Astronomy and Astrophysics – Astronomy
Scientific paper
Oct 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998mnras.300..397r&link_type=abstract
Monthly Notices of the Royal Astronomical Society, Volume 300, Issue 2, pp. 397-410.
Astronomy and Astrophysics
Astronomy
4
Chaos, Mhd, Sun: Activity, Sun: Magnetic Fields, Stars: Magnetic Fields
Scientific paper
In an attempt to produce a simple representation of an interface dynamo, I examine a dynamo model composed of two one-dimensional (radially averaged) pseudo-spherical layers, one in the convection zone and possessing an alpha-effect, and the other in the tachocline and possessing an omega-effect. The two layers communicate by means of an analogue of Newton's law of cooling, and a dynamical back-reaction of the magnetic field on omega is provided. Extensive bifurcation diagrams are calculated for three separate values of epsilon, the ratio of magnetic diffusivities of the two layers. I find recognizable similarities to, but also dramatic differences from, the comparable one-layer model examined by Roald & Thomas. In particular, the solar-like dynamo mode found previously is no longer stable in the two-layer version; in its place there is a sequence of periodic, quasi-periodic and chaotic modes probably created in a homoclinic bifurcation. These differences are important enough to provide support for the view that the solar dynamo cannot be meaningfully modelled in one dimension.
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