From Small-Scale Dynamo to Isotropic MHD Turbulence

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dc.creatorSchekochihin, A. A.
dc.creatorCowley, S. C.
dc.creatorTaylor, S. F.
dc.creatorMaron, J. L.
dc.creatorMcWilliams, J. C.
dc.date2003-06-14
dc.date2004-12-01
dc.date.accessioned2026-07-07T10:47:38Z
dc.date.available2026-07-07T10:47:38Z
dc.descriptionWe 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.
dc.descriptionkluwer latex, 7 pages, 7 figures; Proceedings of the International Workshop "Magnetic Fields and Star Formation: Theory vs. Observations", Madrid, 21-25 April 2003 -- published version (but the e-print is free of numerous typos introduced by the publisher)
dc.identifierhttps://arxiv.org/abs/astro-ph/0306296
dc.identifierhttp://arxiv.org/abs/astro-ph/0306296
dc.identifierAstrophys.SpaceSci.292:141-146,2004
dc.identifierdoi:10.1023/B:ASTR.0000045010.69658.a8
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/183603
dc.subjectAstrophysics
dc.titleFrom Small-Scale Dynamo to Isotropic MHD Turbulence
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