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We have calculated the pulsations of massive stars using a nonlinearhydrodynamic code including time-dependent convection. The basic structuremodels are based on a standard grid published by Meynet et al. (1994). Usingthe basic structure, we calculated envelope models, which include the outer fewpercent of the star. These models go down to depths of at least 2 million K.These models, which range from 40 to 85 solar masses, show a range of pulsationbehaviours. We find models with very long period pulsations ( $>$ 100 d),resulting in high amplitude changes in the surface properties. We also find afew models that show outburst-like behaviour. The details of this behaviour arediscussed, including calculations of the resulting wind mass-loss rates.

Behaviour of Pulsations in Hydrodynamic Models of Massive Stars