Sign on

SAO/NASA ADS Astronomy Abstract Service


· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· Full Refereed Journal Article (PDF/Postscript)
· arXiv e-print (arXiv:0710.4059)
· References in the article
· Citations to the Article (68) (Citation History)
· Refereed Citations to the Article
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Magnetic Diffusivity Tensor and Dynamo Effects in Rotating and Shearing Turbulence
Authors:
Brandenburg, A.; Rädler, K.-H.; Rheinhardt, M.; Käpylä, P. J.
Affiliation:
AA(NORDITA, Roslagstullsbacken 23, SE-10691 Stockholm, Sweden.), AB(Astrophysical Institute Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany), AC(Astrophysical Institute Potsdam, An der Sternwarte 16, D-14482 Potsdam, Germany), AD(NORDITA, Roslagstullsbacken 23, SE-10691 Stockholm, Sweden; Observatory, University of Helsinki, P.O. Box 14, FI-00014 Helsinki, Finland.)
Publication:
The Astrophysical Journal, Volume 676, Issue 1, pp. 740-751. (ApJ Homepage)
Publication Date:
03/2008
Origin:
UCP
Astronomy Keywords:
Magnetohydrodynamics: MHD, Turbulence
DOI:
10.1086/527373
Bibliographic Code:
2008ApJ...676..740B

Abstract

The turbulent magnetic diffusivity tensor is determined in the presence of rotation or shear. The question is addressed whether dynamo action from the shear-current effect can explain large-scale magnetic field generation found in simulations with shear. For this purpose a set of evolution equations for the response to imposed test fields is solved with turbulent and mean motions calculated from the momentum and continuity equations. The corresponding results for the electromotive force are used to calculate turbulent transport coefficients. The diagonal components of the turbulent magnetic diffusivity tensor are found to be very close together, but their values increase slightly with increasing shear and decrease with increasing rotation rate. In the presence of shear, the sign of the two off-diagonal components of the turbulent magnetic diffusion tensor is the same and opposite to the sign of the shear. This implies that dynamo action from the shear-current effect is impossible, except perhaps for high magnetic Reynolds numbers. However, even though there is no alpha effect on the average, the components of the α tensor display Gaussian fluctuations around zero. These fluctuations are strong enough to drive an incoherent alpha-shear dynamo. The incoherent shear-current effect, on the other hand, is found to be subdominant.
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)

   


Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints