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Instabilities in Very Massive Stars
Published online by Cambridge University Press: 12 April 2016
Abstract
Detailed dynamical models and nucleosynthesis yields of very massive stars from early pre-MS through very late stages have been computed. The recent reduction of mass loss rates for the WR stages can have important consequences for both the evolution, surface composition and stability. Depending on mass and metallicity, in the present models instabilities occur during the accretion phase (pre-ZAMS), LBV stage and very late stages (WC).
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- Part 5. Theoretical Models of Classical Pulsating Stars
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- Copyright © Astronomical Society of the Pacific 2000