Simitev, R. D. and Busse, F. H. (2018) Flows and dynamos in a model of stellar radiative zones. Journal of Plasma Physics, 84(3), 735840308. (doi: 10.1017/S0022377818000612)
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Abstract
Stellar radiative zones are typically assumed to be motionless in standard models of stellar structure but there is sound theoretical and observational evidence that this cannot be the case. We investigate by direct numerical simulations a three-dimensional and time-dependent model of stellar radiation zones consisting of an electrically-conductive and stably-stratified anelastic fluid confined to a rotating spherical shell and driven by a baroclinic torque. As the baroclinic driving is gradually increased a sequence of transitions from an axisymmetric and equatorially-symmetric time-independent flow to flows with a strong poloidal component and lesser symmetry are found. It is shown that all flow regimes characterised with significant non-axisymmetric components are capable of generating self-sustained magnetic field. As the value of the Prandtl number is decreased and the value of the Ekman number is decreased flows become strongly time-dependent with progressively complex spatial structure and dynamos can be generated at lower values of the magnetic Prandtl number.
Item Type: | Articles |
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Status: | Published |
Refereed: | Yes |
Glasgow Author(s) Enlighten ID: | Simitev, Professor Radostin |
Authors: | Simitev, R. D., and Busse, F. H. |
College/School: | College of Science and Engineering > School of Mathematics and Statistics > Mathematics |
Journal Name: | Journal of Plasma Physics |
Publisher: | Cambridge University Press |
ISSN: | 0022-3778 |
ISSN (Online): | 1469-7807 |
Published Online: | 25 June 2018 |
Copyright Holders: | Copyright © 2018 Cambridge University Press |
First Published: | First published in Journal of Plasma Physics 84(3):735840308 |
Publisher Policy: | Reproduced in accordance with the copyright policy of the publisher |
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