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Published online by Cambridge University Press: 07 February 2017
Following Davey (1973), we have considered the linear radial pulsational stability of stellar models in the region of the HR diagram populated by β Cephei stars. Instead of one composition, however, we have considered many compositions, some of them rather extreme. No consideration of composition changes for temperatures above a few-million degrees was given, and therefore the stellar structure and its pulsational stability may not be evaluated very accurately. Modulation of nuclear reactions was also neglected. In no case was radial pulsational instability found.