Most gullies on Mars are believed to have been formed by liquid water, either through surface runoff or groundwater seepage. While gas-formed gullies do exist, they are considered a less common occurrence and are often associated with specific regional or environmental conditions.
Areas on Mars that exhibit gas-formed gullies tend to have certain characteristics that favor the production and release of gases. These conditions may include the presence of volatile-rich materials, such as carbon dioxide or methane, and specific topographic features that facilitate the accumulation and movement of gases. Some of the known regions on Mars with gas-formed gullies include the Hellas Basin, Valles Marineris, and the Candor Chasma region.
It is worth noting that the study and identification of gas-formed gullies on Mars are still ongoing areas of research. As our understanding of the Martian climate, geology, and volatile reservoirs continues to improve, our knowledge of the formation processes and distribution of gullies may evolve, potentially revealing new insights into the diversity of geomorphic features on Mars.
