Is the sinuous ridge here a “fluvial-ridge,” i.e., an inversion of a fluvial sediment deposit? It is important…
This image suggestion outlines a contact between gypsum-rich dunes in Olympia Undae and flat-lying layers of the basal…
This closeup of a HiRISE image covers a region in the Eridania Basin that shows interesting inverted ridges (white arrows).
This obsevation focuses a ridge that is standing above the old lava surface of the floor of Echua Chasma.
HiRISE monitors dune fields across Mars to track how they are changing. The mobile sand also cleans dust off of the bedrock in inter-dune areas, providing good views of the bedrock structures and colors.
This observation features an amazing variety of surface terrain and araneiform structures that we dub “spiders.”
The lava appears to overlay sand and sedimentary deposits, so finer scale This image shows a potential outflow channel near Huo Hsing Vallis into an old crater.
A dominant driver of surface processes on Mars today is aeolian (wind) activity. In many cases, sediment from this activity is trapped in low-lying areas, such as craters.
It has been known since the 1970s when the Viking orbiters took pictures of Mars that there are large (i.e., several kilometers-thick) mounds of light-toned deposits within the central portion of Valles Marineris.
Sometimes, we acquire an image for the simple reason of getting either more coverage of an area, and/or to complete a mosaic of a particular spot.