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Coronal ejections from convective spherical shell dynamos

Published online by Cambridge University Press:  05 July 2012

J. Warnecke ,
P. J. Käpylä ,
M. J. Mantere  and
A. Brandenburg
J. Warnecke
Affiliation:
Nordita, Roslagstullsbacken 23, SE-10691 Stockholm, Sweden, email: joern@nordita.org Department of Astronomy, Stockholm University, SE-10691 Stockholm, Sweden
P. J. Käpylä
Affiliation:
Nordita, Roslagstullsbacken 23, SE-10691 Stockholm, Sweden, email: joern@nordita.org Department of Physics, PO BOX 64, FI-00014Helsinki University, Finland
M. J. Mantere
Affiliation:
Department of Physics, PO BOX 64, FI-00014Helsinki University, Finland
A. Brandenburg
Affiliation:
Nordita, Roslagstullsbacken 23, SE-10691 Stockholm, Sweden, email: joern@nordita.org Department of Astronomy, Stockholm University, SE-10691 Stockholm, Sweden
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Abstract

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We present a three-dimensional model of rotating convection combined with a simplified model of a corona in spherical coordinates. The motions in the convection zone generate a large-scale magnetic field which is sporadically ejected into the outer layers above. Our model corona is approximately isothermal, but it includes density stratification due to gravity.

Keywords

MHDSun: magnetic fieldsSun: coronal mass ejections (CMEs)turbulence
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S286: Comparative Magnetic Minima: Characterizing quiet times in the Sun and Stars , October 2011 , pp. 154 - 158
Copyright
Copyright © International Astronomical Union 2012

References

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Warnecke, J., Käpylä, P. J., Mantere, M. J., & Brandenburg, A. 2012, Sol. Phys. (in press, arxiv:1112.0505)Google Scholar