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The Light Curve of V444 Cygni

  • W.-R. Hamann (a1), E. Schwarz (a1) and U. Wessolowski (a1)

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In order to synthesize the eclipse light curve of V444 Cygni, we adopt the following model. The O star revolves round the WR star still within the outer regions of its extended atmosphere. The O star shadows a distinct volume of the WR atmosphere which thus cannot contribute to the total flux seen by the observer. On the other hand, additional radiation emerges from the surface of the O star. Its contribution to the total flux is more or less diminished by absorption when the rays pass through those parts of the WR atmosphere which lie between the O star and the observer. The WR atmosphere is given by our usual models (cf. Hamann and Schmutz, 1987; Wessolowski et al, 1988).

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References

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Cherepashchuk, A.M., Khalliullin, K.F.: 1973, Soviet Astr. - AJ 17, 330
Cherepashchuk, A.M., Eaton, J.A., Khalliullin, K.F.: 1984, Ap. J. 281, 774
Hamann, W.-R., Schmutz, W.: 1987, Astr. Ap. 174, 173
Wessolowski, U., Schmutz, W., Hamann, W.-R: 1988, Astr. Ap. 194, 160

The Light Curve of V444 Cygni

  • W.-R. Hamann (a1), E. Schwarz (a1) and U. Wessolowski (a1)

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