Oral title: The consequences of a large-scale migration of the giant planets on minor bodies of the solar system

Oral abstract: Recently, the pebble accretion mechanism was recognized as a building block in planet formation theories. 
In this frame, giant planets can grow by pebble accretion until their pebble isolation mass and then start to accrete gas, 
migrating rapidly through the disc. The result is a large-scale inward migration of the giant planets, in contrast to classical 
models where Jupiter form and grow in situ, at about 5 au.
Our purpose is to investigate the properties and the evolution of minor bodies populations in our solar system, in 
particular the Jupiter trojan asteroids and the Hilda asteroids, under the effect of a large-scale migration of the giant 
planets and compare the results to the classical in situ growth. 
Our simulations show that inward migration produces asymmetry between the leading and trailing populations of the 
trojans, comparable to the current trojan asymmetry, while the in situ formation of Jupiter generates symmetric 
leading/trailing populations. Moreover, the resulting Trojans and Hildas, in the migration scenario, are composed of bodies 
trapped from the outer solar system and have different orbital parameter distributions from the ones found in the in situ 
formation of Jupiter simulations.