Mars and Planetary Imagery

Black and white images from Mars Odyssey showing various Martian terrains, emphasizing geological features and polar caps.

Detail of an Impact Crater, Acidalia Planitia

In this image from NASA's Mars Odyssey, a mantling layer of sediment slumps off the edge of a mesa in Candor Chasma producing a ragged pattern of erosion that hints at the presence of a volatile component mixed in with the sediment.

Jupiter's Equatorial Region in a Methane Band (Time Set 3)

This image captured by NASA's 2001 Mars Odyssey spacecraft shows part of the north polar cap. This image is along the cap margin.

As spring progresses at the south pole, the surface reacts to the change of season. This image from NASA's 2001 Mars Odyssey spacecraft shows a region of the south pole that is monitored throughout spring, summer, and fall at the south pole.

This image captured by NASA's 2001 Mars Odyssey spacecraft shows the north polar scarp, with the polar cap in the upper left corner.

The windstreaks in this image captured by NASA's 2001 Mars Odyssey spacecraft are located on Tharsis volcanic flows east of Pavonis Mons.

Detail of an Impact Crater, Acidalia Planitia

This VIS image shows 'streamers' of clouds created by katabatic winds at the north polar cap. Katabatic winds are created by cold air sinking at the pole and then speeding along the ice surface towards the edge of the polar cap. When the winds enter troughs the wind regime changes from laminar flow to choatic and clouds of ice particles and/or dust are visible. This wind activity peaks at the start of northern hemisphere summer. Orbit Number 53942 Latitude 86.8433 Longitude 99.3149 Instrument VIS Captured 2014-02-10 10 50

Today's VIS image shows part of eastern Hebes Chasma. The floor of the chasma is covered with chaotic materials, some from landslides and other layered deposits of unknown origin. Hebes Chasma is a closed basin north of Valles Marineris. It measures 126km wide north/south (78 miles), 315 km long east/west (196 miles), and 8 km (5 miles) at its deepest point. Orbit Number 88001 Latitude -1.32567 Longitude 284.971 Instrument VIS Captured 2021-10-16 07 20

South Polar Ice. Today's VIS image shows part of the south polar cap. This image was taken at the end of southern summer. The cap was created over millions of years with deposition of ice and dust during different seasons, creating layers. The ice surface contains several different textures which can be seen in this image. The south polar cap is called Australe Planum. Orbit Number 93158 Latitude -87.0114 Longitude 273.846 Instrument VIS Captured 2022-12-14 21 58 https //photojournal.jpl.nasa.gov/catalog/PIA25845

This 2001 Mars Odyssey image of Jeans Crater shows a sand sheet with dune forms and a layered region to the south of the sand sheet.

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

Located 1200 kilometers (about 745 miles) south of the giant shield volcano Arsia Mons, this infrared temperature image from NASA's Mars Odyssey spacecraft shows the flow margin of a young lava flow from Arsia that covers a much older flow.

Ius Chasma. Today's VIS image shows part of Ius Chasma and one of its mega gullies (bottom of image). Ius Chasma is unique from the other chasmata of Valles Marineris in possessing mega gullies on both sides of the chasma. The largest mega gullies are located in Sinai Planum, dissecting those plains and emptying into the canyon. Mega gullies are thought to be sapping channels caused by groundwater flow and erosion. The Earth analog is springs - water that flows underground and then breaches the surface creating channels. The morphology of the Mars gullies mirrors terrestrial springs. The channel is fairly uniform in width and the head of the channel is rounded like an amphitheater. The channel lengthens by erosion at the head backwards as the surface where the spring emerges is undercut. For Mars it is theorized that subsurface water would stay liquid due to underground heating. Ius Chasma is at the western end of Valles Marineris, south of Tithonium Chasma. Valles Marineris is over 40

Cydonia: Two Years Later

NASA's Voyager spacecraft was 8.6 million kilometers (5.3 million miles) from Neptune when it took this 61 second exposure through the clear filter with the narrow angle camera on August 19, 1989.

