Are there different types of variability among B stars?
Abstract
It is maintained that the beta Cephei stars do not occupy a well-defined instability strip in the HR diagram. Hence, the beta Ceph phenomenon cannot be restricted to the small group of variables inside the box limited by the B0.5-B2 spectral types and by the (II-III)-IV luminosity classes. Furthermore, the pulsation mechanism is probably not strictly related to a narrow evolutionary stage.
- Publication:
-
Space Science Reviews
- Pub Date:
- December 1980
- DOI:
- 10.1007/BF00168320
- Bibcode:
- 1980SSRv...27..353S
- Keywords:
-
- B Stars;
- Stellar Oscillations;
- Variable Stars;
- Hertzsprung-Russell Diagram;
- Stellar Evolution;
- Stellar Luminosity;
- Astronomy