Assuming that frequencies observed in multiperiod β Cephei variables correspond to normal pulsation modes leads to the following conclusions: (1) a variety of low Z oscillations are excited in these stars, (2) at most one radial mode is seen in any of them.

Pulsation constants can be derived for two β Cephei stars without recourse to photometric calibrations. In both cases a 0.5 mag. downward revision of the Balmer line absolute magnitudes is indicated. Implications of this result for Stellingwerf’s opacity bump mechanism are briefly considered.

The text of the paper will appear in Proceedings of the Fifth European Regional Meeting of the IAU.