Journal Article

Flux expulsion by inhomogeneous turbulence

L. Tao, M. R. E. Proctor and N. O. Weiss

in Monthly Notices of the Royal Astronomical Society

Published on behalf of The Royal Astronomical Society

Volume 300, issue 3, pages 907-914
Published in print November 1998 | ISSN: 0035-8711
Published online November 1998 | e-ISSN: 1365-2966 | DOI:
Flux expulsion by inhomogeneous turbulence

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Flux expulsion is an important consequence of the interaction of magnetic fields with fluid convection and has been well studied for particular cases of steady, single-cell flows. Here we examine a related phenomenon in inhomogeneous turbulence using direct numerical simulations. To understand our numerical results, we analyse average properties of our model, and obtain mean transport coefficients which can be used to describe the approach of the system to its final state. For the kinematic problem these transport coefficients give an excellent prediction of the expulsion process; however, the enhanced transport is suppressed by dynamical back-reaction of the Lorentz force. Finally, we discuss the astrophysical implications for magnetic fields in stellar convection zones. Segregation of magnetic fields from turbulent motion not only allows strong toroidal fields to accumulate in regions of convective overshoot but also permits significant poloidal fields to be maintained by dynamo action in stars like the Sun.

Keywords: diffusion; MHD; turbulence

Journal Article.  0 words. 

Subjects: Astronomy and Astrophysics

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