Volume 384, Number 1, MarchII 2002
|Page(s)||48 - 55|
|Section||Cosmology (including clusters of galaxies)|
|Published online||15 March 2002|
Magnetic fields and radio polarization of barred galaxies
3D dynamo simulations
Astronomical Observatory, Jagiellonian University, Kraków, Poland
2 Astrophisikalisches Institut Postdam, Germany
Corresponding author: K. Otmianowska-Mazur, firstname.lastname@example.org
Accepted: 5 December 2001
A three-dimensional (3D) MHD model is applied to simulate the evolution of a large-scale magnetic field in a barred galaxy possessing a gaseous halo extending to about 2.8 kpc above the galactic plane. As the model input we use a time-dependent velocity field of molecular gas resulting from self-consistent 3D N-body simulations of a galactic disk. We assume that the gaseous halo rotates differentially co-rotating with the disk or decreasing its velocity in the Z direction. The dynamo process included in the model yields the amplification of the magnetic field as well as the formation of field structures high above the galactic disk. The simulated magnetic fields are used to construct the models of a high-frequency (Faraday rotation-free) polarized radio emission that accounts for effects of projection and limited resolution, and is thus suitable for direct comparison with observations. We found that the resultant magnetic field correctly reproduces the observed structures of polarization B-vectors, forming coherent patterns well aligned with spiral arms and with the bar. The process initializing a wave-like behavior of the magnetic field, which efficiently forms magnetic maxima between the spiral arms, is demonstrated. The inclusion of the galactic halo constitutes a step towards a realistic model of galactic magnetic fields that includes as many dynamical components as needed for a realistic description.
Key words: MHD / turbulence / galaxies: ISM / galaxies: magnetic fields
© ESO, 2002
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