Volume 402, Number 3, May II 2003
First Science with the ODIN satellite
|Page(s)||879 - 889|
|Published online||23 April 2003|
Magnetic field evolution in galaxies interacting with the intracluster medium
3D numerical simulations
Astronomical Observatory Jagiellonian University Kraków, Poland
2 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
Corresponding author: K. Otmianowska-Mazur, firstname.lastname@example.org
Accepted: 27 January 2003
A fully three-dimensional (3D) magnetohydrodynamical (MHD) model is applied to simulate the evolution of the large-scale magnetic field in cluster galaxies interacting with the intra-cluster medium (ICM). As the model input we use time-dependent gas velocity fields resulting from 3D N-body sticky-particle simulations of a galaxy. The modeled clouds are affected by the ram pressure due to their rapid motion through the ICM in the central part of a cluster. Numerical simulations have shown that after the initial compression phase due to ram pressure, a process of gas re-accretion onto the galactic disk takes place. We find that the gas re-accretion leads to an increase of the total magnetic energy without any dynamo action. The simulated magnetic fields are used to construct the model maps of high-frequency (Faraday rotation-free) polarized radio emission. We show that the evolution of the polarized intensity shows features that are characteristic of different evolutionary stages of an ICM–ISM interaction. The comparison of polarized radio continuum emission maps with our model permits us to determine whether the galaxy is in the compression or in the re-accretion phase. It also provides an important constraint upon the dynamical modeling of ICM–ISM interactions.
Key words: galaxies: evolution / galaxies: ISM / galaxies: magnetic fields / galaxies: clusters: general / galaxies: intergalactic medium / methods: numerical
© ESO, 2003
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