Journal
ASTROPHYSICAL JOURNAL
Volume 588, Issue 2, Pages 1183-1198Publisher
IOP PUBLISHING LTD
DOI: 10.1086/374313
Keywords
convection; Sun : magnetic fields; Sun : photosphere
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Turbulent convection in the solar photosphere can act as a small-scale dynamo, maintaining a disordered magnetic field that is locally intense. On the other hand, convection is inhibited in the presence of a strong, externally imposed magnetic field, as for instance, in a sunspot. Large-scale, three-dimensional, numerical experiments on highly nonlinear magnetoconvection in a Boussinesq fluid show that there is a continuous transition from a dynamo regime through a convective regime to an oscillatory regime as the strength of the imposed magnetic field is progressively increased. The patterns found in these different regimes are described and analyzed.
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