Toroidal Field Reversals and the Axisymmetric Tayler Instability

We present axisymmetric numerical simulations of the solar interior, including the convection zone and an extended radiative interior. We find that differential rotation in the convection zone induces a toroidal field from an initially purely poloidal field. This toroidal field becomes unstable to t...

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Bibliographic Details
Published in:The Astrophysical journal 2011-07, Vol.735 (2), p.100-jQuery1323906575239='48'
Main Author: Rogers, T. M
Format: Article
Language:English
Subjects:
Astronomy
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
AXIAL SYMMETRY
COMPUTERIZED SIMULATION
CONVECTION
Earth, ocean, space
ENERGY TRANSFER
Exact sciences and technology
FLUID MECHANICS
HEAT TRANSFER
HYDRODYNAMICS
INSTABILITY
MAGNETOHYDRODYNAMICS
MAIN SEQUENCE STARS
MASS TRANSFER
MECHANICS
SIMULATION
STARS
SUN
SYMMETRY
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Summary:We present axisymmetric numerical simulations of the solar interior, including the convection zone and an extended radiative interior. We find that differential rotation in the convection zone induces a toroidal field from an initially purely poloidal field. This toroidal field becomes unstable to the axisymmetric Tayler instability and undergoes equatorward propagating toroidal field reversals. These reversals occur in the absence of a dynamo and without accompanying poloidal field reversals. The nature and presence of such reversals depends sensitively on the initial poloidal field strength imposed, with north-south symmetric reversals only seen at a particular initial field strength. Coupled with a dynamo mechanism which regenerates the poloidal field this could be one ingredient in the sunspot cycle.
ISSN:0004-637X
1538-4357
DOI:10.1088/0004-637X/735/2/100