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CYCLIC MAGNETIC ACTIVITY DUE TO TURBULENT CONVECTION IN SPHERICAL WEDGE GEOMETRY
Stockholm University, Faculty of Science, Department of Astronomy. Stockholm University, Nordic Institute for Theoretical Physics (Nordita).
2012 (English)In: Astrophysical Journal Letters, ISSN 2041-8205, E-ISSN 2041-8213, Vol. 755, no 1, L22Article in journal (Refereed) Published
Abstract [en]

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.

Place, publisher, year, edition, pages
2012. Vol. 755, no 1, L22
Keyword [en]
convection, magnetohydrodynamics (MHD), turbulence
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
URN: urn:nbn:se:su:diva-81570DOI: 10.1088/2041-8205/755/1/L22ISI: 000306930700022OAI: oai:DiVA.org:su-81570DiVA: diva2:563302
Note

AuthorCount:3;

Available from: 2012-10-29 Created: 2012-10-25 Last updated: 2017-12-07Bibliographically approved

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