Hydrodynamic turbulence in disks with embedded planets

The vertical shear instability (VSI) is a source of hydrodynamic turbulence that can drive vigorous mixing and moderate levels accretion in protoplanetary disks, it could be observable the near future. With high-resolution three-dimensional numerical hydrodynamics simulations, we modeled behavior VSI disks with without embedded planets. We then measured its capabilities by comparing full Reynolds stress, which includes contribution nonaxisymmetric features, such as spiral arms vortices, to stress due azimuthally averaged velocity field, attributed good approximation VSI. verified contribute showed that, depending on disk conditions, an planet coexist or suppress turbulent stress. Specifically, presence shocks launched planet-generated vortices interfere planet's vicinity, recovering at large enough distances from vortex. Our results suggest observations signatures are unlikely contain massive, features.