Sources of uncertainties in the s-process in massive stars: convection and reaction rates

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dc.creatorCosta, V.
dc.creatorPumo, M. L.
dc.creatorBonanno, A.
dc.creatorZappala', R. A.
dc.date2008-05-23
dc.date.accessioned2026-07-07T09:40:38Z
dc.date.available2026-07-07T09:40:38Z
dc.descriptionCurrent models of s-nucleosynthesis in massive stars ($M\sim15 M_{\odot}$ to $\sim 30 M_{\odot}$) are able to reproduce some main features of the abundance distributions of heavy isotopes in the solar system, at least in the $A\sim 60-90$ mass range. The efficiency of the process and the above specified mass range for the s-nuclei are still heavily uncertain due to both nuclear reaction rates and stellar models uncertainties. A series of s-process simulations with stellar models in the $15-30 M_{\odot}$ (mass at ZAMS) and metallicity $Z=0.02$ mass have been performed to analyse the impact of the overshooting model used on the s-process yields. As in a previous exploratory work performed with stellar models having $M_{ZAMS}=25 M_{\odot}$ and $Z=0.02$, enhancements factors in the range 2-5 are found in the final s-process efficiency when overshooting is inserted in the models.
dc.description4 pages, 2 figures, Proceedings of the ''Catania workshop on nuclear and neutrino astrophysics''
dc.identifierhttps://arxiv.org/abs/0805.3607
dc.identifierhttp://arxiv.org/abs/0805.3607
dc.identifierINAF- Catania Astrophysical Observatory Special Publications, 2008, 1, 97
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/161545
dc.subjectAstrophysics
dc.titleSources of uncertainties in the s-process in massive stars: convection and reaction rates
dc.typetext

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