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DL Cyg

Borkovits1999 - Borkovits1999V (Johnson V)

The solution presented is from Borkovits & Biro (1999). They used a circumstellar cloud in the 1998 version of the Wilson-Devinney program (Wilson 1998) in their modeling that Binary Maker 3.0 does not have, so the model shown is without that effect. They give three separate models (a, b, c) and the model shown here is model “a” (assumes synchronous rotation of both stars). The lack of fit in the descending shoulder of primary eclipse is most likely due to the variable opacity of the gas stream coming from the L1 point and splashing onto the primary star. The occluding effect can be roughly simulated by placing a cooler region onto the primary star (see other model).