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Solar Internal Rotation, the Boundary Layer Dynamo and Latitude Distribution of Activity Belts

Published online by Cambridge University Press:  12 April 2016

G. Belvedere ,
M.R.E. Proctor  and
G. Lanzafame
G. Belvedere
Affiliation:
Istituto di Astronomia, Università di Catania, Italy
M.R.E. Proctor
Affiliation:
Department of Applied Mathematics and Theoretical Physics, University of Cambridge, England
G. Lanzafame
Affiliation:
Istituto di Astronomia, Università di Catania, Italy

Abstract

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We suggest that the latitude distribution of solar activity belts and the related equatorward or poleward migration of different tracers of the solar cycle are a natural consequence of the internal radial profile of angular velocity via the working of a dynamo in the boundary layer beneath the convection zone. This has been confirmed by the results of a non-linear dynamo model in a very thin spherical shell which show that dynamo action may reasonably take place in the boundary layer and reproduce the observed surface phenomenology.

Extending the argument to late main-sequence stars, it is reasonable to think that observations of the latitude distribution and migration of stellar active regions by current sophisticated techniques may make it possible to infer their internal rotation profile in a simple and direct way.

Type
Part III Solar magnetism and large-scale flows
Information
International Astronomical Union Colloquium , Volume 130: The Sun and Cool Stars: activity, magnetism, dynamos , 1991 , pp. 237 - 240
Copyright
Copyright © Springer-Verlag 1991

References

Belvedere, G.: 1990, in Inside the Sun, Proc. IAU Coll. 121, Berthomieu, G. and Cribier, M. eds., Kluwer, Dordrecht, p. 371 CrossRefGoogle Scholar
Belvedere, G., Pidatella, R.M., Proctor, M.R.E.: 1990, Geophys. Astrophys. Fluid Dyn. 51, 263 CrossRefGoogle Scholar
Brown, T.M., Christensen-Dalsgaard, J., Dziembowski, W., Goode, P.R., Gough, D.O., Morrow, C.A.: 1989, Astrophya. J. 343, 526 Google Scholar
Dziembowski, W.A., Goode, P.R., Libbrecht, K.G.: 1989, Astrophys. J. 337, L53 Google Scholar
Glatzmaier, G.A.: 1985a, Geophys. Astrophys. Fluid Dyn. 31, 137 Google Scholar
Glatzmaier, G.A.: 1985b, Astrophys. J. 291, 300 Google Scholar
Harvey, J.W.: 1988, in Seiamology of the Sun and Sun-like Stara, Rolfe, E.J. ed., ESA-SP 286, 55 Google Scholar
Libbrecht, K.G.: 1989, Astrophys. J. 336, 1092 Google Scholar
Parker, E.N.: 1955, Astrophys. J. 122, 293 Google Scholar
Yoshimura, H.: 1975a, Astrophys. J. Suppl. 29, 467 Google Scholar
Yoshimura, H.: 1975b, Astrophys. J. 201, 740 Google Scholar