This image captured by NASA's 2001 Mars Odyssey spacecraft looks a plank of wood, with a beautiful grain to it. Orbit Number 64928 Latitude -86.5268 Longitude 158.521 Instrument VIS Captured 2016-08-02 23 46

Pits on Ascraeus

Today's VIS image shows the upper elevations of Olympus Mons, including part of the summit caldera. Scarps and extensional features (graben) record multiple stages of caldera collapse at the summit of Olympus Mons. Olympus Mons is the largest volcano in the solar system, reaching heights over 40 km (25 miles) tall from base to summit, with the base covering an area as large as the state of Arizona. For comparison, Mauna Loa is 9 km (5.5 miles) tall measured from its base on the sea floor. Orbit Number 90561 Latitude 17.6564 Longitude 226.782 Instrument VIS Captured 2022-05-15 02 28

Dust Devil Tracks

Don't be afraid, this image captured by NASA's 2001 Mars Odyssey spacecraft looks like a ghost! Orbit Number 58468 Latitude -85.1331 Longitude 47.4519 Instrument VIS Captured 2015-02-17 23 28

Icy particles in the cloud around Hartley 2, as seen by NASA's EPOXI mission spacecraft. A star moving through the background is marked with red and moves in a particular direction, with a particular speed; icy particles move in random directions.

As the sun warms the surface and more frost is removed, the dunes and other features near the north pole of Mars are revealed. This image from NASA's Mars Odyssey shows that the inter-dune areas are complex.

South Polar Ice. Today's VIS image shows part of the south polar cap. This image was taken at the end of southern summer. The cap was created over millions of years with deposition of ice and dust during different seasons, creating layers. The ice surface contains several different textures which can be seen in this image. The south polar cap is called Australe Planum. Orbit Number 93142 Latitude -86.9334 Longitude 11.9312 Instrument VIS Captured 2022-12-13 14 21 https //photojournal.jpl.nasa.gov/catalog/PIA25843

The unusual and apparently layered surface in this image is located in Aureum Chaos

The dark, narrow band of sand dunes in this image from NASA's 2001 Mars Odyssey spacecraft is called Hyperboreae Undae.

This image captured by NASA's Mars Odyssey shows parts of two giant gully that are located on the southern side of Ius Chasma. Ius Chasma has the largest number of mega gullies of any of the chasmata that make up Valles Marineris.

This image shows clouds in the mid-southern latitudes of Saturn's largest moon, Titan, one of a series of images captured by NASA's Cassini spacecraft a few months after fall began in the southern hemisphere.

V 5964. Thule (depicted name)

Day And Night In Terra Meridiani

The complex dune forms in this VIS image are located on the floor of Russell Crater. The large ridge dune is unique to Russell Crater. Russell Crater is located in Noachis Terra and is 135km (83miles) in diameter. Orbit Number 82807 Latitude -54.2373 Longitude 13.1536 Instrument VIS Captured 2020-08-14 15 11

This image captured by NASA's 2001 Mars Odyssey spacecraft shows sand dunes on the floor of an unnamed crater in Terra Sirenum.

The Road Less Traveled (right eye)

Between July 10 and 12, 2017, the Larsen C Ice Shelf in West Antarctica calved one of the largest icebergs in history (named A-68 ), weighing approximately one trillion tons. The rift in the ice shelf that spawned the iceberg has been present on the shelf since at least the beginning of the Landsat era (approximately the 1970s), but remained relatively dormant until around 2012, when it was observed actively moving through a suture zone in the ice shelf (Jansen et al., 2015). Suture zones are wide bands of ice that extend from glacier grounding lines (the boundary between a floating ice shelf and ice resting on bedrock) to the sea comprised of a frozen mixture of glacial ice and sea water, traditionally considered to be stabilizing features in ice shelves. When the Antarctic entered its annual dark period in late April, scientists knew the rift only had a few more miles to go before it completely calved the large iceberg. However, due to the lack of sunlight during the Antarctic winter

This VIS image shows part of Candor Chasma.

