cos y cos P

For the primary, the mid-disk intensity I0i is normalized to I0i = 1 which leads to I02 = J1 for the secondary component, where J1 and J2 are the (central) surface brightnesses of the stars. The numerical integration uses the GauB quadrature. In most cases, a 16 by 16 point integration is sufficient and leads to an accuracy of 0.0003 light units for spherical stars.

The total light I of the system is computed by adding the light of the components and subtracting the light lost during eclipse

Light is normalized to quarter phase, i.e., 1(0 = 0.25) = 1.

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