Three-dimensional simulations of shear instabilities in magnetized flows

Shear mixing is believed to be the main mechanism to provide extra mixing in stellar interiors. We present results of three-dimensional (3D) simulations of the magnetohydrodynamic Kelvin—Helmholtz instability in a stratified shear layer. The magnetic field is taken to be uniform and parallel to the shear flow. We describe the evolution of the fluid flow and the magnetic field for a range of initial conditions. In particular, we investigate how the mixing rate of the fluid depends on the Richardson number and the magnetic field strength. It is found that the magnetic field can enhance as well as suppress mixing. Moreover, we have performed two-dimensional (2D) simulations and discuss some interesting differences between the 2D and 3D results.