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3. Wolf-Rayet star atmospheres

Published online by Cambridge University Press:  25 April 2016

David C. Abbott

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Wolf-Rayet (WR) stars are the helium-burning remnants of massive stars (initial mass ≲30 M©), which have lost their outer hydrogen-rich layers through the processes of Roche lobe overflow to a companion or mass loss by a strong stellar wind. The characteristic emission-line spectrum which defines the WR spectral type is produced by a stellar wind that is so dense and opaque, that the radiation of all lines and continua arise from material in the wind. Because the wind completely screens any radiation emitted by the hydrostatic core of the star, the spectra of WR stars are nearly impossible to interpret quantitatively, and the basic parameters — such as mass, luminosity, temperature, and chemical composition — are poorly determined.

Type
Research Article
Information
Transactions of the International Astronomical Union , Volume 19 , Issue 1 , 1985 , pp. 510 - 513
Copyright
Copyright © Reidel 1985

References

Abbott, D.C.: 1984, in Radio Stars, eds. Hjellming, R.M. (Reidel: Dordrecht), in press.Google Scholar
Abbott, D.C. and Hummer, D.G.: 1984, submitted to Astrophys. J.Google Scholar
Barlow, M.J., Smith, L.J. and Willis, A.J.: 1981, Monthly Notices Peu. Astron. Soc. 196, 101.CrossRefGoogle Scholar
Bieging, J.H., Abbott, D.C. and Churchwell, E.: 1982, Astrophys. J. 263, 207.CrossRefGoogle Scholar
Castor, J.I. and Lamers, H.J.G.L.M.: 1979, Astrophys. J. Suppl. 39, 481.CrossRefGoogle Scholar
Castor, J.I. and Van Blerkom, D.: 1970, Astrophys. J. 161, 485.CrossRefGoogle Scholar
Cherepashchuk, A.M., Eaton, J.A. and Khaliullin, Kh. F.: 1984, Astrophys. J. 281,774.CrossRefGoogle Scholar
Conti, P.S., Leep, E.M. and Perry, D.N.: 1983, Astrophys. J. 268, 228.CrossRefGoogle Scholar
Garmany, C.D., Massey, P. and Conti, P.S.: 1984, Astrophys. J. 278, 233.CrossRefGoogle Scholar
Hamann, W.R.: 1984, Astron. Astrophys, submitted.Google Scholar
Hillier, D.J.: 1983, Ph.D. Thesis, Australian National University, Canberra.Google Scholar
Lundström, I. and Stenholm, B.: 1984, preprint.Google Scholar
Maeder, A.: 1982, Astron. Astrophys. 105, 149.Google Scholar
Maeder, A.: 1984, in Observational Tests of the Stellar Evolution Theory, eds. Maeder, A. and Renzini, A. (Dordrecht: Reidel), p. 299.CrossRefGoogle Scholar
Massey, P.: 1982, in Wolf-Rayet Stars: Observations, Physios and Evolution, eds. Loore, C.W.H. de and Willis, A.J. (Dordrecht: Reidel), p. 251.CrossRefGoogle Scholar
Massey, P.: 1984, Astrophys. J. 281, 789.CrossRefGoogle Scholar
Massey, P. and Conti, P.S.: 1983, Astrophys. J. 264, 126.CrossRefGoogle Scholar
Massey, P., Conti, P.S. and Niemela, V.S.: 1981, Astrophys. J. 246, 145.CrossRefGoogle Scholar
Niemela, V.: 1979, in Mass Loss and Evolution of O-Type Stars, eds. Conti, P.S. and Loore, C.W.H. de (Dordrecht: Reidel), p. 291.CrossRefGoogle Scholar
Prévot-Burnichon, M.L., Prévot, L., Rebeirot, E., Rousseau, J. and Martin, N.: 1981,Astron. Astrophys. 103, 83.Google Scholar
Schmutz, W.: 1984, in Observational Tests of the Stellar Evolution Theory, eds. Maeder, A. and Renzini, A. (Dordrecht: Reidel), p. 269.CrossRefGoogle Scholar
Smith, L.J. and Willis, A.J.: 1982, Monthly Notices Roy. Astron. Soo. 201, 451.CrossRefGoogle Scholar
Torres, A. and Conti, P.S.: 1984, Astrophys. J. 280, 181.CrossRefGoogle Scholar
Vreux, J.M.: 1984, preprint.Google Scholar