'Columbia Hills' Oblique View

$Tithonium Chasma. Today's VIS image shows the part of the eastern end of Tithonium Chasma. Tithonium Chasma is at the western end of Valles Marineris. Valles Marineris is over 4000 kilometers long, almost as wide as the United States. Tithonium Chasma is almost 810 kilometers long (499 miles), 50 kilometers wide and over 6 kilometers deep. In comparison, the Grand Canyon in Arizona is about 175 kilometers long, 30 kilometers wide, and only 2 kilometers deep. The canyons of Valles Marineris were formed by extensive fracturing and pulling apart of the crust during the uplift of the vast Tharsis plateau. In this image, the shallower regions of Tithonium are visible. The northern cliff of Ius Chasma is visible at the bottom of the image. Orbit Number 92650 Latitude -5.20867 Longitude 275.913 Instrument VIS Captured 2022-11-03 01 37 https //photojournal.jpl.nasa.gov/catalog/PIA25767$

This image captured by NASA's 2001 Mars Odyssey spacecraft shows part of an area just off the margin of the south polar cap. The bright and dark markings are identical to some seen on the cap, telling us that ice is located at the surface.

South Polar Turbulence

Naming New Lands - October Flyby

MOC View of Mars98 Landing Zone - 1/16/98

Aerial view of a part of the area affected during the flood disaster of 1953. Note: The description of this photo is not yet complete and will be supplemented on the basis of the data available at a later stage. However, of many photos of the flood disaster 1953, the location is unknown.

This VIS image shows more of the variety of textures on the south polar cap. Orbit Number 68068 Latitude -86.1964 Longitude 308.717 Instrument VIS Captured 2017-04-18 16 22

. Charlier Crater Dunes. This VIS image shows part of the large sand sheet with surface dune forms on the floor of Charlier Crater in Terra Sirenum. Orbit Number 91804 Latitude -68.028 Longitude 190.573 Instrument VIS Captured 2022-08-25 10 08

Beside 'Vostok Crater'

Opportunity's Surroundings After Sol 2220 Drive (Vertical)

Dunes cover all but the highest hill of this image captured by NASA's 2001 Mars Odyssey spacecraft. These dunes are part of Olympia Undae, a huge dune field located near the north pole.

Herschel's Dunes

Map of Enceladus

Hotei Arcus in Infrared

Sulphur Dioxide on the Chaac Region of Io

Images from NASA's Mars Odyssey spacecraft were used to create this mosaic of nighttime infrared images of Gusev Crater, which has been draped over topography data obtained by NASA's Mars Global Surveyor.

This VIS image captured by NASA's 2001 Mars Odyssey spacecraft shows a small area just off the margin of Mars' southern polar cap.

Polar Dust Storm

No NASA Mars orbiter has been in a position to observe morning daylight on Mars since the twin Viking orbiters of the 1970s. This image, taken by Viking Orbiter 1 on Aug. 17, 1976, shows water-ice clouds in the Valles Marineris area of equatorial Mars.

Polar surface winds can reach high velocities. These winds can cause clouds to form when the winds flow into troughs and become chaotic. This image from NASA's Mars Odyssey shows trough clouds as linear bands.

This radar image mosaic of Venus from NASA's Magellan spacecraft, is in the Lada region. The mosaic shows a system of east-trending radar-bright and dark lava flows encountering and breaching a north-trending ridge belt (left of center).

Very High Resolution View of Io's Surface

Dust Mantle Near Pavonis Mons

Almost all of the hydrocarbon seas and lakes on the surface of Saturn's moon Titan cluster around the north pole, as can be seen in this mosaic from NASA's Cassini mission.

View from West of Victoria Crater, Sol 1664

This daytime 2001 Mars Odyssey image of Terra Cimmeria shows dunes occurring both on crater floors and on the plains between the craters.

Opportunity's Sol 446 Position, with Relative Heights

These images, taken on February 19, 1997 by NASA's Galileo orbiter, show two of the three long-lived White Ovals that formed to the south of the Jupiter's Great Red Spot.

With its Multispectral Visible Imaging Camera (MVIC), half of the Ralph instrument, New Horizons captured several pictures of mesoscale gravity waves in Jupiter's equatorial atmosphere.

Follow the Fault

$A fracture on the Moon's surface, located in the northeastern floor of Alphonsus crater.$

Seeing 'Endurance' Through Infrared Eyes

Titan in Near-Infrared Light

Dry Ice Etches Terrain

Patches of Remnant Frost/Snow on Crater Rim in Northern Summer

Opportunity's View, Sol 381

The edge of the south polar cap is the bright band in the center of this image captured by NASA's 2001 Mars Odyssey spacecraft.

