Dynamical origin of the Dwarf Planet Ceres

The Dwarf Planet Ceres revealed the presence of ammonia and other unique properties compared to asteroids in main belt which suggests that it was not formed situ. We model early dynamical evolution outer Solar System study possible mechanisms implant a Ceres-sized planetesimal asteroid from trans-Saturnian region. calculate fraction population planetesimals are captured is range 2.8e-5 1.2e-3 depending on initial location disk. bodies have 70% probability semimajor axis between 2.5 3 au, 33% an eccentricity smaller than 0.2 45% orbital inclination 10 degrees. Assuming existence 3,600 Ceres-size inner part disk, consistent with estimate Nesvorny & Vokrouhlicky (2016) for trans-Neptunian our estimated capture final 80% depletion during subsequent giant planet instability, lead 1 belt, 15%, 34%, 51% be located inner, middle respectively.