The formation history of giant planets seen through multiple elemental ratios

Comparative studies of protoplanetary disks, exoplanetary systems, and the Solar System reveal the presence of giant planets over a wide range of orbital radii, spanning from 0.01 to 100 au from the host star. This great diversity of architectures suggests that giant planets can interact with multiple and diverse chemical environments in protoplanetary disks while they form and migrate to their final orbits, accreting gas and solids with different compositions and relative abundances of refractory and volatile elements. The interplay between accretion and migration shapes the composition of giant planets and of their atmospheres: as such, the composition of planetary atmospheres can be used as a proxy into the formation and migration histories of giant planets. We explore the implications of the wider formation regions suggested by observations coupling N-body simulations of forming and migrating giant planets with astrochemical models of protoplanetary discs. In our analysis we expand the set of elemental ratios we trace by including one of the most volatile elements, N, and one of the most refractory ones, S, to complement the information provided by C and O. In this talk we discuss the implications of different disk astrochemical scenarios for the final composition of giant planets, and show how this enhanced set of elemental ratios can be used to constrain both the extent of migration and the sources of the planetary metallicity in both chemical inheritance and reset scenarios of the host protoplanetary disk....