Planetesimal Dynamics in the Presence of a Giant Planet

Standard models of planet formation explain how planets form in axisymmetric, unperturbed disks single star systems. However, it is possible that giant could have already formed when other planetary embryos start to grow. We investigate the dynamics planetesimals under perturbation a gaseous disk. Our aim understand effect planet's on cores outside orbit planet. calculate orbital evolution ranging from 1013 1020 g, with Jupiter-mass located at 5.2 au. find alignment distributed ?9–15 au, except for mean motion resonance (MMR) locations. The degree increases increasing distance and decreasing planetesimal mass. Aligned orbits lead low encounter velocity thus faster growth. typical dispersion identical-mass MMR relative decreases mass ratio planetesimals. When eccentricity vectors reach equilibrium gas drag secular perturbation, becomes lower masses two are both larger end spectrum. results show embedded disk, growth another core might be accelerated certain