This VIS image shows are region of lava covered plains east of Olympus Mons. Winds are common in the area and have created windstreaks downwind of craters in the region and on the lava flows.
Chaotic terrains on Mars are disorganized regions of blocks and large mounds which appear to have been produced by the collapse of pre-existing terrain.
This unnamed crater in the far northern lowlands contains a sand sheet with dune forms on its floor. Many craters this close to the pole contain similar dune fields.
This image shows a landslide in the Coprates Chasma region of Valles Marineris that occurred when a large unstable area of rock broke away from the cliffs along the top of the image.
This image spans the floor and two walls of a pit in Noctis Labyrinthus, a system of deep, steep-walled valleys on the western edge of Valles Marineris.
Nili Fossae, a series of tectonic fractures, is the low region on the right side of this image. A small channel is visible draining into the large tectonic depression.
The region southwest of Olympus Mons is covered with materials that have been eroded by the wind. Surface materials in this area indicate wind action in many different directions.
Understanding what kinds of materials formed the layers, how they were set in place, and how they have evolved will provide insight into Martian geologic history.
It's possible that the flanks of Arsia Mons contain ice-rich material possibly deposited during a different obliquity (tilt of Mars' spin axis) or climate regime.
Valley networks are thought to have formed by groundwater sapping either in conjunction with an ice layer to cover the running water or during a past warmer, wetter climate regime on Mars.