Orbital evolution of eccentric planets in radiative discs

摘要: With an average eccentricity of about 0.29, the distribution extrasolar planets is markedly different from solar system. Among other scenarios considered, it has been proposed that may grow through planet-disc interaction. Recently, noticed thermodynamical state disc can significantly influence migration properties growing protoplanets. However, evolution planetary in radiative discs not considered yet. In this paper we study on eccentric orbits are embedded a three-dimensional viscous and analyse disc's effect orbital planet. We use hydrodynamical code NIRVANA includes full tensor viscosity implicit radiation transport flux-limited diffusion approximation. The uses FARGO-algorithm to speed up simulations. First measure torque power exerted planet by for fixed orbits, then let start with initial evolve disc. For locally isothermal confirm previous results find damping inward cores. case discs, experience as long its lies above certain threshold. After cores masses below 33 Earthmasses begin migrate outward while higher mass always inward. all studied (up 200 Earthmasses) damping. damped during independent mass. Hence, interaction does seem be viable mechanism explain observed high exoplanets.