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Ejections of magnetic structures above a spherical wedge driven by a convective dynamo with differential rotation View all abstracts by submitter

Axel Brandenburg   Submitted: 2012-12-18 20:39

We combine a convectively driven dynamo in a spherical shell with a nearly isothermal density-stratified cooling layer that mimics some aspects of a stellar corona to study the emergence and ejections of magnetic field structures. This approach is an extension of earlier models, where forced turbulence simulations were employed to generate magnetic fields. A spherical wedge is used which consists of a convection zone and an extended coronal region to approx1.5 times the radius of the sphere. The wedge contains a quarter of the azimuthal extent of the sphere and 150degr in latitude. The magnetic field is self-consistently generated by the turbulent motions due to convection beneath the surface. Magnetic fields are found to emerge at the surface and are ejected to the coronal part of the domain. These ejections occur at irregular intervals and are weaker than in earlier work. We tentatively associate these events with coronal mass ejections on the Sun, even though our model of the solar atmosphere is rather simplistic.

Authors: J. Warnecke, P.J. Käpylä, M.J. Mantere, A. Brandenburg
Projects: None

Publication Status: Solar Phys. 280, 299-319 (2012)
Last Modified: 2012-12-19 12:10
Go to main E-Print page  A Note on Computation of Relative Magnetic Helicity Flux Across the Photosphere  Magnetic Activity Cycles in the Exoplanet Host Star epsilon Eridani  Edit Entry  Download Preprint  Submitter's Homepage Delete Entry 

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