Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 1988
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988mnras.230...55u&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 230, Jan. 1, 1988, p. 55-68. NSERC-supported research.
Astronomy and Astrophysics
Astronomy
5
Stellar Atmospheres, Stellar Interiors, Stellar Models, Stellar Temperature, Supermassive Stars, Absorption Spectra, Continuous Spectra, Emission Spectra, Line Spectra, O Stars, Stellar Winds, Wolf-Rayet Stars
Scientific paper
The problem of identifying real massive stars with models of the interiors and atmospheres of massive stars is reviewed. The usual way to identify a star with a stellar interior model is through the effective temperature estimated from the integrated flux of the star or from spectrum analysis and any two of the parameters log g, stellar radius, and stellar mass. It is noted that the discrepancies between the observed absorption-line and emission-line spectra of massive stars and spectra predicted using models which represent the continuum forming parts of the atmospheres give information about the physical state of the line forming regions outside the photosphere of the star. This state may be generated by factors additional to the radiation field which is generated in the interior of the star by nuclear reactions. Consequently Wolf-Rayet and Of spectral types may be used as indices of the stage of evolution of a massive star only after it has been shown that the factors generating emission lines can be related in a monotonic manner with the changes which occur in a model massive star as time increases and the model star evolves. The foundations of two views of the evolutionary status of Wolf-Rayet stars are compared and evaluated.
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