Modeling of differential rotation in rapidly rotating solar-type stars
arXiv:1107.2685 · doi:10.1088/0004-637X/740/1/12
Abstract
We investigate differential rotation in rapidly rotating solar-type stars by means of an axisymmetric mean field model that was previously applied to the sun. This allows us to calculate the latitudinal entropy gradient with a rea- sonable physical basis. Our conclusions are as follows: (1) Differential rotation approaches the Taylor-Proudman state when stellar rotation is faster than so- lar rotation. (2) Entropy gradient generated by the attached subadiabatic layer beneath the convection zone becomes relatively small with a large stellar angu- lar velocity. (3) Turbulent viscosity and turbulent angular momentum transport determine the spatial difference of angular velocity . (4) The results of our mean field model can explain observations of stellar differential rotation.
36 pages, 10 figures, accepted to ApJ
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