Evolution of a 30 M mass of the Sun star with mass loss

Five tracks for a 30 Msun star with mass loss given by the algorithm dM/dt = - kLR/M have been computed to core He exhaustion with initial ZAMS rates of (0.0, 1.0, 2.5, 5.0, 10.0) x 10-7.Msun.yr-1. The main-sequence phase has been described in an earlier paper and the present paper continues the detailed comparison of the tracks and the internal structure of the evolving stars to clarify further the effects of mass loss on stellar evolution. Two of the sequences showed reversals in their direction of evolution across the HR diagram. These reversals have been demonstrated to occur when mass loss dominates over the effects of the shell source. The highest mass loss rate track reached the giant branch before burning any He, while the next highest rate produced a star which spent, due to a reversal, the major portion of the He burning as a hot blue supergiant and a WR type star. It is shown that the mass-luminosity law can be used to explain features of the evolution and internal structure such as the changes of stellar luminosity, He core luminosity and He burning age with central He abundance. The sizes and positions of the convective shell are also discussed. (author)