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. © 2008 IOP Publishing Ltd.