Lecture 19 Pair Instability Supernovae and Population III
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Lecture 19 Pair Instability Supernovae and Population III. Mass Loss in Very Massive Primordial Stars. Negligible line-driven winds (mass loss ~ metallicity 1/2 ) (Kudritzki 2002) No opacity-driven pulsations (no metals ) Continuum-driven winds likely small contribution - PowerPoint PPT Presentation
Transcript of Lecture 19 Pair Instability Supernovae and Population III
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Lecture 19
Pair Instability SupernovaeandPopulation III
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Mass Loss in Very Massive Primordial StarsNegligible line-driven winds (mass loss ~ metallicity1/2) (Kudritzki 2002)No opacity-driven pulsations (no metals)Continuum-driven winds likely small contributionEpsilon mechanism inefficient in metal-free stars below ~1000 M (Baraffe, Heger & Woosley 2000) from pulsational analysis we estimate upper limits:120solar masses:
