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.
Publisher
Cambridge University Press (CUP)
Reference7 articles.
1. Turbulent transport of magnetic fields. III - Stochastic excitation of global magnetic modes
2. “Turbulent transport of magnetic fields, II. The role of fluctuations in kinematic theory,”;Hoyng;Astron. Astrophys.,1987
3. van Geffen J.H.G.M. , “Distribution of magnetic energy in αΩ-dynamos, III: a localized solar dvnamo,” Astron. Astrophys. , submitted (1992b) (‘Paper III).
4. 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).