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Mechanisms for Dynamo Mode Excitation

Published online by Cambridge University Press:  19 July 2016

P. Hoyng
P. Hoyng*
Affiliation:
Laboratory for Space Research Sorbonnelaan 2, 3584 CA Utrecht The Netherlands

Extract

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Dynamo theory of the solar magnetic field finds itself in a period of reappraisal since about 1980. There are two reasons for this: (1) The required increase of the angular speed Ω, with decreasing r is neither found in numerical simulations nor measured by helioseismology. (2) Mean field modeling shows often little regard for inherent physical restrictions and selfconsistency.

Type
II. The Solar Interior
Information
Symposium - International Astronomical Union , Volume 142: Basic Plasma Processes on the Sun , 1990 , pp. 45 - 49
Copyright
Copyright © Kluwer 1990 

References

Belvedere, G., Pidatella, R.M. and Proctor, R.M.E.: 1989, Geophys. Astrophys. Fluid Dynamics , to appear.Google Scholar
Brandenburg, A., Moss, D. and Tuominen, I.: 1989, Geophys. Astrophys. Fluid Dynamics , to appear.Google Scholar
Feynman, J. and Gabriel, S.B.: 1990, Solar Physics , to appear.Google Scholar
Gokhale, M.H. and Javaraiah, J.: 1990, M.N.R.A.S. , to appear.Google Scholar
Hoyng, P.: 1990, in Solar photosphere: Structure, Convection, and Magnetic fields , ed. Stenflo, J.O., Kluwer (Dordrecht), p. 359.Google Scholar
Rai Choudhuri, A.: 1990a, these proceedings.Google Scholar
Rai Choudhuri, A.: 1990b, Astrophys. J. , to appear.Google Scholar
Schmitt, D. and Schüssler, M.: 1989, Astron. Astrophys. 223, 343.Google Scholar