Abstract
Meridional flow and rotation law are computed for convection zones of solar-type stars. The solar differential rotation known by helioseismology is reproduced with the hydrodynamic theory of the Lambda-effect. The meridional flow in the convection zone is of order 5-10 m/s and returns to the equator at its base. The present-day models only yield one cell in latitude in each hemisphere. For the theory of the polar branch a double-cell flow pattern would be helpful. For eddy diffusivities of 1011cm2/s the meridional flow adopts magnetic Reynolds numbers of order102_..3so that drastic consequences for the solar dynamo can be expected.
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© 2000 Springer Science+Business Media Dordrecht
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Rüdiger, G. (2000). Differential Rotation, Meridional Flow and a High-Prandtl Number Solar/Stellar Dynamo. In: Cheng, K.S., Chau, H.F., Chan, K.L., Leung, K.C. (eds) Stellar Astrophysics. Astrophysics and Space Science Library, vol 254. Springer, Dordrecht. https://doi.org/10.1007/978-94-010-0878-5_2
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DOI: https://doi.org/10.1007/978-94-010-0878-5_2
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