Three Dimensional Structure of Relativistic Jet Formation

TL;DR

This study uses high-resolution 3D simulations to explore how relativistic jets form and develop non-axisymmetric instabilities, revealing stabilization mechanisms influenced by external medium perturbations.

Contribution

It provides new insights into the 3D structure and stability of relativistic jets, focusing on non-axisymmetric mode development and control in simulation models.

Findings

Non-axisymmetric modes saturate at ~20 inner disk radii.

External perturbations can stabilize jet formation.

Artificial noise amplification can be mitigated in simulations.

Abstract

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 to m=5 modes are analyzed and found to saturate at a height of \sim 20 inner disk radii. We also discuss a means to control artificial amplification of m = 4 noise in the cartesian simulation geometry. Strong perturbations due to an in-homogeneous ambient medium lead to flow configurations with increased magnetic pitch and thus indicate a self-stabilization of the jet formation mechanism.