Cyclic magnetic activity due to turbulent convection in spherical wedge geometry

We report on simulations of turbulent, rotating, stratified, magnetohydrodynamic convection in spherical wedge geometry. An initially small-scale, random, weak-amplitude magnetic field is amplified by several orders of magnitude in the course of the simulation to form oscillatory large-scale fields...

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Bibliographic Details
Published inarXiv.org
Main Authors Käpylä, Petri J, Mantere, Maarit J, Brandenburg, Axel
Format Paper Journal Article
LanguageEnglish
Published Ithaca Cornell University Library, arXiv.org 18.11.2013
Subjects
Convection
Differential rotation
Fluid dynamics
Fluid flow
Latitude
Magnetism
Magnetohydrodynamic turbulence
Magnetohydrodynamics
Physics - Solar and Stellar Astrophysics
Solar cycle
Solar rotation
Wedges
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Summary:We report on simulations of turbulent, rotating, stratified, magnetohydrodynamic convection in spherical wedge geometry. An initially small-scale, random, weak-amplitude magnetic field is amplified by several orders of magnitude in the course of the simulation to form oscillatory large-scale fields in the saturated state of the dynamo. The differential rotation is solar-like (fast equator), but neither coherent meridional poleward circulation nor near-surface shear layer develop in these runs. In addition to a poleward branch of magnetic activity beyond 50 degrees latitude, we find for the first time a pronounced equatorward branch at around 20 degrees latitude, reminiscent of the solar cycle.
Bibliography:Nordita-2012-040
ISSN:2331-8422
DOI:10.48550/arxiv.1205.4719