The stellar structure equations for uniformly rotating, synchronous close binaries have been derived using a modified double approximation technique which has been successful in studies of rotating stars and close binary polytropes. The auxiliary functions which are necessary to obtain interior models have been derived and their numerical values are given for various mass ratios. In order to calculate the apparent luminosities and colours of binary models the effects of gravity darkening (either radiative or convective) must be taken into account. Tables are presented for different degrees of distortion, mass ratio, and the two extremes of inclination which allow the apparent luminosity and mean effective temperature to be determined if the interior luminosity and separation of the components are given.
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- 1 - Physical Sciences ; 2 - Earth and Planetary Sciences ; 3 - Space and Planetary Science
- 1 - Physical Sciences ; 2 - Physics and Astronomy ; 3 - Astronomy and Astrophysics