Main-sequence instability strip for different opacities and heavy element abundances: a comparison with observations
Abstract
Updated theoretical instability domains are presented for β Cephei and SPB star models. Calculations were performed using new OP opacities for old (GN93) and new (A04) solar heavy element mixtures. The position of observed β Cephei and SPB variables in the HR and related diagrams is compared with theoretical domains for three heavy element mass fractions: Z = 0.020, 0.015 and 0.010.
- Publication:
-
Journal of Physics Conference Series
- Pub Date:
- October 2008
- DOI:
- 10.1088/1742-6596/118/1/012079
- Bibcode:
- 2008JPhCS.118a2079Z