Analysis of the Light Changes in the Frequency-Domain: Distorted Stars

Abstract

In the preceding chapter of this book we outlined the basic principles of the analysis of the light curves of eclipsing binary systems in the frequency-domain; and presented an explicit form of such an analysis appropriate for the case in which both components can be regarded as spheres. With the completion of this task the question is, however, bound to arise as to the extent to which a model consisting of spherical stars can be regarded as a satisfactory representation of eclipsing systems actually encountered in the sky; for axial rotation of their components and their mutual tidal distortion is bound to cause them to depart from spherical form. In many known eclipsing systems, to be sure, the components are separated widely enough — and, consequently, their distortion is sufficiently small — that (within the limits of observational errors) they can be regarded as spheres; and methods expounded in Chapter V applied to the observations as they stand.