How does the shape and thickness of the tachocline affect the distribution of the toroidal magnetic fields in the solar dynamo?

Details How does the shape and thickness of the tachocline affect the distribution of the toroidal magnetic fields in the solar dynamo? How does the shape and thickness of the tachocline affect the distribution of the toroidal magnetic fields in the solar dynamo?

2006-10-24

arxiv.org/abs/astro-ph/0610703v1

Astronomy and Astrophysics

Astrophysics

Accepted for publication in A&A

Scientific paper

10.1051/0004-6361:20065834

Flux-dominated solar dynamo models, which have demonstrated to be quite successful in reproducing most of the observed features of the large scale solar magnetic cycle, generally produce an inappropriate latitudinal distribution of the toroidal magnetic fields, showing fields of large magnitude in polar regions where the radial shear has a maximum amplitude. Employing a kinematic solar dynamo model, we here explore the contribution of both the radial and the latitudinal shear in the generation of the toroidal magnetic fields by varying the shape and the thickness of the solar tachocline. We also explore the effects of the diffusivity profile of the convective zone. We find that the latitudinal component is always dominant over the radial component at producing toroidal field amplification. These results are very sensitive to the adopted diffusivity profile, specially in the inner convection zone. A diagram of the toroidal field at a latitude of 60 degrees versus the diffusivity at the convection layer for different values of the tachocline width has revealed that these fields are mainly eliminated for tachoclines with width d_1>0.08 Ro, for a restric range of diffusivites; or for d_1<0.02 and almost any value of eta_c in the appropriate solar range. For intermediate values of d_1=0.04Ro-0.06Ro, strong toroidal fields should survive at high latitudes in the butterfly diagram and those values are therefore not suitable.

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