Physics
Scientific paper
Apr 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aps..apr.h4002h&link_type=abstract
American Physical Society, April Meeting, April 28 - May 1, 2001 Washington, DC Bulletin of the American Physical Society, Vol.
Physics
Scientific paper
Stars of more than about eight solar masses are the main source of heavy elements in the universe. In the recent years significant progress has been made in modeling the evolution of these stars and their nucleosynthesis. In this talk we will discuss current stellar evolution calculations that include all burning phases in massive stars till the onset of core collapse and through the supernova explosion. These calculations follow the nucleosynthesis of thousands of isotopes up to bismuth. We will also review the uncertainties of crucial nuclear reaction rates in stellar evolution that affect these results, particularly C^12(α,γ)^16O and Ne^22(α,n)^25Mg. The latter is the key reaction responsible for most of the s-process in massive stars. The former affects yields of all major elements, and also influences the pre-supernova structure. We will show results from calculations using the most recent weak rates and how they affect the structure of the iron core prior to core collapse. As time allows, we will also discuss the evolution and nucleosynthesis peculiarities of the first generation of stars, as they might have been considerably more massive and have produced a unique nucleosynthesis pattern.
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