Global three-dimensional simulations of magnetic field evolution in a galactic disk

TL;DR

This paper uses 3D simulations combining galactic dynamics and MHD to study how gas flows influence the structure and intensity of magnetic fields in galactic disks, revealing sensitivity to dynamical changes.

Contribution

It introduces a numerical approach integrating N-body galactic dynamics with MHD simulations to analyze magnetic field evolution in response to gas flow variations.

Findings

Magnetic fields are highly sensitive to gas velocity changes.

Magnetic arms form due to nonuniform intensity structures.

Magnetic lines align with spiral arms and bars.

Abstract

The evolution of three-dimensional, large-scale, magnetic fields, in a galactic disk is investigated numerically. The N-body simulations of galactic dynamics are incorporated into the kinematic calculations of induction equations to study the influence of non-axisymmetric gas flows on the galactic magnetic field. The time-dependent gas velocity fields are introduced as input parameters for the MHD-simulations. Our principal concern is to check how dynamical evolution of the galactic gas affects the global magnetic field structure and intensity. We have found that the magnetic field responds sensitively to changes in the gas velocity field, and even slight variations of the dynamical parameters, such as the gas mass/total mass ratio results in nonuniform intensity structures, i.e. magnetic arms. The magnetic lines of force are well aligned with spiral arms and bar due to compressional flows in these features. In the inter-arm regions the areas with magnetic vectors going opposite to the main magnetic spirals are present.