Galactic dynamics and magnetic fields. I - Superbubbles in galactic central regions

Details Galactic dynamics and magnetic fields. I - Superbubbles in galactic central regions Galactic dynamics and magnetic fields. I - Superbubbles in galactic central regions

Feb 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...268...58l&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 268, no. 1, p. 58-64.

Statistics

Computation

8

Celestial Mechanics, Galactic Halos, Galactic Structure, Interstellar Magnetic Fields, Starburst Galaxies, Computational Astrophysics, Dynamo Theory, Interacting Galaxies

Scientific paper

The evolution of magnetic fields in the halos of galaxies is investigated. It is shown that the field structure in the halo sensitively depends on dynamic processes of the underlying disk. Whereas strong interacting galaxies like M82 and NGC 4631 exhibit huge radio halos with extensions up to 8 kpc containing radial magnetic fields, weakly interacting galaxies show radio halos which are considerably smaller although the X-ray luminosity is comparable. We argue that the prestarburst magnetic field structure determines the extension and shape of the poststarburst radio halo. Due to short tidal interaction time scales in M82/NGC 4631, dynamo action was either completely suppressed or at least heavily disturbed. Thus, no large-scale magnetic field was present before the galactic wind, driven by the central starburst, convects the field into the observed radial halo field configuration. In noninteracting galaxies, the time scale for a starburst and dynamo action are of the same order of magnitude. A starburst in those objects also drives a wind but the plasma flow now sweeps up the field lines of the large-scale field generated by the dynamo. The further propagation of the wind is considerably dammed by the field, so that the radio halo is much smaller than in interacting galaxies.

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