Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999aas...193.9610m&link_type=abstract
American Astronomical Society, 193rd AAS Meeting, #96.10; Bulletin of the American Astronomical Society, Vol. 31, p.670
Astronomy and Astrophysics
Astronomy
Scientific paper
The generation of the solar magnetic field is investigated through an extension of the basic interface dynamo model of Parker (1993). In this model the generation of the strong toroidal field by the differential rotation takes place in a thin layer below the convection zone where the turbulent diffusivity is small, while the production of the poloidal field via the alpha-effect takes place within the convection zone. The two layers are coupled by diffusion across an interface at the base of the convection zone where the diffusivity is discontinuous. The dynamo equations are solved with a 2-D finite difference code in spherical coordinates. When the differential rotation is assumed to be purely radial, solutions analogous to those found by Parker (1993) are found, namely waves propagating along the interface. When the full two-dimensional rotational profile determined from helioseismology is included, however, these solutions are no longer found and only stationary solutions exist. This result is explained via a physical picture which demonstrates that the latitudinal component of the differential rotation dominates and prevents the solutions found when only the radial shear is considered. This result indicates a serious problem with the interface dynamo model.
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