"Mass wasting" is a geologic term that encompasses the rapid downhill movement of rocks and fine particles due to the force of gravity.
One of the most common and generic types of mass wasting features on Earth are landslides, but there are many others such as rock
falls, debris flows, soil creep, and debris avalanches.
Landslides or any other mass wasting feature, require some type of triggering mechanism to induce the movement of particles under gravity. Some of these
mechanisms include volume expansion of fractures (i.e. cracks) in rocks by freeze/thaw processes, increase in soil pore pressure (i.e. water content),
undermining or removal of less-resistant material below a stronger material layer, and strong vibrational forces produced from above (e.g., meteorite impact) or
below ground (e.g., volcanic eruption, earthquake).
On Mars, two of the most common mass wasting features are landslides and dust
avalanches (also referred to as slope streaks). Some of the most spectacular landslides in the solar system are found in the Valles
Marineris canyon system on Mars and exhibit many of the classic characteristics of landslides on Earth. These characteristics
include a semi-circular main scarp in the source region, a hummocky (i.e. irregular) or blocky surface in the upper portion of the deposit,
surface ridges parallel to landslide flow direction in the middle portion of the deposit, and a lobate outer margin that has some
significant thickness (e.g., tens to hundreds of meters). Dust avalanches are common on dune faces, crater interior walls, mesa slopes,
and canyon scarps. The streaks are thought to occur when dust and/or other small particles on a sloped surface begins to move due
to sublimation of a thin layer of water frost or by the over-steepening of slopes in localized dusty air fall deposits.
For more information about landslides on Earth, click here.
Major Science Questions for This Theme
What are the current and past rates for mass wasting in various terrains on Mars?
Do slope streaks involve water in their triggering and subsequent downslope movement?
What triggers large landslides (e.g., Marsquakes, tectonic oversteepening of slopes, fluvial and/or eolian undercutting of slopes,
weakening of rock materials from hydrothermal, physical, or chemical weathering)?
Can one type of mass wasting feature be clearly distinguished from another on the basis of boulder frequency and distribution?
Features of Interest Potentially Visible at HiRISE Scale
Boulders: The sizes, shapes, sorting, colors, and distribution of boulders (~0.5 meters or larger in diameter)
tell us a great deal about the transport process of mass wasting features. For slope streaks or other small mass wasting features,
stereo coverage from HiRISE images may help resolve the topography or morphologies that are diagnostic of these processes.
Ridges: small ridges that can be seen in HiRISE images, but are too small or
subtle to be seen in Mars Orbiter Camera (MOC) images, may be an indicator of a change in direction or rate of movement for
landslide deposits or other larger mass wasting features. Faults—small offsets in the deposit layers such as along fractures
or faults—may be an indicator compressional flow of materials in parts of the mass wasting feature.