Internal solar rotation and the boundary layer non-linear dynamo
Most recent helioseismological results suggest the location of dynamo action in the boundary layer between the radiative and convective zones. This is confirmed by some preliminary results of a non-linear dynamo model in a spherical shell (0.05 Re thick, with full time and latitude resolution. The internal solar rotation profile deduced by helioseismological data is assumed. Periodic symmetric regime is found for negative helicity and absolute values of the dynamo number of order unity. These small values are compatible with the steep radial angular velocity gradient in the boundary layer.
KeywordsBoundary Layer Spherical Shell Convection Zone Differential Rotation Solar Dynamo
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- Belvedere, G., Pidatella, R.M., and Proctor, M.R.E. 1989, Geophys. Astrophys. Fluid Dyn., in press.Google Scholar
- Gilman, P.A., Morrow, C.A., and De Luca, E.E. 1989, Astrophys. J., 338, 528.Google Scholar
- Glatzmaier, G.A. 1985a, Geophys. Astrophys. Fluid Dyn., 31, 137.Google Scholar
- Harvey, J.W. 1988, in Seismology of the Sun and Sun-Like Stars, ed. E.J. Rolfe, ESA SP-286 (ESA Publication Division, Noordwijk), p.55.Google Scholar
- Rhodes, E.J., Cacciani, A., Korzennik, S., Tomczyk, S., Ulrich, R.K., and Woodard, M.F. 1990, Astrophys. J., in press.Google Scholar
- Spruit, H.C., and Van Ballegooijen, A.A. 1982, Astron. Astrophys., 106, 58.Google Scholar