Abstract
New computations of He shell nucleosynthesis occurring during both radiative and convective phases are presented for stars in the range 8 – 25 M⊙, taking in account the recent changes proposed for many cross sections. While the internal zones, swept by the radiative shell, are shown to efficiently produce elements up to A = 70‒80 only in the most massive stellar models, the intermediate convective regions can be an important source for elements like 12C, 18O, 22Ne and Mg isotopes.
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© 1987 D. Reidel Publishing Company
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Busso, M., Gallino, R., Picchio, G. (1987). Nucleosynthesis by 14N Depletion during Shell He Burning in Massive Stars. In: Kwok, S., Pottasch, S.R. (eds) Late Stages of Stellar Evolution. Astrophysics and Space Science Library, vol 132. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-3813-7_37
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DOI: https://doi.org/10.1007/978-94-009-3813-7_37
Publisher Name: Springer, Dordrecht
Print ISBN: 978-94-010-8196-2
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