Investigating Ring-Like Structures in Vertical Shear Instability of Protoplanetary Disks
C. Hegde, R. Burn, H. Klahr
Max-Planck-Institut für Astronomie, Heidelberg
The radial transport of angular momentum is a cornerstone of the accretion process in protoplanetary disks. Turbulence, resulting from diverse physical processes, is a fundamental driver of angular momentum transport, making a critical contribution to the accretion process. In protoplanetary disks, vertical shear can emerge, leading to hydrodynamic instabilities that generate turbulence. This study delves into the fascinating realm of vertical shear instability (VSI) within protoplanetary disks, employing one-dimensional simulations utilizing the Bern model of planetary formation and evolution known as Planete. Our investigation centers on the α-description for turbulence, utilizing the VSI model where VSI-induced turbulence is parameterized using the alpha prescription. We systematically explore the impact of various physical parameters, such as radial drift, dust grain size, and fragmentation velocity, on VSI-α. However, our primary focus lies on the intriguing ring-like structures that appear in our model due to the inclusion of the VSI-α. We conduct a comprehensive analysis of the formation and evolution of these rings in VSI-α and their dependence on critical disk properties, including dust surface density, the cooling timescale, and opacities.