The origin of hot Jupiters

Since the first detection of a hot Jupiter around a main sequence star more than 30 years ago, the question of where these planets originally formed is still not fully answered. Theoretical models predict different formation pathways that include the formation in the outer disc regions with subsequent smooth inward migration during the protoplanetary gas disc phase or scattering after the gas disc dissipated. Recent advanced in atmospheric characterization have allowed us to constrain the composition of the atmospheres of these hot Jupiters, thought to hold a key into unlocking their origin. As the planet-forming discs show a radial decrease in temperature, planets forming at different positions can accrete materials of different composition, allowing us to match the planetary composition to their origin. However, as simple as this approach sounds, it faces several shortcomings related to the large parameter space of planet formation simulations. In this talk, I will discuss the recent ideas of how giant planets can form and how these models could be used to unlock the origin of these giant planets.