Turbulent Magnetic Dynamos with Halo Lags, Winds, and Jets

TL;DR

This paper develops scale-invariant galactic magnetic dynamo models, compares them with observations, and predicts a correlation between magnetic field morphology and AGN activity, emphasizing the role of winds and outflows.

Contribution

It introduces self-similar dynamo models incorporating halo lags, winds, and jets, highlighting the influence of AGN outflows on galactic magnetic fields.

Findings

Magnetic scale heights increase with radius and wind velocity.

A correlation between magnetic field morphology and AGN presence is predicted.

Neglecting diffusion under certain conditions simplifies the dynamo equations.

Abstract

This paper presents scale invariant/self-similar galactic magnetic dynamo models based on the classic equations, and compares them qualitatively to recently observed magnetic fields in edge-on spiral galaxies. We classify the axially symmetric dynamo magnetic field by its separate sources, advected flux and sub scale turbulence. We neglect the diffusion term under plausible physical conditions. There is a time dependence determined by globally conserved quantities. We show that magnetic scale heights increase with radius and wind velocity. We suggest that AGN outflow is an important element of the large scale galactic dynamo, based on the dynamo action of increasing sub scale vorticity. This leads us to {\it predict} a correlation between the morphology of coherent galactic magnetic field (i.e. extended polarized flux) and the presence of an AGN.