[en] Numerical results of stellar evolution affected by the mass loss are presented. Initial masses of stars are in the range 40-120 Msub(solar). The mass loss rate is defined in the way that approximates observational data obtained by Hutchings (1976). For comparison evolutionary sequences with the above mass loss rate multiplied by factors: 2, 5, and 10, as well as with the rate defined by Lamers et al. (1976) are also presented. An analytical formula for the mass loss rate which approximates Hutchings' data is derived. Influence of the mass loss on the shape of the upper main sequence is discussed. (Author)