Global three-dimensional simulations of outer protoplanetary discs with ambipolar diffusion

The structure and evolution of protoplanetary discs (PPDs) are largely governed by disc angular momentum transport, mediated by magnetic fields. In the most observable outer disc, ambipolar diffusion is the primary non-ideal magnetohydrodynamic (MHD) effect. In this work, we study the gas dynamics in outer PPDs by conducting a series of global three-dimensional non-ideal MHD simulations with ambipolar diffusion and net poloidal magnetic flux, using the Athena++ MHD code, with resolution comparable to local simulations. Our simulations demonstrate the coexistence of magnetized disc winds and turbulence driven by the magneto-rotational instability (MRI). While MHD winds dominate disc angular momentum transport, the MRI turbulence also contributes significantly. We observe that magnetic flux spontaneously concentrates into axisymmetric flux sheets, leading to radial variations in turbulence levels, stresses, and accretion rates. Annular substructures arise as a natural consequence of magnetic flux concentration. The flux concentration phenomena show diverse properties with different levels of disc magnetization and ambipolar diffusion. The disc generally loses magnetic flux over time, though flux sheets could prevent the leak of magnetic flux in some cases. Our results demonstrate the ubiquity of disc annular substructures in wealdy MRI turbulent outer PPDs and imply a stochastic nature of disc evolution.

Automated summary

The study of gas dynamics in outer protoplanetary discs shows the coexistence of magnetized disc winds and turbulence driven by the magneto-rotational instability. Magnetic flux concentrates into axisymmetric flux sheets, leading to radial variations in turbulence levels. The disc generally loses magnetic flux over time, with flux sheets sometimes preventing the leak of magnetic flux.