Image Context:


Wide Context:

Context image credit: NASA/JPL/MOLA
View on map

These windstreaks are located on lava flows from Arsia Mons.

Source: THEMIS - Mars Odyssey Mission

Image Context:


Wide Context:

Context image credit: NASA/JPL/MOLA
View on map

This image captured part of one of the larger storms that occurred during the latest spring season on Mars. Southern spring is the season of dust storms. This storm is located over Promethei Terra.

Source: THEMIS - Mars Odyssey Mission

Image Context:


Wide Context:

Context image credit: NASA/JPL/MOLA
View on map

This dune field is located in a small unnamed crater of the western edge of the Argyre Basin.

Source: THEMIS - Mars Odyssey Mission

Image Context:


Wide Context:

Context image credit: NASA/JPL/MOLA
View on map

Dust devil tracks are a common feature in the southern hemisphere of Mars. These streaks are located in Promethei Terra, the site of the major dust storm image several days ago.

Source: THEMIS - Mars Odyssey Mission

Wow always love checking up on these photos god what i would give to walk around on mars

Image Context:


Wide Context:

Context image credit: NASA/JPL/MOLA
View on map

This VIS image shows part of the rim of Huygens Crater. The rim is deeply incised with channels.

Source: THEMIS - Mars Odyssey Mission

Image Context:


Wide Context:

Context image credit: NASA/JPL/MOLA
View on map

This image show where Allegheny Vallis intersects Ophir Cavus (the canyon at the bottom of the frame).

Source: THEMIS - Mars Odyssey Mission

Image Context:


Wide Context:

Context image credit: NASA/JPL/MOLA
View on map

The border between clear and cloudy in this image is likely the edge of a polar trough, with the clouds located in the trough itself. It is common during the spring in the southern hemisphere for clouds and haze to obscure the polar cap.

Source: THEMIS - Mars Odyssey Mission

Image Context:


Wide Context:

Context image credit: NASA/JPL/MOLA
View on map

At one time the floor of this unnamed crater west of Hellas Basin was completely filled with material from rim to rim. As this image shows, part of that fill material is being removed. The hole that is formed shows that the fill material was layered. A very rough surface is located at the bottom of the hole.

Source: THEMIS - Mars Odyssey Mission

Image Context:


Wide Context:

Context image credit: NASA/JPL/MOLA
View on map

This isolated hill is located south of Reull Vallis on the eastern margin of Hellas Basin. Material from the hill is collecting at the base of the hill. The surface patterns on the top of the material indicate that volitiles may be involved in the flow of the material downhill.

Source: THEMIS - Mars Odyssey Mission

Image Context:


Wide Context:

Context image credit: NASA/JPL/MOLA
View on map

These lava flows are located between Syria Planum and Solis Planum and probably originated from volcanic vents in Syria Planum.

Source: THEMIS - Mars Odyssey Mission

Image Context:


Wide Context:

Context image credit: NASA/JPL/MOLA
View on map

This image shows part of Reull Vallis, a large channel which originates in Promethei Terra and empties into Hellas Basin.

Source: THEMIS - Mars Odyssey Mission

Image Context:


Wide Context:

Context image credit: NASA/JPL/MOLA
View on map

These dust devil tracks are located in Noachis Terra.

Source: THEMIS - Mars Odyssey Mission

Image Context:


Wide Context:

Context image credit: NASA/JPL/MOLA
View on map

The arcuate fractures and broken up surface shown in this image is called Avernus Colles [colles means small hills or knobs]. This unique surface has developed on the southeast margin of Elysium Plainitia.

Source: THEMIS - Mars Odyssey Mission

Image Context:


Wide Context:

Context image credit: NASA/JPL/MOLA
View on map

This image of Aeolis Planum shows the long term effect of wind on soft/poorly cemented material. Stretching from just south of Olympus Mons to Aeolis Planum is a region called the Medusa Fossae Formation. MFF is materials that are completely sculpted by the wind.

Source: THEMIS - Mars Odyssey Mission

Image Context:


Wide Context:

Context image credit: NASA/JPL/MOLA
View on map

These dark sand dunes and nearby dust devil tracks are located on the floor of Green Crater.

Source: THEMIS - Mars Odyssey Mission

Image Context:


Wide Context:

Context image credit: NASA/JPL/MOLA
View on map

The dust devil tracks in this region of Noachis Terra are found on the plains and within craters.

Source: THEMIS - Mars Odyssey Mission

Image Context:


Wide Context:

Context image credit: NASA/JPL/MOLA
View on map

This infrared image shows part of Zephyria Planum. This region is well named, Zephyria is one of the winged mares of Selene (the moon goddess of Greek mythology), and this region has been subject to intense wind activity. Each level of surface in this image records a different wind direction. Note the small double-circle opening in the thumbnail which reveals a surface etched in a NW/SE direction beneath one etched by the wind in a NNW/SSE direction.

Source: THEMIS - Mars Odyssey Mission

Image Context:


Wide Context:

Context image credit: NASA/JPL/MOLA
View on map

These dark sand dunes are found in Hellas Basin, location of the lowest elevations on Mars.

Source: THEMIS - Mars Odyssey Mission

Image Context:


Wide Context:

Context image credit: NASA/JPL/MOLA
View on map

This image shows a small portion of Amphitrites Patera. The odd surface texture is also seen on Peneus Patera. Both paterae are thought to be ancient volcanoes, and both are located near the south pole.

Source: THEMIS - Mars Odyssey Mission

Image Context:


Wide Context:

Context image credit: NASA/JPL/MOLA
View on map

These dust devil tracks are located in Malea Planum.

