Formation of different planetary classes in evolving accretion discs

The formation of planets with gaseous envelopes takes place in protoplanetary accretion discs on time-scales of several millions of years. Small dust particles stick to each other to form pebbles, pebbles concentrate in the turbulent flow to form planetesimals and planetary embryos and grow to planets, which undergo substantial radial migration. All these processes are influenced by the underlying structure of the protoplanetary disc, specifically the profiles of temperature, gas scale height and density. Protoplanetary disc models with both viscous and stellar heating show several bumps and dips in temperature, scale height and density caused by transitions in opacity. These play an important role in the formation of planets, as they can act as sweet spots for the formation of planetesimals via the streaming instability and affect the direction and magnitude of type-I-migration. In this talk, I will present our new model for the formation of planets. It combines the formation of planets via pebble and gas accretion with migration of these planets in evolving discs. The resulting planets can be categorised in different classes (e.g. gas and ice giants, small planets) and I will discuss what leads to the formation of these different planetary classes.