Jet confinement by magneto-torsional oscillations

TL;DR

This paper investigates how magneto-torsional oscillations can stabilize astrophysical jets, providing a simplified model and numerical solutions to estimate the conditions for jet confinement.

Contribution

It introduces a new model linking torsional oscillations to jet stabilization, offering quantitative estimates of parameter ranges for confinement.

Findings

Torsional oscillations can create stabilizing azimuthal magnetic fields.

Numerical solutions identify parameter ranges for jet stability.

The model explains jet structure with magnetic confinement without charge separation.

Abstract

Many quasars and active galactic nuclei (AGN) appear in radio, optical, and X-ray maps, as a bright nuclear sources from which emerge single or double long, thin jets. When observed with high angular resolution these jets show structure with bright knots separated by relatively dark regions. Nonthermal nature of a jet radiation is well explained as the synchrotron radiation of the relativistic electrons in an ordered magnetic field. We consider magnetic collimation, connected with torsional oscillations of a cylinder with elongated magnetic field, and periodically distributed initial rotation around the cylinder axis. The stabilizing azimuthal magnetic field is created here by torsional oscillations, where charge separation is not necessary. Approximate simplified model is developed. Ordinary differential equation is derived, and solved numerically, what gives a possibility to estimate quantitatively the range of parameters where jets may be stabilized by torsional oscillations.