Magnetohydrodynamic simulations of the tayler instability in rotating stellar interiors

The Tayler instability is an important but poorly studied magnetohydrodynamic that likely operates in stellar interiors. nonlinear saturation of the understood and has crucial consequences for dynamo action angular momentum transport radiative regions stars. We perform three-dimensional MHD simulations a cylindrical geometry, including strong buoyancy Coriolis forces as appropriate its operation realistic rotating linear growth characterized by predominantly $m=1$ oscillation with rates roughly following analytical expectations. non-linear appears to be caused secondary shear instabilities also accompanied morphological change flow. argue, however, occurs via other mechanisms real stars where separation scales larger than those reached our simulations. observe amplification axisymmetric poloidal magnetic field, suggesting could field generation evolving