Seasonal flows on warm Martian slopes are thought to be either salty water flows occurring during the warmest months on Mars, or dry grains that "flow" downslope of at least 27 degrees.
Reprojected view of warm-season flows in Newton Crater
Close, color view of recurrent slope lineae, as seen by HiRISE under HiWish program Arrows point to some of the recurrent slope lineae. Fan may have been built up by past recurrent slope lineae.
Recurrent slope lineae elongate when the slopes are at their warmest. Near the equator, RSL elongate on northern slopes in the northern summer and on the southern slopes in the southern summer.
Ice (white), salt (red) and warm-season flows (blue) on Mars
Valles Marineris
Videos
Valles Marineris is a system of canyons that runs along the Martian surface east of the Tharsis region. At more than 4,000 km long, 200 km wide and up to 7 km deep, Valles Marineris is the largest can
Valles Marineris stretches over 4,000 km (2,500 mi) across Mars, mostly east-west just below the equator, as seen in this Viking 1 orbiter image mosaic.
Valles Marineris in mosaic of THEMIS infrared images from 2001 Mars Odyssey
Valles Marineris with major features labeled.
Morning water ice fog spills out of Noctis Labyrinthus (Viking 1 orbiter image)