Physics
Scientific paper
Oct 1989
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26a...223..343s&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 223, no. 1-2, Oct. 1989, p. 343-351.
Physics
76
Astronomical Models, Convection, Dynamo Theory, Nonlinear Evolution Equations, Solar Magnetic Field, Eigenvalues, Magnetic Field Configurations, Solar Physics
Scientific paper
A simple model of a boundary layer alpha-effect dynamo at the bottom of the solar convection zone is considered in order to study nonlinear solutions. After discussing the various modes that result from the solution of the linear eigenvalue problem the results of a numerical study are presented, including two different kinds of nonlinearities: (1) quenching of the alpha-effect for increasing amplitude of the magnetic field and (2) loss of magnetic flux from the dynamo region due to magnetic buoyancy or related instabilities. It turns out that the spectrum of nonlinear solutions, especially for alpha-effect quenching, is very complicated and that the results may sensitively depend on the initial conditions. Nonlinear modes appear which have no linear counterpart. The implications for the solar dynamo are discussed; it is argued that the flux loss nonlinearity leads to results which are in better accordance with the properties of the solar cycle. Consequences for the interpretation of observations of active stars are briefly mentioned.
Schmitt Denis
Schuessler Manfred
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