This image from NASA's Mars Odyssey spacecraft shows Rampart crater in Utopia Planitia, west of NASA's Viking 2 landing site.

In this image the martian surface is completely hidden from view by thick clouds. The thickness of the clouds indicates the dust is a major component of the clouds

Today's VIS image crosses both Ophir Chasma (top) and Candor Chasma (bottom). Layered and eroded material covers the floors of both chasmata. Both canyons are part of Valles Marineris. Often called the grand canyon of Mars, Valles Marineris extends over 3,000 kilometers (1864 miles) long, spans as much as 600 kilometers across, and as deep as 8 kilometers. By comparison, the Earth's Grand Canyon in Arizona, USA is 800 kilometers long, 30 kilometers across, and 1.8 kilometers deep. Orbit Number 84551 Latitude -4.18643 Longitude 286.548 Instrument VIS Captured 2021-01-05 04 50

Spirit's View on Sol 124 (left eye)

This movie was taken by Deep Impact's flyby spacecraft shows the flash that occurred when comet Tempel 1 ran over the spacecraft's probe. It was taken by the flyby craft's medium-resolution camera.

This image of the surface of comet Tempel 1 was taken about 20 seconds before NASA's Deep Impact's probe crashed into the comet on July 3, 2005. This particular region contains the impact site.

This image captured by NASA's 2001 Mars Odyssey spacecraft shows that the seasonal change in weather is not constrained to just the polar region.

Earth Observations taken by Expedition 34 crewmember.

Three of Titan's major surface features-dunes, craters and the enigmatic Xanadu-appear in this radar image from NASA's Cassini spacecraft. The hazy bright area at the left that extends to the lower center of the image marks the northwest edge of Xanadu.

This full resolution mosaiced image covers an area located in the Lakshmi region of Venus.

Aerial view of a part of the area affected during the flood disaster of 1953. Note: The description of this photo is not yet complete and will be supplemented on the basis of the data available at a later stage. However, of many photos of the flood disaster 1953, the location is unknown.

This infrared image from NASA's 2001 Mars Odyssey spacecraft shows part of the dune field on the floor of Rabe Crater. The dunes are 'brighter' than the surrounding material, indicating that they are warmer.

Mimas and the Rings

Brachiopod, 1904 - 1906, by James McDonald.

Large Dust Devil on Horizon, Sol 468

The region surrounding the South Polar Cap contains many different terrain types. This image from NASA's 2001 Mars Odyssey spacecraft shows both etched terrain and a region of 'mounds.'

High-resolution View of Gullies

Zephyria Channel System

NASA's Deep Impact's flyby spacecraft shows the flash that occurred when comet Tempel 1 ran over the spacecraft's probe taken by the high-resolution camera over a period of 40 seconds.

Proctor Crater Dunes. This VIS image displays sand dunes within Proctor Crater. 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. In this case, there are few clear slipfaces that would indicate the downwind direction. The crests of the dunes also typically run north-south in the image. This dune form indicates that there are probably two prevailing wind directions that run east and west (left to right and righ

Cloud Interactions

The THEMIS VIS camera contains 5 filters. The data from different filters can be combined in multiple ways to create a false color image. These false color images may reveal subtle variations of the surface not easily identified in a single band image. Today's false color image shows part of Dawes Crater. Dawes Crater is located in Terra Sabaea and is 185 km (115 miles) in diameter. Orbit Number 71178 Latitude -9.23145 Longitude 37.0457 Instrument VIS Captured 2017-12-30 22 27

The low albedo feature known as Senkyo is visible through the haze of Titan's atmosphere in this image captured by NASA's Cassini spacecraft.

As Cassini watches the rings pass in front of brightred giant star Aldebaran, the star's light fluctuates, providing information about the concentrations of ring particles within the various radial features in the rings

Nili Fossae in Color

NASA's Terra spacecraft captured this image of the growing oil spill in the Gulf of Mexico on May 7, 2010. The thickest parts of the oil spill appear as dark grey, filamentous masses in the southern part of the image, extending off of the bottom.

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