Speaker
Petri J. Käpylä
(Department of Physics, University of Helsinki)
Description
We present results from three-dimensional simulations of rotating, magnetised,
turbulent convection in spherical wedge geometry. We concentrate on the parameter
regime where the differential rotation is solar-like, i.e. the equator rotates faster
than the poles. We find that large-scale magnetic fields are generated within the
whole convection zone. Many of the simulations show cyclic magnetic activity where
the activity belts migrate either poleward or equatorward. The direction of the
migration appears to change when the density
stratification of the convection zone is increased: equatorward (poleward) migration
is observed for high (low) stratification. The cycle period in the most solar-like
case is roughly 400 convective turnover times, corresponding to roughly 33 years.
Primary author
Petri J. Käpylä
(Department of Physics, University of Helsinki)
