The effects of the mass loss on the internal structure and the evolution of a medium-size star (7 solar masses) from the main sequence to the late stage of the evolution are investigated using Waldron's (1984) empirical relation and a newly derived formula to calculate the mass loss rates of the star throughout the HR diagram. It is shown that, in the main sequence phase, the behavior of a star of this magnitude is different from that of a massive star with significant mass loss, in that there exist nearly no differences with respect to the masses of the H burning core and the masses of the convective core.
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