Are there different types of variability among B stars? |
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Authors: | J -P Sareyan J -M Le Contel J -C Valtier D Ducatel |
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Institution: | (1) Nice Observatory, B.P.n 252, 06007 Nice Cedex, France |
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Abstract: | Conclusion It now appears difficult to write that the Cephei stars occupy a well defined instability strip in the HR diagram (Lesh and Aizenman, 1978): the 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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