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V444 Cygni and CQ Cephei, Key Wolf-Rayet Binary Stars

Published online by Cambridge University Press:  03 August 2017

Anne B. Underhill
Anne B. Underhill*
Affiliation:
Department of Geophysics and Astronomy University of British Columbia Vancouver, B. C. V6T 1W5, Canada

Extract

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Radial-velocity and photometric observations of eclipsing binaries allow one to estimate the masses of the stars in such systems, their relative brightnesses and sizes. If polarization variations are detected throughout the binary period, one may confirm the inclination of the system. All three types of information are available for V444 Cygni and CQ Cephei, see Underhill, Yang, and Hill (1988a,b), Underhill, Gilroy, and Hill (1990), and the references quoted in those papers.

Type
Session IV. Binaries
Information
Symposium - International Astronomical Union , Volume 143: Wolf–Rayet Stars and Interrelations with other Massive Stars in Galaxies , 1991 , pp. 255
Copyright
Copyright © Kluwer 1991 

References

REFERENCES

Maeder, A., and Meynet, G. 1988, Astr. Ap., 76, 411.Google Scholar
Underhill, A. B., Gilroy, K. K., and Hill, G. M. 1990, Ap. J., 351, 651.Google Scholar
Underhill, A. B., Yang, S., and Hill, G. M. 1988a, P. A. S. Pacific, 100, 741.Google Scholar
Underhill, A. B., Yang, S., and Hill, G. M. 1988b, P. A. S. Pacific, 100, 1256.Google Scholar