Three-dimensional structure of relativistic jet formation

Using high-resolution adaptive mesh refinement simulations in 3D, we investigate the formation of relativistic jets from rotating magnetospheres. Here, we focus on the development of non-axisymmetric modes due to internal and external perturbations to the jet. These originate either from injection of perturbations with the flow or from a clumpy external medium. In the helical field geometry of the accelerating jet, the m = 1-5 modes are analysed and found to saturate at a height of ∼20 inner disc radii. We also discuss a means to control artificial amplification of m = 4 noise in the Cartesian simulation geometry. Strong perturbations due to an inhomogeneous ambient medium lead to flow configurations with increased magnetic pitch and thus indicate a self-stabilization of the jet formation mechanism.