The Nonlinear Alpha-Omega Dynamo

Details The Nonlinear Alpha-Omega Dynamo The Nonlinear Alpha-Omega Dynamo

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...208.2105v&link_type=abstract

American Astronomical Society Meeting 208, #21.05; Bulletin of the American Astronomical Society, Vol. 38, p.102

Astronomy and Astrophysics

Astronomy

Scientific paper

We consider the growth of a magnetic field in an idealized galactic disk, driven by a turbulent dynamo. Differential rotation supplies the symmetry-breaking necessary for a vertical magnetic helicity flux. The necessary seed for the dynamo will be supplied by the long wavelength tail of the turbulent magnetic field. The magnetic field will saturate when the Alfven speed is roughly the disk thickness times the global shear. For a typical disk galaxy this is indistinguishable from equipartition between the turbulent and magnetic pressures, although it can be much higher. In any case the magnetic field will reach its final value in less than a few billion years. We conclude that magnetogenesis does not require an exotic seed mechanism in the early universe.

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