Speaker
Description
Planet population synthesis models can only partially reproduce the observed population of planets in full. Such models implement different prescriptions for planet formation and disc evolution. We explore the impact of different disc models on the planet population they produce. We adopt two families of discs: the viscosity-driven and the MHD winds-driven model, in turn divided into steady and non-steady evolutionary models. Planets grow through pebble plus gas accretion, and migrate due to planet-disc interactions. We aim to constrain different formation environments from the planet populations they form. The evolution of the dust-to-gas ratio of the disc strongly impacts the variety of the population of planets and creates preferred regions for planet formation. In particular, the latter give rise to two populations of giants, with similar core masses, but different formation histories and potentially different composition. The efficiency of MHD winds changes the relative occurrence of these two populations. Regardless of the disc family, MHD winds extend the mass spectrum of gas giants produced by non-steady models, and reduce the migration distance of planets in both steady and non-steady models. Based on the above results, we identified diagnostics for the planet-forming environment based on the distribution of final orbits and masses of the planets. Our results suggest that one single disc model can hardly reproduce the entire observed population of planets. Rather, multiple models should be taken into account.