It is assumed that the meridional motions (U) and angular velocity (g2) in the surface layers of the convection zone are given by simple expressions of the form: Ur=2~t(r)P2(cosO)/Qr 2, Uo = --~u'(r) sin0 cosO/er, and ~ =-(20[(1 + coo(r) + c02 (r) P2(cos0)]. Here q/(r) is the stream function, P2 (co
On differential rotation
✍ Scribed by H. Köhler
- Publisher
- Springer
- Year
- 1974
- Tongue
- English
- Weight
- 142 KB
- Volume
- 34
- Category
- Article
- ISSN
- 0038-0938
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✦ Synopsis
In a first order approximation the influence of meridional circulations in a spherical shell on the radial dependence of the angular velocity is studied. Due to stationarity the flux of angular momentum which is transported through any sphere by the circulations must be cancelled by the flux of angular momentum due to turbulent friction. If the circulation goes equatorward at the outer surface the law of rotation must be such that angular momentum is transported in outward direction through the sphere.
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## Abstract 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