From Small-Scale Dynamo to Isotropic MHD Turbulence

Details From Small-Scale Dynamo to Isotropic MHD Turbulence From Small-Scale Dynamo to Isotropic MHD Turbulence

2003-06-14

arxiv.org/abs/astro-ph/0306296v2

Astrophys.SpaceSci.292:141-146,2004

Astronomy and Astrophysics

Astrophysics

kluwer latex, 7 pages, 7 figures; Proceedings of the International Workshop "Magnetic Fields and Star Formation: Theory vs. Ob

Scientific paper

10.1023/B:ASTR.0000045010.69658.

We consider the problem of incompressible, forced, nonhelical, homogeneous, isotropic MHD turbulence with no mean magnetic field. This problem is essentially different from the case with externally imposed uniform mean field. There is no scale-by-scale equipartition between magnetic and kinetic energies as would be the case for the Alfven-wave turbulence. The isotropic MHD turbulence is the end state of the turbulent dynamo which generates folded fields with small-scale direction reversals. We propose that the statistics seen in numerical simulations of isotropic MHD turbulence could be explained as a superposition of these folded fields and Alfven-like waves that propagate along the folds.

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