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The Light Curve of V444 Cygni

Published online by Cambridge University Press:  03 August 2017

W.-R. Hamann ,
E. Schwarz  and
U. Wessolowski
W.-R. Hamann
Affiliation:
Institut für Theoretische Physik und Sternwarte der Universität, Olshausenstraße 40, D-2300 Kiel, Federal Republic of Germany
E. Schwarz
Affiliation:
Institut für Theoretische Physik und Sternwarte der Universität, Olshausenstraße 40, D-2300 Kiel, Federal Republic of Germany
U. Wessolowski
Affiliation:
Institut für Theoretische Physik und Sternwarte der Universität, Olshausenstraße 40, D-2300 Kiel, Federal Republic of Germany

Extract

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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).

Type
Session IV. Binaries
Information
Symposium - International Astronomical Union , Volume 143: Wolf–Rayet Stars and Interrelations with other Massive Stars in Galaxies , 1991 , pp. 254
Copyright
Copyright © Kluwer 1991 

References

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