models of stellar winds give the mass loss rates in the form of power-law in luminosity with various exponents and they usually also depend on other stellar parameters. Let us note that unlike the Reimers’ formula (\[Reimers\]) corresponding to the stellar winds of late-type stars, which for chosen $M$ gives the $\dot{M}$ proportional to $R$ increasing for orders of magnitude for stars evolving from the main sequence to the red-giant branch, our approximation (\[MLR\]) intended to an unspecified mass loss mechanism varies linearly with $L$ only, i.e. much less in the course of evolution of the star.

It can be expected that the mass loss rate is more complicated in reality, however, to get an insight into its possible effects on the stellar evolution before a proper model of the mass loss mechanism will be available we are limited to the use of such an [*ad hoc*]{} assumption. In our parametrization, the mass loss parameter $N=100$ gives for the luminosity $L\sim 10^{6}L_{\odot}$ typical for stars with mass of the order $100\,M_{\odot}$ a mass loss rate of $\dot{M}\sim 10^{-5} M_{\odot}$yr$^{-1}$ which is able to reduce significantly the initial mass of the star during its characteristic life-time $\tau\sim 10^{6}$yr. Calculations with different 