Longcope, D.W., McLeish, T.C.B. and Fisher, G.H. (2003) A viscoelastic theory of turbulent fluid permeated with fibril magnetic fields. Astrophysical Journals, 599 (1 ). pp. 661-674. ISSN 1538-4365
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The solar convection zone is a turbulent plasma interacting with a magnetic field. Its magnetic field is often described as fibrillar since it consists of slender flux tubes occupying a small fraction of the total volume. It is well known that plasma flow will exert a force on these magnetic fibrils, but few models have accounted for the back-reaction of the fibrils on the flow. We present a model in which the back-reaction of the fibrils on the flow is manifest as viscoelastic properties. On short timescales the fibrils react elastically with a shear modulus proportional to their overall magnetic energy density. On longer timescales they produce an effective viscosity resulting from collective aerodynamic drag. The viscosity due to flux tubes in the solar convection zone can be comparable to that attributed to turbulence there. These forces might have observable effects on the convection zone flows.
|Copyright, Publisher and Additional Information:||© 2003 The American Astronomical Society. Reproduced in accordance with the publisher's self-archiving policy.|
|Keywords:||convection, magnetic fields, MHD, Sun, interior, magnetic fields turbulence|
|Institution:||The University of Leeds|
|Academic Units:||The University of Leeds > Faculty of Maths and Physical Sciences (Leeds) > School of Physics and Astronomy (Leeds)|
|Depositing User:||Repository Officer|
|Date Deposited:||16 Aug 2006|
|Last Modified:||05 Jun 2014 02:07|
|Publisher:||University of Chicago Press|