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Solar-like differential rotation and equatorward migration in a convective dynamo with a coronal envelope

Published online by Cambridge University Press:  18 July 2013

J. Warnecke ,
P. J. Käpylä ,
M. J. Mantere  and
A. Brandenburg
J. Warnecke
Affiliation:
NORDITA, KTH Royal Institute of Technology and Stockholm University, Roslagstullsbacken 23, SE-10691 Stockholm, Sweden, email: joern@nordita.org Department of Astronomy, Stockholm University, SE-10691 Stockholm, Sweden
P. J. Käpylä
Affiliation:
NORDITA, KTH Royal Institute of Technology and Stockholm University, 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 Department of Information and Computer Science, Aalto University, PO Box 15400, FI-00076 Aalto, Finland
A. Brandenburg
Affiliation:
NORDITA, KTH Royal Institute of Technology and Stockholm University, 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 results of convective turbulent dynamo simulations including a coronal layer in a spherical wedge. We find an equatorward migration of the radial and azimuthal fields similar to the behavior of sunspots during the solar cycle. The migration of the field coexist with a spoke-like differential rotation and anti-solar (clockwise) meridional circulation. Even though the migration extends over the whole convection zone, the mechanism causing this is not yet fully understood.

Keywords

MHDSun: magnetic fieldsSun: activitySun: rotationturbulence

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