Evolution of A 30 M⊙ Star: The Interplay of Nuclear Burning and Mass Loss
Evolutionary tracks for a 30 M⊙ star with various mass loss rates (MLR) were evolved to core He exhaustion. The “overluminosity” of mass losing (ML) stars is explained in terms of the well known mass-luminosity (M-L) law. A critical ZAMS MLR above which mass loss leads to evolution to fainter luminosities is derived. Two tracks showed reversals in their direction of evolution across the HR diagram. These have been shown to be a consequence of mass loss dominating over the effects of the shell source. An analytic criterion for this condition has been derived.
KeywordsMass Loss Mass Loss Rate Stellar Evolution Evolutionary Track Convective Core
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