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Kinematic active region formation in a three-dimensional solar dynamo model

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

Kinematic active region formation in a three-dimensional solar dynamo model Thumbnail


Authors

A. Munoz-Jaramillo



Abstract

We propose a phenomenological technique for modelling the emergence of active regions within a three-dimensional, kinematic dynamo framework. By imposing localized velocity perturbations, we create emergent flux tubes out of toroidal magnetic field at the base of the convection zone, leading to the eruption of active regions at the solar surface. The velocity perturbations are calibrated to reproduce observed active region properties (including the size and flux of active regions, and the distribution of tilt angle with latitude), resulting in a more consistent treatment of flux-tube emergence in kinematic dynamo models than artificial flux deposition. We demonstrate how this technique can be used to assimilate observations and drive a kinematic three-dimensional model, and use it to study the characteristics of active region emergence and decay as a source of poloidal field.We find that the poloidal components are strongest not at the solar surface, but in the middle convection zone, in contrast with the common assumption that the poloidal source is located near the solar surface. We also find that, while most of the energy is contained in the lower convection zone, there is a good correlation between the evolution of the surface and interior magnetic fields.

Citation

Yeates, A., & Munoz-Jaramillo, A. (2013). Kinematic active region formation in a three-dimensional solar dynamo model. Monthly Notices of the Royal Astronomical Society, 436(4), 3366-3379. https://doi.org/10.1093/mnras/stt1818

Journal Article Type Article
Publication Date Dec 21, 2013
Deposit Date Dec 10, 2013
Publicly Available Date Jan 27, 2014
Journal Monthly Notices of the Royal Astronomical Society
Print ISSN 0035-8711
Electronic ISSN 1365-2966
Publisher Royal Astronomical Society
Peer Reviewed Peer Reviewed
Volume 436
Issue 4
Pages 3366-3379
DOI https://doi.org/10.1093/mnras/stt1818
Keywords Sun interior, Magnetic, Photosphere, Sunspots.

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Copyright Statement
This article has been published in the Monthly Notices of the Royal Astronomical Society.

© 2013 The Authors Published by Oxford University Press on behalf of The Royal Astronomical Society. All rights reserved.





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