Source: THEMIS - Mars Odyssey Mission

Image Context:


Wide Context:

Context image credit: NASA/JPL/MOLA
View on map

This image shows a small portion of Iani Chaos. The different tones and surface textures indicate that different types of material exist in this region.

Source: THEMIS - Mars Odyssey Mission

Image Context:


Wide Context:

Context image credit: NASA/JPL/MOLA
View on map

These sand dunes are located on the floor of Wirtz Crater. Wirtz Crater is one of the candidate MSL (Mars Sceince Laboratory) landing sites.

Source: THEMIS - Mars Odyssey Mission

Image Context:


Wide Context:

Context image credit: NASA/JPL/MOLA
View on map

These dunes are located on the floor of an unnamed crater in Terra Cimmeria. While the dune field is approximately the same size as in yesterday's image, the dune form is very different. The difference may be due to different wind conditions, the availability of sand, or the texture of the crater floor.

Source: THEMIS - Mars Odyssey Mission

Image Context:


Wide Context:

Context image credit: NASA/JPL/MOLA
View on map

This hill, called Euripus Mons, is surrounded by debris flow. Euripus Mons is located just east of Hellas Basin, in a region where most of the hills are shedding material and forming debris flows.

Source: THEMIS - Mars Odyssey Mission

Image Context:


Wide Context:

Context image credit: NASA/JPL/MOLA
View on map

These short, dark dust devil tracks are located in Argyre Basin.

Source: THEMIS - Mars Odyssey Mission

Image Context:


Wide Context:

Context image credit: NASA/JPL/MOLA
View on map

The right margin and bottom of this image shows a portion of Dao Vallis. The channel of Dao Vallis is very complex and contains regions of chaos.

Source: THEMIS - Mars Odyssey Mission

Image Context:


Wide Context:

Context image credit: NASA/JPL/MOLA
View on map

One of the most interesting features of Maunder Crater is the large trough seen in this image. The crater rim is in the bottom portion of the image and the floor is to the top of the 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. How and why the trough came to be is unknown.

Source: THEMIS - Mars Odyssey Mission

Image Context:


Wide Context:

Context image credit: NASA/JPL/MOLA
View on map

The fractures and graben seen in the image are part of the highland called Claritas Rupes. Claritas Rupes extends southward from the western edge of Noctis Labyrinthus and divides the volcanic flows of Deadalia Planum and Solis Planum.

Source: THEMIS - Mars Odyssey Mission

Image Context:


Wide Context:

Context image credit: NASA/JPL/MOLA
View on map

This image of Coprates Chasma illustrates a common issue when imaging the bottom of Valles Marineris - haze in the canyon. The top of the canyon walls are clearly visible, while the floor is indistinct due to hazy conditions.

Source: THEMIS - Mars Odyssey Mission

Image Context:


Wide Context:

Context image credit: NASA/JPL/MOLA
View on map

This VIS image covers half of an unnamed crater south of Coprates Chasma. This type of crater is termed a "central peak" crater. Note the central rise on the floor of the crater. This rise or peak was formed by rebound of the ground during the impacting event and crater formation.

Source: THEMIS - Mars Odyssey Mission

Image Context:


Wide Context:

Context image credit: NASA/JPL/MOLA
View on map

Small bright dunes occur along the margins of the graben that crosses this image. The graben is an extension of Noctis Labyrinthus into Sinai Planum.

Source: THEMIS - Mars Odyssey Mission

Image Context:


Wide Context:

Context image credit: NASA/JPL/MOLA
View on map

This field of dark sand dunes is located on the floor of an unnamed crater is Terra Sirenum.

Source: THEMIS - Mars Odyssey Mission

Image Context:


Wide Context:

Context image credit: NASA/JPL/MOLA
View on map

Gullies occur on the interior of the rim of this unnamed crater in Terra Sirenum. This crater is located on the rim and ejecta blanket of a larger crater.

Source: THEMIS - Mars Odyssey Mission

Image Context:


Wide Context:

Context image credit: NASA/JPL/MOLA
View on map

This VIS image shows part of the flank of the Arsia Mons volcano. Rather than the rough surface typical of the young Arsia Mons lava flows found around the foot of the volcano, the surface of the flank comprised of small ridges and honeycomb-like depressions. It is likely that this surface has been modified since the last flow coated the surface.

Source: THEMIS - Mars Odyssey Mission

Image Context:


Wide Context:

Context image credit: NASA/JPL/MOLA
View on map

Any place that wind blows over poorly consolidated material erosion will occur. This image shows erosion and the removal of material in a region just southeast of Apollineris Patera. The material may be volcanic ash from the nearby patera.

Source: THEMIS - Mars Odyssey Mission

Image Context:


Wide Context:

Context image credit: NASA/JPL/MOLA
View on map

This unnamed central peak crater east of Hadriaca Patera is slowly being modified from its original pristine state. The crater rim is cut by multiple channels and part of the rim has failed due to gravity and produced a landslide that reached all the way to the central peak itself (to the left of the channels in the center of the image).

Source: THEMIS - Mars Odyssey Mission

Image Context:


Wide Context:

Context image credit: NASA/JPL/MOLA
View on map

This VIS image shows a small portion of Australe Mensa, part of the South Pole of Mars. How these different textures form is still being studied. The central part of the image contains a texture called "swiss-cheese" because of its holey appearance. Below that is "thumbprint" texture. "Swiss-cheese" appears to become "thumbprint".

Source: THEMIS - Mars Odyssey Mission

Image Context:


Wide Context:

Context image credit: NASA/JPL/MOLA
View on map

These windstreaks are located on lava flows from Arsia Mons.

Source: