts have better exposures of bedrock, but in this example the terraces steal the show, displaying beautiful green- and light-toned bedrock at multiple locations.
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Color mosaic of Olympus Mons volcano on Mars from the Viking 1 Orbiter. The mosaic was created using images from orbit 735 taken 22 June 1978. Olympus Mons is about 600 km in diameter and the summit caldera is 24 km above the surrounding plains.
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This map show a portion of Endeavour Crater's western rim that includes the 'Marathon Valley' area investigated intensively by NASA's Mars Exploration Rover Opportunity in 2015 and 2016.
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Near the lower left corner of this view is the three-petal lander platform that NASA's Mars Exploration Rover Spirit drove off in January 2004.
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This is the latest image of NASA's Opportunity rover at Solander Point, where it spend a few week investigation Pinnacle rock (the 'jelly donut') that was flipper over by the rover wheel. This observation is from NASA's Mars Reconnaissance Orbiter.
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This long image is entirely over the extensive central peak complex of Hale Crater. Of particular interest are bedrock outcrops and associated fine-grained sediments with different colors. This 153-kilometer diameter crater was named after American astronomer George Ellery Hale.
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A Martian dust devil was captured winding its way along the Amazonis Planitia region of Northern Mars on March 14, 2012 NASA's Mars Reconnaissance Orbiter.
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A delta is a pile of sediment dumped by a river where it enters a standing body of water. Evidence for deltas that formed billions of years ago on Mars has been mounting in recent years. This image is from NASA's Mars Reconnaissance Orbiter.
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Apollinaris Patera
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This image covers a pit in the lower West flank of Arsia Mons, one of the four giant volcanos of the Tharsis region.
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Mercator Projection of Huygens's View
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Meteor Impact Crater In The Libyan Desert, Egypt, True Colour Satellite Image. True colour satellite image of an impact structure in the Libyan desert, Egypt. Image taken on 9 November 1986 using LANDSAT data.
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Three impact craters of different sizes, arranged in the shape of a snowman, make up one of the most striking features on Vesta, as seen in this view from NASA's Dawn mission.
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This image from NASA's Dawn spacecraft shows a fresh scarp rimmed crater with many boulders on asteroid Vesta's crater floor. These boulders have diameters of 100-200m, which is roughly the size of many asteroids.
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This image taken by NASA's Mars Reconnaissance Orbiter shows a series of parallel layers eroding into peculiar knobs and hills.
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In the northern section of this from image NASA's Mars Reconnaissance Orbiter, we see flat terrain that is probably an ancient lava field. These dust avalanches are common in dust-covered regions on Mars.
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Smile! Spring has sprung in the martian southern hemisphere. With it comes the annual retreat of the winter polar frost cap. This view of Happy Face Crater --officially named Galle Crater --shows patches of white water ice frost in and around the crater's south-facing slopes. Slopes that face south will retain frost longer than north-facing slopes because they do not receive as much sunlight in early spring. This picture is a composite of images taken by the Mars Global Surveyor Mars Orbiter Camera (MOC) red and blue wide angle cameras. The wide angle cameras were designed to monitor the changing weather, frost, and wind patterns on Mars. Galle Crater is located on the east rim of the Argyre Basin and is about 215 kilometers (134 miles) across. In this picture, illumination is from the upper left and north is up. http //photojournal.jpl.nasa.gov/catalog/PIA02325
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July 25, 2005 - This Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) image shows a gullied crater wall in the Terra Sirenum region of Mars. The fluids that formed the gully channels and deposited debris in aprons at the base of the crater wall may have percolated through layers in the layered bedrock exposed in the crater wall. As fluid seeped out of the ground, it undermined overlying layers of rock, and caused the formation of several compex alcoves, higher in the crater wall. The formati
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Mars digital-image mosaic merged with color of the MC-29 quadrangle, Eridania region of Mars. This image is from NASA's Viking Orbiter 1.
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Spider-shaped features in the south polar region of Mars are carved by vaporizing dry ice in a dynamic seasonal process. Mars Reconnaissance Orbiter.
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Hadriaca Patera
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NASA's Mars Reconnaissance Orbiter acquired this image to aid in the search for the missing lander, Mars 2. If the debris field is found, it could serve as a future landing location to study the effects of crash landing on the Martian surface.
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Evidence of Flood Waters on Mars
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Opportunity at Crater's 'Cape Verde'
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Mars digital-image mosaic merged with color of the MC-10 quadrangle, Lanae Palus region of Mars. This image is from NASA's Viking Orbiter 1.
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This March 18, 2015, view from the Mast Camera on NASA's Curiosity Mars rover shows a network of two-tone mineral veins at an area called 'Garden City' on lower Mount Sharp.
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Every Martian spring, fans of dust are blown out from under the seasonal layer of carbon dioxide ice that forms a polar cap over the winter. Gas blowing out from under the ice carries with it a load of dust that is deposited on the surface in a direction determined by the wind at the time of the eruption. Like windsocks, these fans in a polar area we've dubbed Macclesfield, record the direction that the wind was blowing. A citizen science task at Planet Four enlists the public to outline the fans. Their measurements go into a data base that will ultimately help us to understand weather on Mars.
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Rover's Wheel Churns Up Bright Martian Soil
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Mars digital-image mosaic merged with color of the MC-6 quadrangle, Casius region of Mars. This image is from NASA's Viking Orbiter 1.
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An oblique, color image of central Valles Marineris, Mars showing relief of Ophir and Candor Chasmata; view toward east. The photograph is a composite of Viking high-resolution images in black and white and low-resolution images in color.
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Terrain in Mawrth Vallis Region Seen by Mars Reconnaissance Orbiter
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NASA's Mars Reconnaissance Orbiter (MRO) observed this image of Ganges Chasma in the northeast portion of Valles Marineris, and opens into outflow channels that flowed to the north. Scattered hills on the canyon floor may be remnants of chaos terrain that formed from collapse of the canyon. Some of the bedrock has diverse colors. More information is available at
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This image from NASA's Mars Reconnaissance Rover shows a degraded impact crater in the southern highlands. Part of the crater rim is visible at the top and bottom of the image, with the boulder-covered crater floor in the center.
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The Ever-Changing Swiss Cheese of Mars. Mars has a small South Polar cap of carbon dioxide ice. Although this cap persists year round, it is always changing it has pits and mesas that in some places resemble a slice of Swiss cheese. The pits are expanding because the carbon dioxide is sublimating, but in other places new carbon dioxide deposits are building up on flat ground. HiRISE monitors many areas of the cap to study these changes. Usually when we study changes, we can align the images with features that haven't changed, but here that is difficult nearly everything is different! By lining up the pattern of shallow pits on top of a mesa, which are not changing much, we can see the variations in the eight Mars years between observations (PSP_004992_0945 and this one). Some of the walls have retreated by more than 15 meters (about 50 feet).
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NASA's Curiosity Mars rover and its tracks are visible in this view combining information from three observations by the HiRISE camera on NASA's Mars Reconnaissance Orbiter. You need 3-D glasses to view this image.