Main-sequence instability strip for different opacities and heavy element abundances: a comparison with observations

Details Main-sequence instability strip for different opacities and heavy element abundances: a comparison with observations Main-sequence instability strip for different opacities and heavy element abundances: a comparison with observations

Oct 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008jphcs.118a2079z&link_type=abstract

Journal of Physics: Conference Series, Volume 118, Issue 1, pp. 012079 (2008).

Physics

10

Scientific paper

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.

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