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Instabilities in LBVs and WR Stars
Published online by Cambridge University Press: 12 April 2016
Abstract
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Using a dynamical stellar code, detailed evolutionary models have been computed that follow the evolution and nucleosynthesis of massive stars from the pre-MS (accretion phase) up to the onset of O-burning. Various instabilities occur during the evolution. As an example, the evolution of a star with maximum mass 120 Mʘ is discussed.
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- Section V Pulsation
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- Copyright © Springer-Verlag 1999
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