Sources of uncertainties in the s-process in massive stars: convection and reaction rates
http://www.arxiv.org/abs/0805.3607V. Costa, M.L. Pumo, A. Bonanno, R.A. Zappala'
4 pages, 2 figures, Proceedings of the ''Catania workshop on nuclear and neutrino astrophysics''
Current 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.
Located at http://www.arxiv.org/abs/0805.3607
