Disentangling the Early History of the Solar System

Abstract: Giant planets form out of a disc of gas and dust – called protoplanetary disc -- that surrounded the protosun at the time of its formation. While the cores of giant planets were growing via planetesimal and pebble accretion, they started to interact with the gas in the protoplanetary disc. These interactions can lead to inward migration of all the four giant planets in our Solar System during the protoplanetary disc-phase.In this thesis I investigate the possibility that our Solar System was affected by the early inward migration of the giant planets. In paper I, II and III we computed growth tracks for the giant planets and implemented them into an N-body code. In paper I and II, we explored the consequences of the inward migration of the giant planets on the small body populations of the inner Solar System, such as the Jupiter Trojans, the Hilda asteroids and the asteroid belt. In paper III we focused on the region beyond the orbit of Neptune, i.e. the Kuiper belt. We analysed if the inward migration of the giant planets could have affected that region too.We found traces of the inward migration of Jupiter in the Jupiter Trojan asymmetry ratio. Indeed the feature arises only if Jupiter is migrating and growing at the same time, a condition achieved when Jupiterwas embedded in the protoplanetary disc. We also found an explanation to the high inclinations of the Trojan asteroids. Finally we concluded that the giant planets inward migration also affected the Kuiper belt region, injecting material from the inner disc into the different dynamical populations of the trans-Neptunian region.