Abstract: Recent observations suggest that protoplanetary disks are not as turbulent as previously predicted by theoretical models. To explain angular momentum transfer and accretion processes in non-viscous disks, astronomers have turned their attention to the MHD disk wind mechanism. In this talk, I will introduce our 2D multi-fluid hydrodynamic simulations with a simplified prescription of MHD disk winds, that study the formation of substructures in disks when angular momentum transfer dominated by MHD disk winds, as opposed to traditional viscosity-dominated disks. By identifying different observational signatures of these substructures, we may be able to directly determine the presence of MHD disk winds in disks through ALMA imaging. Additionally, I will discuss how this method has been applied in my latest research to explain the asymmetric structures and high accretion rates observed in the well-known DM Tau system. Lastly, I will present my recently work on how MHD disk winds or turbulent affect planet migration, this could be insightful for studying stellar-mass black holes merger in AGN disks and their associated processes.
Bio: 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.
