Galaxies in box: A simulated view of the interstellar medium

Abstract

We review progress in the development of physically realistic three dimensional simulated models of the galaxy.We consider the scales from star forming molecular clouds to the full spiral disc. Models are computed using hydrodynamic (HD) or magnetohydrodynamic (MHD) equations and may include cosmic ray or tracer particles. The range of dynamical scales between the full galaxy structure and the turbulent scales of supernova (SN) explosions and even cloud collapse to form stars, make it impossible with current computing tools and resources to resolve all of these in one model. We therefore consider a hierarchy of models and how they can be related to enhance our understanding of the complete galaxy.

Chapter in Large Scale Magnetic Fields in the Universe

References in corpus (10)

• Dependence of Interstellar Turbulent Pressure on Supernova Rate
• Direct simulations of a supernova-driven galactic dynamo
• Towards simulating star formation in the interstellar medium
• Global galactic dynamo driven by cosmic-rays and exploding magnetized stars
• The Distribution of Pressures in a Supernova-Driven Interstellar Medium. I. Magnetized Medium
• The Generation and Dissipation of Interstellar Turbulence - Results from Large Scale High Resolution Simulations
• Generation of Magnetic Fields in the Multi-phase ISM with Supernova-Driven Turbulence
• Models of Vertically Stratified Two-Phase ISM Disks with MRI-Driven Turbulence
• Superbubbles in magnetized interstellar media --- Blowout or confinement ? ---
• The Effect of Cosmic Ray Diffusion on the Parker Instability