Massive stars are known to pulsate at many stages of evolution. Most spectacular are the Luminous Blue Variables (LBVs), in which pulsation is one possible origin for the S-Dor type outbursts. In this work, we study the radial pulsations of stars with initial masses of 20,40, 60 and 85 M_(?) using both linear and non-linear pulsation codes. The pulsations can then interact with time-dependent convection, which increases the luminosity until the Eddington limit is exceeded locally, potentially driving mass loss and S-Dor outbursts. We consider models at various stages of evolution and metallicity, covering the observed properties of the majority of the observed LBV and LBV candidates. Preliminary results characterizing the pulsations as functions of Y and Z are presented.
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