Stellar evolution with rotation IV: von Zeipel's theorem and anisotropic losses of mass and angular momentum

The von Zeipel theorem is generalised to account for differential rotation in the case of a "shellular" rotation law (cf. Zahn 1992). We write this la w in the form Omega - Omega(r), a simplification which does not apply to fa st rotation. We find that von Zeipel's relation contains a small additional term, generally further increasing the radiative flux at the pole and decr easing it at the equator. We also examine the local Eddington factor in rot ating stars and notice some significant differences with respect to current expressions. We examine the latitudinal dependence of the mass loss rates (M) over dot ( theta) in rotating stars and find two main source of wind anisotropies: 1) the L "g(eff)" effect which enhances the polar ejection; 2) the "opacity ef fect" (or "kappa-effect"), which favours equatorial ejection. In O-stars th e g(eff) effect is expected to largely dominate. In B- and later type stars the opacity effect should favour equatorial ejection and the formation of equatorial rings. We also examine the behaviour of the wind density and not ice a strong enhancement at the equator of B- and later type stars. Possibl e relations with the polar ejections and the skirt of eta Carinae and with the inner and outer rings of SN 1987 A are mentioned. If (M) over dot (?) h as sharp extrema due to some peaks in the opacity law, non equatorial and s ymmetrical rings may be produced. We also show that the global mass loss rate of a star at a given location i n the HR diagram is rapidly increasing with rotation, which is in good agre ement with the numerical models by Friend & Abbott (1986). Anisotropic stellar winds remove selectively the angular momentum. For exam ple, winds passing through polar caps in O-stars remove very little angular momentum, an excess of angular momentum is thus retained and rapidly redis tributed by horizontal turbulence. These excesses may lead some Wolf-Rayet stars, those resulting directly from O-stars, to be fast spinning objects, while we predict that the WR-stars which have passed through the red superg iant phase will have lower rotation velocities on the average. We also show how anisotropic ejection can be treated in numerical models by properly mo difying the outer boundary conditions for the transport of angular momentum . Finally, in an Appendix the equation of the surface for stars with shellu lar rotation is discussed.