the evolution is rather modest. For instance, a star with initial mass of $16 M_\odot$ loses only about $0.8 M_\odot$ during the evolution from ZAMS to the point when helium is depleted in its core. The maximum value of the mass-loss rate is reached on the tip of the red giant branch and for the $16 M_\odot$ star it has the value of $\dot{M}_\mathrm{max}=10^{-5.6}~M_\odot/yr$. Mass loss seems to have a negligible effect on instability of models immediately beyond TAMS, whereas this effect on the instability on the blue loops is much more pronounced. With the reduced mass a star reaches lower luminosity during helium burning phase and also a blue loop reaches lower effective temperature than for models calculated without mass loss. Both of these effects lead to smaller instability range during this phase of evolution. The description of wind which we used for lower effective temperatures (de Jager et al. (1988)) gives relatively low values of mass loss when compared to other models we checked (Nieuwenhuijzen & de Jager 1990, van Loon et al. 2005, Reimers 1975). It means that the instability areas on the blue loops calculated with other mass-loss models would be even smaller or entirely vanished. 