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Differential rotation and meridional flow in the solar convection zone and beneath
Author(s) -
Kitchatinov L. L.,
Rüdiger G.
Publication year - 2005
Publication title -
astronomische nachrichten
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 0.394
H-Index - 63
eISSN - 1521-3994
pISSN - 0004-6337
DOI - 10.1002/asna.200510368
Subject(s) - meridional flow , differential rotation , radiation zone , helioseismology , convection zone , tachocline , physics , solar rotation , geophysics , dynamo , turbulence , mechanics , convection , laminar flow , zonal and meridional , radiative transfer , rotation (mathematics) , dynamo theory , geology , atmospheric sciences , astrophysics , geometry , solar physics , magnetic field , optics , stars , mathematics , quantum mechanics
The influence of the basic rotation on anisotropic and inhomogeneous turbulence is discussed in the context of differential rotation theory. An improved representation for the original turbulence leads to a Λ ‐effect which complies with the results of 3D numerical simulations. The resulting rotation law and meridional flow agree well with both the surface observations (∂ Ω /∂ r < 0 and meridional flow towards the poles) and with the findings of helioseismology. The computed equatorward flow at the bottom of convection zone has an amplitude of about 10 m/s and may be significant for the solar dynamo. The depth of the meridional flow penetration into the radiative zone is proportional to ν 0.5 core , where ν core is the viscosity beneath the convection zone. The penetration is very small if the tachocline is laminar. (© 2005 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)