Hydrodynamic turbulence in disks with embedded planets

Abstract

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

arXiv comment12 pages, 14 figures, 1 table; accepted in A&A

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Cited by in corpus (3)

• How to form compact & other longer-lived planet-induced vortices: VSI, planet migration, or re-triggers, but not feedback
• Starlight-driven flared-staircase geometry in radiation hydrodynamic models of protoplanetary disks
• How two-dimensional are planet-disc interactions? II. Radiation hydrodynamics and suitable cooling prescriptions