Fig. 6
The position of the β Cephei and candidate β Cephei stars in the H-R diagram. Upper panel: the boundaries of the theoretical instability strips are calculated using the OP opacities. Lower panel: boundaries are calculated using OPAL opacities. Full lines correspond to strips for metallicity Z = 0.01 and dotted lines to strips with metallicity Z = 0.02. The thick and thin lines correspond to the boundaries of the β Cephei and SPB instability regions, respectively.
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