Gas giant planet interactions with protoplanetary discs

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Planets form out of protoplanetary discs. While young and massive, these discs are expected to fragment on gas clumps of a few Jupiter masses. The clumps may eventually evolve into gas giants, smaller planets or massive brown dwarfs. Which one of these outcomes is realised depends on the disc-planet interactions. In these interactions, the planet and the disc may exchange mass in both gas and grains, energy via radiation andangular momentum via gravitational torques. These key processes have not yet been studied in detail and are the subject of this project. We shall begin the study by looking at pebble accretion onto precollapse gas clumps via both 3D discplanet numerical simulations and simplified 2D models. Next, zoom-in simulations onto the internal evolution of clumps will be employed to understand the outcome of pebble accretion in the planetary regime.