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Thanks to ALMA, the recent advances in observational astronomy have enabled the detection of more than 200 annular structures in protoplanetary disks, many of which suggest the presence of planets. However, these observations need to be translated into quantitative measures of the system, which can be achieved through hydrodynamics simulations with planets embedded in disks. In this talk, a series of 2D multi-fluid hydrodynamics simulations using the FARGO3D code will be presented, with a focus on two works that use numerical simulations to better understand observation results and constrain the parameters of protoplanetary disk systems. The first part of the talk will propose a novel method that combines planet migration and dust drift to limit the disk mass (Wu, Baruteau & Nayakshin, 2023). This method is based on simulations and some parameters get from the famous system - HD 163296. In the second part of the talk, a novel approach to identifying traditional turbulence viscosity and MHD disk wind contributions to angular momentum transport will be presented (Wu, Chen & Jiang et al. 2023). This approach is based on studying the gap and ring morphology of planet-forming disks in the ALMA continuum. The results presented in this talk will contribute to a better understanding of protoplanetary disk systems and planetary formation, maybe also with implications for how our solar system form.
Yinhao Wu's primary research interest lies in the field of theoretical and computational astrophysics, with a focus on studying dusty protoplanetary disks and planet-disk interaction. He completed his undergraduate degree in Physics from Northwest University in 2019 and is currently pursuing his PhD as a candidate at the School of Physics and Astronomy, University of Leicester, since 2021.