| We propose a three-dimensional radiation hydrodynamics investigation of the interaction between young planets and the disk in which they were born. These disks contain not only gas, but also dust particles and we will model this mix with a multifluid astrophysical hydronamics code developed by ourselves. Three-dimensional models of dusty disks containing planets will give us better values for the orbit changes of the planet due to the disk, the accretion rates onto the forming planet, as well as the observational appaerance of the disks themselves. This will improve our understanding of the formation of planets and the early days of our own solar system. The study will consist of two parts. In the first part we will use a simplified model for the temperature structure of the disk, in the second part we will develop a more sophisticated model in which the temperature is calculated from the hydrodynamics and the influence of the radiation from the central star. |
