Astronomy and Astrophysics – Astronomy
Scientific paper
Jun 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000mnras.315..165t&link_type=abstract
Monthly Notices of the Royal Astronomical Society, Volume 315, Issue 1, pp. 165-183.
Astronomy and Astrophysics
Astronomy
19
Instabilities, Mhd, Sun: Magnetic Fields, Sunspots
Scientific paper
It is now widely accepted that the large-scale solar magnetic field is generated by some kind of non-linear αω-dynamo. However, these dynamos have the disadvantage that the non-linearities, and in particular the α-effect, are chosen in an ad hoc fashion and are only vaguely related to the underlying physical processes. Here, on the other hand, an αω-dynamo with an α-effect based on magnetic buoyancy instabilities is described. This α-effect has one main advantage over previous descriptions, namely that it is derived from a numerical model of the physical processes that are thought to occur at the base of the convection zone. In this paper we investigate a one-dimensional and a two-dimensional αω-dynamo in a cylindrical and a spherical shell, respectively. In both models the ω-effect is described by a simple shear flow, while α is proportional to the radial gradient of the magnetic field because, simply speaking, this gradient determines when magnetic buoyancy instabilities occur and hence when the α-effect sets in.
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