Magnetic dynamo action in astrophysical turbulence

Abstract

We investigate the structure of magnetic field amplified by turbulent velocity fluctuations, in the framework of the kinematic Kazantsev-Kraichnan model. We consider Kolmogorov distribution of velocity fluctuations, and assume that both Reynolds number and magnetic Reynolds number are very large. We present the full numerical solution of the model for the spectra and the growth rates of magnetic fluctuations. We consider astrophysically relevant limits of large and small magnetic Prandtl numbers, and address both helical and nonhelical cases.

13 pages, 3 figures, minor changes are made to match the published version

References in corpus (5)

• On the Origin of Cosmic Magnetic Fields
• Simulations of nonhelical hydromagnetic turbulence
• On magnetic field generation in Kolmogorov turbulence
• Magnetic-field generation in helical turbulence
• Magnetic dynamo action in helical turbulence

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• Gradient measurement of synchrotron polarization diagnostic: Application to spatially separated emission and Faraday rotation regions
• On obliquely magnetized and differentially rotating stars