SIMBAD references

The stability with respect to radial perturbations of massive zero-age main-sequence stars having solar chemical composition and masses between 50 and 150 M_☉ is reinvestigated. As a first step, a linear non-adiabatic stability analysis is performed, confirming the existence of dynamical strange mode instabilities for models with masses above 58 M_☉. For selected models, the evolution of the strange mode instabilities into the non-linear regime is followed by numerical simulation. The final results of strange mode instabilities are thus found to be finite amplitude pulsations with periods between 3 and 24 h. Mean acoustic luminosities capable to drive winds with mass-loss rates of the order of 0.5 x 10^–7 M_☉ yr^–1, which can at most marginally affect stellar evolution in the vicinity of the zero-age main sequence, are associated with these finite amplitude pulsations.