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Abstract

Motivated by the tachocline region within the Sun, we investigate the interaction of buoyant structures with convection in a numerical set-up that resembles the base of the solar convection zone, where the fully compressible, non-linear magnetohydrodynamics equations are solved. Fully-developed convective flows are prescribed, with particular attention paid to identifying the features established in the earlier studies of [1] and [2] where parameterisation of the small-scale turbulent pumping is imposed using mean-field approximation. Analysis of several magnetoconvection regimes in quasi-two-dimensions reveals that the equipartition criterion between kinetic and magnetic energy does contribute globally to the flux emergence process as fluctuating motions in turbulent flows become more energetic. However, results were found to be less pronounced in the three-dimensional simulations due to the effectively reduced fluctuations.

Publication Type:	Article
Additional Information:	©2022 Ali and Silvers; This is an Open Access article distributed under the terms of the Creative Commons Attribution License(http://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium,provided the original work is properly cited.
Publisher Keywords:	Convection; instabilities; MHD; Sun: interior; Sun: magnetic fields
Subjects:	Q Science > QB Astronomy Q Science > QC Physics
Departments:	School of Science & Technology > Mathematics

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