On Stellar Rotation: V. The Structure of Rotating Stars

In previous papers in this series the structure of rotating, upper main sequence stars was examined, and the distributions of angular momentum and magnetic field strength were derived under the assumption that there was no large scale meridional circulation. In this paper we obtain the changes in the remaining physical quantities due to the effect of rotation. Results are given for models with Schwarzschild, Kramers and electron scattering opacity laws and, in the latter case, for a series of values of magnetic field strength. The change in the position of a star in a plot of Mbolυ . log Te is given in terms of the parameter |$\lambda = \Omega_c{}^2 R_u{}^3/GM$| both for stars viewed pole on and perpendicular to the rotation axis. ( Ωc , the angular velocity of the convective core, R u the radius of a non-rotating star of mass M .) It is shown that the total luminosity of a star is reduced by rotation but that at a given value of T e rotating stars appear brighter than their non-rotating counterparts.