# The supernova-regulated ISM -- VI. Magnetic effects on the structure of the interstellar medium

## TL;DR

This study investigates how magnetic fields influence the vertical structure and phase distribution of the supernova-driven interstellar medium, revealing that magnetic amplification leads to cooler, more homogeneous gas and alters outflow dynamics.

## Contribution

It demonstrates the impact of magnetic fields on ISM structure and dynamics using simulations with dynamo action, highlighting magnetic quenching effects and vertical magnetic field distribution.

## Key findings

- Magnetic fields cause gas to become cooler and more homogeneous.
- Magnetic quenching reduces vertical velocity and cooling length.
- Vertical magnetic field distribution influences outflow and pressure gradients.

## Abstract

We explore the effect of magnetic fields on the vertical distribution and multiphase structure of the supernova-driven interstellar medium (ISM) in simulations that admit dynamo action. As the magnetic field is amplified to become dynamically significant, gas becomes cooler and its distribution in the disc becomes more homogeneous. We attribute this to magnetic quenching of vertical velocity, which leads to a decrease in the cooling length of hot gas. A non-monotonic vertical distribution of the large-scale magnetic field strength, with the maximum at |z| $\approx$ 300 pc causes a downward pressure gradient below the maximum which acts against outflow driven by SN explosions, while it provides pressure support above the maximum.