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

Research output: Contribution to journalArticleScientificpeer-review

Researchers

Research units

  • Newcastle University

Abstract

We explore the effect of magnetic fields on the vertical distribution and multiphase structure of the supernova-driven interstellar medium 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| approximate to 300pc causes a downward pressure gradient below the maximum which acts against outflow driven by SN explosions, while it provides pressure support above the maximum.

Details

Original languageEnglish
Pages (from-to)5065-5074
Number of pages10
JournalMonthly Notices of the Royal Astronomical Society
Volume488
Issue number4
Publication statusPublished - Oct 2019
MoE publication typeA1 Journal article-refereed

    Research areas

  • MHD, turbulence, ISM: evolution, galaxies: kinematics and dynamics, galaxies: magnetic fields, COSMIC-RAY, HYDROSTATIC EQUILIBRIUM, TURBULENT MODEL, 3-DIMENSIONAL EVOLUTION, DYNAMICAL EVOLUTION, DIRECT SIMULATIONS, GALACTIC WINDS, STAR-FORMATION, GLOBAL-MODELS, DRIVEN

ID: 34380470