FoRp r FG p r

which, using (3.1.95), leads to the first part of equation (3.1.97). Although formula (3.1.97) looks simple, the computations are complicated by the fact that the reference flux can only be computed for a predefined orientation of the irradiated surface. The surface in turn adjusts itself according to incident flux. Thus an iterative procedure is necessary which assumes first a surface normal pointing to the mass center of the irradiating star. The surface normal is then improved until convergence.

Once the functions 5**(0, p, r) are known, the modified Roche potentials

for and in the coordinate frame of component 1 and

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