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Existence and Energy Balance of the Solar Dynamo

  • J.H.G.M. van Geffen (a1)

Abstract

The idea behind the use of ensemble averaging and the finite magnetic energy method of van Geffen and Hoyng (1992) is briefly discussed. Applying this method to the solar dynamo shows that the turbulence — an essential ingredient of traditional mean field dynamo theory — poses grave problems: the turbulence makes the magnetic field so unstable that it becomes impossible to recognize any period.

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References

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Hoyng, P., “Turbulent transport of magnetic fields, II. The role of fluctuations in kinematic theory,” Astron. Astrophys. 171, 357 (1987).
Hoyng, P., “Turbulent transport of magnetic fields, III. Stochastic excitation of global magnetic modes,” Astrophys. J. 332, 857 (1988).
Krause, F. and Rädler, K.-H., Mean-Field Magnetohydrodynamics and Dynamo Theory , Pergamon Press, Oxford (1980).
Parker, E.N., Cosmical Magnetic Fields: their origin and their activity , Clarendon Press, Oxford (1979).
van Geffen, J.H.G.M., “Distribution of magnetic energy in αΩ-dynamos, II: a solar convection zone dynamo,” Geophys. & Astrophys. Fluid Dynamics , in press (1992a) (‘Paper II).
van Geffen, J.H.G.M., “Distribution of magnetic energy in αΩ-dynamos, III: a localized solar dvnamo,” Astron. Astrophys. , submitted (1992b) (‘Paper III).
van Geffen, J.H.G.M. and Hoyng, P., “Distribution of magnetic energy in αΩ-dynamos, I: the method,” Geophys. & Astrophys. Fluid Dynamics , in press (1992) (‘Paper I).

Existence and Energy Balance of the Solar Dynamo

  • J.H.G.M. van Geffen (a1)

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