Rucinskis Model

Rucinski's WUMA3 uses sky-grid integration and hence has low integration efficiency, requiring at least 10,000 integration points. The intention was to have a program which would be totally free of systematic errors related to uneven distribution of integration points. Other properties are

• Roche model (only for equipotentials between the inner and outer critical common envelopes);

• interpolation between semi-empirical, color-index-based fluxes;

• differential corrections via Rucinski's least-squares program;

• no spots are modeled but provision to change temperature or surface brightness along (or on one side of) the common equipotential;

• line profiles calculated in WUMA3's descendants (WUMA5 and WUMA6);

• input through a separate parameter file;

• extreme simplicity and modular structure permit easy modification.

This code is not supported generally and has restricted distribution. According to Rucinski, there is no intention at present to continue development of the WUMAn codes.

6.3.6 Wilson-Devinney Models The 1998 Wilson-Devinney Model

The original Wilson-Devinney model and program has been extended in many publications and software releases [Wilson & Devinney (1971), Wilson (1979, 1990, 1993)]. All versions released after 1982 treat elliptic orbits with eccentricity, e, and semi-major axis, a. The constant distance between the stars is replaced by the phase-dependent distance d = d($>). Nonsynchronous rotation of components is described by a parameter F which is the ratio of rotational angular velocity to mean orbital angular velocity. The surfaces of the components are derived from the Roche equipotentials, defined as

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