Uniformly Rotating Main-Sequence Stars

Models of homogeneous, uniformly rotating main-sequence stars have been constructed by an ex- tension of the method described by Roxburgh, Griffith, and Sweet and results for three stellar masses are presented here Detailed opacity and nuclear energy generation data were included and the prescription due to Faulkner, Griffiths, and Hoyle was adopted to determine the surface boundary conditions. By subsequently fitting appropriate "gray" atmospheres at each latitude the changes in visual magnitude V and color index B - V were evaluated for a range of rotational velocities and aspect angles At maxi- mum rotational speed there are found to be differences of up to 1.3 mag in V and 0.25 mag in B - V for stars of the same mass seen at different orientation. The maximum spread in the main sequence ranges between 0.4 and 1.2 mag depending on color