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Differential rotation on the lower main sequence
Author(s) -
Küker M.,
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.200410387
Subject(s) - differential rotation , rotation (mathematics) , physics , meridional flow , solar rotation , convection , differential equation , rotation around a fixed axis , astrophysics , classical mechanics , stars , zonal and meridional , mechanics , geometry , mathematics , solar physics , quantum mechanics , atmospheric sciences
We compute the differential rotation of main sequence stars of the spectral types F, G, K, and M by solving the equation of motion and the equation of convective heat transport in a mean‐field formulation. For each spectral type the rotation rate is varied to study the dependence of the surface shear on this parameter. The resulting rotation patterns are all solar‐type. The horizontal shear turns out to depend strongly on the effective temperature and only weakly on the rotation rate. The meridional flow depends more strongly on the rotation rate and has different directions in the cases of very slow and very fast rotation, respectively. (© 2005 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)