Abstract
An improved version of the OPAL opacities, with the metal abundance parameter Z having values of 0.02 and 0.03, has been used in a stability survey for models of 7- to 16-M ○ . stars in the main-sequence (MS) and early post-MS evolutionary phases. All β Cep stars lie within the domain of the HR diagram where pulsational instability is caused by the opacity mechanism acting in the metal opacity bump at T ≃ 2 × 10 5 K. For most of the objects, a value of Z = 0.02 suffices to account for the pulsation. The positions of β Cep stars in the HR diagram correspond to models in an advanced phase of core hydrogen burning, constructed without allowing for effects of the convective overshooting
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