Dynamo Supported Magnetic Fields in Clusters of Galaxies

Both observations and theoretical arguments suggest that the hot gas in clusters of galaxies is turbulent, with turbulent velocities $\gtw 100$ km/s. This turbulence will act as a dynamo, maintaining magnetic fields at levels whose energy density is comparable to that in the turbuence. If the turbulence is helical, the magnetic fields will be ordered on scales larger than the turbulent scale size. This paper describes the large-scale magnetic fields which can be maintained by helical turbulence in a cluster. Simulations of the strength and spatial distribution of the rotation measure from such a field are presented, and other likely observational consequences are discussed.

¹NMT

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