A sufficiently massive planet will induce spiral arms, gap formation, migration and accretion shocks in his surrounding disk. We attempt to understand how all those processes backreact onto planetary formation and disk evolution.

Members working on this project

Aiara Lobo Gomes - Migration due to interaction with spiral arms (PhD project)

Simulations of a Jupiter mass planet interacting with its parent disk. The planet is located at 5 au and the results are after 23 planetary orbits. In the top left side, a locally isothermal model is shown, while in the top right side an adiabatic model, and in the bottom a model where the thermal radiation from the dust was considered. We can see that the midplane gap is carved out faster for the locally isothermal case than for others. Nevertheless, the planet mostly does not affect the disk atmosphere for the locally isothermal case, whereas in the adiabatic and radiation cases, a gap is also visible in the top disk layers.

"Planets are formed in the discs of young stars, they interact with the circumstellar disc and can survive until the latter has evaporated. It is of major importance to understand the interplay between planets and their parental discs to explain the variety of exoplanets observed and to constrain planet formation theories.

The goal of this project is to study several aspects of planet-disc interactions when considering non-isothermal discs. For that purpose we carry out (radiative-)hydrodynamical simulations of planet-disc interactions using the PLUTO code."

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