Conclusion
It now appears difficult to write that “the β Cephei stars occupy a well defined “instability strip” in the HR diagram (Lesh and Aizenman, 1978): the β Cep phenomenon — from any observational definition we could give — cannot be restricted to the small group of variables inside the box limited by the B 0.5 - B 2 spectral types and by the (II–III) – IV luminosity classes.
So the pulsation mechanism is probably not strictly related to a narrow evolutionary stage. From this point of view, a mechanism related to envelope properties could better allow for variability in a wider region of the HR diagram. Which should be the new boundaries for such a phenomenon ? Should we expect an “amplification” of the phenomenon towards the center of its HR domain?
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Sareyan, J.P., Le Contel, J.M., Valtier, J.C. et al. Are there different types of variability among B stars?. Space Sci Rev 27, 353–359 (1980). https://doi.org/10.1007/BF00168320
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DOI: https://doi.org/10.1007/BF00168320