Astronomy and Astrophysics – Astrophysics
Scientific paper
Jul 1980
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980ap%26ss..70..441c&link_type=abstract
Astrophysics and Space Science, vol. 70, no. 2, July 1980, p. 441-445. Research supported by the Consiglio Nazionale delle Rice
Astronomy and Astrophysics
Astrophysics
Stellar Mass Ejection, Stellar Winds, Supermassive Stars, Variable Stars, Hertzsprung-Russell Diagram, Stellar Evolution, Stellar Luminosity, Systems Stability
Scientific paper
The effects of mass loss by stellar winds in massive stars on the Beta Cephei instability strip on the HR diagram are discussed. It is pointed out that the mass extension of semiconvective zones during the core hydrogen-burning phase is critically dependent on mass loss rate, and that the effective temperatures derived for Beta Cephei stars are too low to permit core hydrogen burning as inferred from the position of the instability strip on the HR diagram. It is then shown that part of the disagreement can be removed if mass loss is taken into account in the computation of theoretical models of Beta Cephei pulsation. The application of a model such as that of Osaki (1971, 1974) to the intermediate fully convective zone of mass-losing stars would then predict the existence of the instability strip for stars with masses greater than 8-10 solar masses and less than 20 to 25 solar masses, as is observed.
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