Theoretical Photometry of Distorted Eclipsing Systems
In the preceding chapter of this book an outline has been given of the mathematical theory of eclipsing binary systems as long as their components (characterized by an arbitrary distribution of brightness on their apparent discs) can be regarded as spherical, and would appear in projection on the celestial sphere as circular discs. The question is, however, bound to be raised as to the extent to which such a model can be regarded as a satisfactory representation of close binaries actually encountered in the sky. This would, in principle, be legitimate only in the absence of forces which distort the shape of both components and cause their equipotential surfaces to depart from spheres: these are, however, ever present in the form of axial rotation of the components, and of their mutual tidal action. A theory of the effects produced by such forces has recently been summarized by the present writer in another volume (cf. Kopal, 1989), to which the reader is referred for fuller details that need not be repeated in this place.
KeywordsMain Sequence Direction Cosine Secondary Component Equipotential Surface Light Change
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