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 inAstrophysical journal. Letters Vol. 755; no. 1; pp. 1 - 5
Main Authors Kapyla, Petri J, Mantere, Maarit J, Brandenburg, Axel
Format Journal Article
LanguageEnglish
Published United States 10.08.2012
Subjects
ASTROPHYSICS
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
CONVECTION
Differential rotation
Fluid dynamics
Latitude
LAYERS
MAGNETIC FIELDS
MAGNETOHYDRODYNAMICS
magnetohydrodynamics (MHD)
RANDOMNESS
ROTATION
SHEAR
Shear layers
Simulation
SOLAR CYCLE
SPHERICAL CONFIGURATION
SURFACES
TURBULENCE
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:ObjectType-Article-1
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ISSN:2041-8205
2041-8213
2041-8213
DOI:10.1088/2041-8205/755/1/L22