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Abstract

Protoplanetary disks control the formation and evolution of planets, in reaction the planets also influence the disk structure. Disk gas and dust are the building materials of planets. Tidal forces between planet and disk determine the radial movement of the planet (migration); the planets simultaneously influence the disk, possibly carving out a gap. The interplay between planets and disks is important to understand the variety of exoplanets observed and constrain planet formation theories. This thesis studies new aspects of planet-disk interactions in non-isothermal disks; an important step to a better description of this subject. To this end, radiative-hydrodynamical simulations of planet-disk interactions are performed. Firstly, a Newtonian cooling law is used to investigate the dynamics of vortices, which are generated by the planet and amplified by the convective overstability. The formation of density rings beyond the position of a planetary gap carved out by a high mass planet is studied, as well as the migration rates of low mass planets. Finally, radiative-hydrodynamical simulations are performed. The coupling of radiation transfer to hydrodynamics yields a more accurate determination of the disk temperature in the planet’s vicinity, which has a strong influence on the formation and properties of gaps in disks.