Galactic dynamo simulations

Abstract

Recent simulations of supernova-driven turbulence within the ISM support the existence of a large-scale dynamo. With a growth time of about two hundred million years, the dynamo is quite fast -- in contradiction to many assertions in the literature. We here present details on the scaling of the dynamo effect within the simulations and discuss global mean-field models based on the adopted turbulence coefficients. The results are compared to global simulations of the magneto-rotational instability.

10 pages, 5 figures, IAU Symp. 259 proceedings (in press)

References in corpus (6)

• Differential Rotation and Turbulence in Extended HI Disks
• Amplification of Galactic Magnetic Fields by the Cosmic-Ray Driven Dynamo
• Galactic dynamos supported by magnetic helicity fluxes
• Models of Vertically Stratified Two-Phase ISM Disks with MRI-Driven Turbulence
• Discovery of a strong spiral magnetic field crossing the inner pseudoring of NGC 4736
• Global Three-Dimensional MHD Simulations of Galactic Gaseous Disks: I. Amplification of Mean Magnetic Fields in Axisymmetric Gravitational Potential

Cited by in corpus (5)

• Magnetic fields in Local Group dwarf irregulars
• Magnetised winds in dwarf galaxies
• Toward a hybrid dynamo model for the Milky Way
• Do magnetic fields influence gas rotation in galaxies?
• Supernova-driven interstellar turbulence and the galactic dynamo