Like most of the Tharsis region, Pavonis Mons has a high albedo (reflectivity) and low thermal inertia, indicating that the volcano and surrounding areas are covered with large amounts of fine dust (see Martian surface). The dust forms a mantle over the surface that obscures or mutes much of the fine-scale topography and geology of the region. Tharsis is probably dusty because of its high elevations. The summit experiences an atmospheric pressure of around 130 Pa (1.3 mbar), about 21% of Mars' mean surface pressure. The atmospheric density is too low to mobilize and remove dust once it is deposited.