A dynamo model for axisymmetric and non-axisymmetric solar magnetic fields

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dc.creatorJiang, J.
dc.creatorWang, J. X.
dc.date2007-02-20
dc.date.accessioned2026-07-07T10:21:49Z
dc.date.available2026-07-07T10:21:49Z
dc.descriptionIncreasing observations are becoming available about a relatively weak, but persistent, non-axisymmetric magnetic field co-existing with the dominant axisymmetric field on the Sun. It indicates that the non-axisymmetric magnetic field plays an important role in the origin of solar activity. A linear non-axisymmetric alpha2-Omega dynamo model is set up to discuss the characteristics of the axisymmetric m=0 and the first non-axisymmetric m=1 modes and to provide further the theoretical bases to explain the active longitude, flip-flop and other non-axisymmetric phenomena. The model consists of a updated solar internal differential rotation, a turbulent diffusivity varied with depth and an alpha-effect working at the tachocline in rotating spherical systems. The difference between the alpha2-Omega and the alpha-Omega models and the conditions to favor the non-axisymmetric modes with the solar-like parameters are also presented.
dc.description9 pages, 9 figures, and 2 tabels; MNRAS accepted
dc.identifierhttps://arxiv.org/abs/astro-ph/0702508
dc.identifierhttp://arxiv.org/abs/astro-ph/0702508
dc.identifierMon.Not.Roy.Astron.Soc.377:711-718,2007
dc.identifierdoi:10.1111/j.1365-2966.2007.11644.x
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/175303
dc.subjectAstrophysics
dc.titleA dynamo model for axisymmetric and non-axisymmetric solar magnetic fields
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