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Cyclic magnetic activity due to turbulent convection in spherical wedge geometry
KTH, Centres, Nordic Institute for Theoretical Physics NORDITA.ORCID iD: 0000-0002-7304-021X
2012 (English)In: Astrophysical Journal Letters, ISSN 2041-8205, Vol. 755, no 1, L22- p.Article 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- p.
Keyword [en]
convection, magnetohydrodynamics (MHD), turbulence
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
URN: urn:nbn:se:kth:diva-102124DOI: 10.1088/2041-8205/755/1/L22ISI: 000306930700022Scopus ID: 2-s2.0-84864477375OAI: oai:DiVA.org:kth-102124DiVA: diva2:551258
Funder
Swedish Research Council, 621-2007-4064EU, European Research Council, 227952
Note

QC 20120910

Available from: 2012-09-10 Created: 2012-09-10 Last updated: 2013-08-28Bibliographically approved

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Brandenburg, Axel

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  • apa
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  • nn-NB
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  • Other locale
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