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The need for active region disconnection in 3D kinematic dynamo simulations

Whitbread, T; Yeates, A.R.; Munoz-Jaramillo, A.

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Authors

T Whitbread

A. Munoz-Jaramillo



Abstract

In this paper we address a discrepancy between the surface flux evolution in a 3D kinematic dynamo model and a 2D surface flux transport model that has been closely calibrated to the real Sun. We demonstrate that the difference is due to the connectivity of active regions to the toroidal field at the base of the convection zone, which is not accounted for in the surface-only model. Initially, we consider the decay of a single active region, firstly in a simplified Cartesian 2D model and subsequently the full 3D model. By varying the turbulent diffusivity profile in the convection zone, we find that increasing the diffusivity – so that active regions are more rapidly disconnected from the base of the convection zone – improves the evolution of the surface field. However, if we simulate a full solar cycle, we find that the dynamo is unable to sustain itself under such an enhanced diffusivity. This suggests that in order to accurately model the solar cycle, we must find an alternative way to disconnect emerging active regions, whilst conserving magnetic flux.

Citation

Whitbread, T., Yeates, A., & Munoz-Jaramillo, A. (2019). The need for active region disconnection in 3D kinematic dynamo simulations. Astronomy & Astrophysics, 627, Article A168. https://doi.org/10.1051/0004-6361/201935986

Journal Article Type Article
Acceptance Date Jul 3, 2019
Online Publication Date Jul 18, 2019
Publication Date Jul 1, 2019
Deposit Date Jul 5, 2019
Publicly Available Date Aug 1, 2019
Journal Astronomy and astrophysics.
Print ISSN 0004-6361
Electronic ISSN 1432-0746
Publisher EDP Sciences
Peer Reviewed Peer Reviewed
Volume 627
Article Number A168
DOI https://doi.org/10.1051/0004-6361/201935986

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Copyright Statement
Whitbread, T, Yeates, A. R. & Munoz-Jaramillo, A. (2019). The need for active region disconnection in 3D kinematic dynamo simulations. Astronomy & Astrophysics 627: A168, reproduced with permission, © ESO.





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