Journal
ASTROPHYSICAL JOURNAL LETTERS
Volume 755, Issue 1, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/2041-8205/755/1/L22
Keywords
convection; magnetohydrodynamics (MHD); turbulence
Categories
Funding
- Academy of Finland [136189, 140970, 218159, 141017]
- Swedish Research Council [621-2007-4064]
- European Research Council [227952]
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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.
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