Cyclic magnetic activity due to turbulent convection in spherical wedge geometry
2012 (English)In: Astrophysical Journal Letters, ISSN 2041-8205, Vol. 755, no 1, L22- p.Article in journal (Refereed) Published
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.
convection, magnetohydrodynamics (MHD), turbulence
Astronomy, Astrophysics and Cosmology
IdentifiersURN: urn:nbn:se:kth:diva-102124DOI: 10.1088/2041-8205/755/1/L22ISI: 000306930700022ScopusID: 2-s2.0-84864477375OAI: oai:DiVA.org:kth-102124DiVA: diva2:551258
FunderSwedish Research Council, 621-2007-4064EU, European Research Council, 227952
QC 201209102012-09-102012-09-102013-08-28Bibliographically approved