The dynamo origin of magnetic fields in galaxy clusters

Details The dynamo origin of magnetic fields in galaxy clusters The dynamo origin of magnetic fields in galaxy clusters

Nov 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989mnras.241....1r&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 241, Nov. 1, 1989, p. 1-14.

Statistics

Computation

90

Computational Astrophysics, Dynamo Theory, Galactic Clusters, Intergalactic Media, Interstellar Magnetic Fields, Radio Sources (Astronomy), Chaos, Cygnus Constellation, Magnetohydrodynamic Turbulence, Probability Distribution Functions, Reynolds Number

Scientific paper

The generation of magnetic fields by turbulent motions of intracluster gas in rich galaxy clusters is considered. A qualitative discussion of the properties of intracluster MHD turbulence, its spectrum, characteristic scales and velocities, and estimation of hydrodynamic and magnetic Reynolds numbers is presented. Turbulence arises in the wakes of galaxies which move transonically through the gas. Magnetic field is generated at scales below the energy-range scale of turbulence. The magnetic fields are concentrated within thin intense ropes which occupy a small fraction of the total volume. The field strength within the ropes is about 10 microG, as determined by equipartition with kinetic energy of turbulence, while the rms field strength within a turbulent cell is as low as 2 microG. The correlation function of the chaotic magnetic field has a number of characteristic scales ranging from 20 kpc (the turbulence correlation scale) to 0.002 kpc (the skin-layer thickness). The results are in agreement with observations of magnetic fields in the radiohaloes of galaxy clusters, in particular with recent observations of Cygnus A.

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