Title:
Combining numerical simulations and observations to study MHD disk winds and disk substructures
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 is 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.
Time: May 28th (Tuesday), 12- 1 p.m. at Sterling Hall 4530, or by Zoom https://uwmadison.zoom.us/j/94458178418?pwd=Ym1sZWQ2SEJIMWk0ZmI1c1VIQ1E4dz09