Rafael A. García
CEA, Université Paris-Saclay, Université Paris Cité, France

Abstract
In 2013, McQuillan et al. compared stellar rotation periods (Prot) with orbital exoplanet periods (Porb) showing a dearth of close-in planets. In this talk, I revisit the Prot extraction of Kepler planet-host stars and study the Prot vs. Porb diagram classifying the stars by their spectral type. The results are then confronted to the synthetic population obtained from the star-planet secular evolution code ESPEM, which takes into account the tidal and magnetic interactions as well as the influence of stellar winds. Comparing the outcome of ESPEM’s Prot with either the full set of confirmed planets or the ones in which a Prot has been measured, there are no biases between them, meaning that this last dataset is a good statistical representation of the population of Kepler exoplanets systems detected to date. The detailed analysis of the observations uncovers that the dearth in close-in planets orbiting around fast rotating stars depends on the stellar spectral in both observations and simulations. The dearth is filled for K stars while it is present in G and F type stars. I will discuss the ingredients of the model and show that the realistic formation hypothesis included in the model and the proper treatment of tidal and magnetic migration are enough to quantitatively explain the dearth of hot planets around fast rotating stars. These physical properties are the basic ingredients to shape the architecture of the observed Kepler single-planet systems.

2023 March 22, 13:30

IA/U.Porto
Centro de Astrofísica da Universidade do Porto (Auditorium)
Rua das Estrelas, 4150-762 Porto