Table of Contents
Galaxies, Volume 7, Issue 2 (June 2019)
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Cover Story (view full-size image) Radio continuum and polarization observations are best for revealing the magnetic field structure [...] Read more. Radio continuum and polarization observations are best for revealing the magnetic field structure and strength of nearby spiral galaxies. They show a similar magnetic pattern, which is of spiral shape along the disk plane and X-shaped in the halo, sometimes accompanied by strong vertical fields above and below the central region of the disk. The disk magnetic field can, in principle, be explained by a combination of turbulent- and α˗Ω dynamo action. The total halo magnetic field has a comparable strength as the disk field, and has recently been discovered to also contain large-scale components, like giant magnetic ropes, by RM-synthesis. From the analysis of radio scale heights, we conclude that galactic winds exist in several spiral galaxies. These galactic winds may be essential for an effective dynamo action and may transport large-scale magnetic fields and magnetic helicity from the disk into the halo. View this paper