Speaker
Description
Protoplanetary discs are the birthplace of planets and the site in which they accrete and evolve. It is then fundamental to characterize their evolution to fully understand the emerging exoplanetary population. Substructures in protoplanetary discs – such as rings, gaps, spirals – are routinely detected within discs using all the available tracers and represent key tracers of ongoing interactions in the disc’s material. These features show a strong wavelength dependent morphology, reflecting the different coupling levels between the different dust grain sizes and the gas dynamics. Among many explanations, embedded protoplanets interacting with the parental material is a compelling one. My work combines high-resolution 3D hydrodynamic, radiative transfer and telescope pipelines coupling to explore planet-induced structures, identifying observables to infer and confirm or reject the presence of massive protoplanets in discs. I will describe results from the modelling of single, bright sources (e.g., HD169142, PDS70), and will underline the information we can obtain by comparing multi-wavelengths observations with results from the hydrodynamical models. In particular, I will focus on how simulations can support observational campaigns with several instruments (VLT, ALMA) and I will present the results developed within the JEDIEX collaboration to generate synthetic MICADO/MORFEO observations of substructures in protoplanetary discs. These models will be key to identifying targets where hidden substructures could be revealed and to exploring less-studied objects.
