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The role of the Yoshizawa effect in the Archontis dynamo
Stockholm University, Faculty of Science, Department of Astronomy.
2009 (English)In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 399, no 1, 273-280 p.Article in journal (Refereed) Published
Abstract [en]

The generation of mean magnetic fields is studied for a simple non-helical flow where a net cross-helicity of either sign can emerge. This flow, which is also known as the Archontis flow, is a generalization of the Arnold-Beltrami-Childress flow, but with the cosine terms omitted. The presence of cross-helicity leads to a mean-field dynamo effect that is known as the Yoshizawa effect. Direct numerical simulations of such flows demonstrate the presence of magnetic fields on scales larger than the scale of the flow. Contrary to earlier expectations, the Yoshizawa effect is found to be proportional to the mean magnetic field and can therefore lead to its exponential instead of just linear amplification for magnetic Reynolds numbers that exceed a certain critical value. Unlike α effect dynamos, it is found that the Yoshizawa effect is not notably constrained by the presence of a conservation law. It is argued that this is due to the presence of a forcing term in the momentum equation, which leads to a non-zero correlation with the magnetic field. Finally, the application to energy convergence in solar wind turbulence is discussed.

Place, publisher, year, edition, pages
2009. Vol. 399, no 1, 273-280 p.
Keyword [en]
magnetic fields, MHD, hydrodynamics, turbulence
Identifiers
URN: urn:nbn:se:su:diva-32537DOI: 10.1111/j.1365-2966.2009.15254.xISI: 000271163200021OAI: oai:DiVA.org:su-32537DiVA: diva2:282396
Available from: 2009-12-20 Created: 2009-12-12 Last updated: 2017-12-12Bibliographically approved

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