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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

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