The dwarf planet Ceres has unique geomorphology, different from airless silicate objects like the Moon or asteroid Vesta, but also different from the icy outer planet satellites. All four primary planetary geologic processes [impact cratering, tectonism, volcanism, and gradation (weathering, erosion, and deposition of loose material)] are visible on Ceres’ surface.Ceres’ low albedo, heavily cratered surface displays craters <300 km in diameter, in which the lack of larger, multi-ring basins suggests resurfacing event(s) early in the dwarf planet’s history. Ejecta blankets in the youngest craters display bluish ejecta and rays, and lobate deposits in and around craters suggest impact slurries, ice-rich landslides, or cryovolcanic flows. Some landslides have exposed water ice, in less than a dozen locations on the surface. Tectonic features include impact-induced secondary crater chains and non-impact-related pit chains and fractures. Several impact craters have heavily fractured floors akin to those on the Moon. The distinctive mountain Ahuna Mons appears to be a cryovolcanic edifice, composed of a viscous, salt-rich, carbonate-bearing material. Ceres distinctive bright spots, Cerealia and Vinalia Faculae within Occator crater, are composed of salt-rich liquids containing carbonates, and were likely emplaced by some combination of deep brines extrusion and hydrothermal (shallow brines) processes.