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Scientific paper
May 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aipc..769.1350h&link_type=abstract
INTERNATIONAL CONFERENCE ON NUCLEAR DATA FOR SCIENCE AND TECHNOLOGY. AIP Conference Proceedings, Volume 769, pp. 1350-1355 (200
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Nucleosynthesis In Novae, Supernovae, And Other Explosive Environments, Stellar Structure, Interiors, Evolution, Nucleosynthesis, Ages, 3H-, 3He-, And 4He-Induced Reactions
Scientific paper
The last decades have seen an enormous progress in modeling astrophysical objects, which lead to a significantly improved understanding of various nucleosynthesis scenarios. This applies in particular for asymptotic giant branch (AGB) stars where about half of the heavy elements are synthesised by the main component of the s process. In order to test these models and to compare the model predictions with observational data accurate neutron capture cross sections of isotopes with mass numbers A > 90 are indispensable. This holds especially for nuclei near closed neutron shells and in the vicinity of branch points since the analysis of s-process branchings yields important information on stellar parameters like temperature, neutron density, mass density and even convection time scales during the s process. Within this picture neutron reactions on abundant light elements are also important since these act as neutron poisons, hence affecting the neutron balance in the star. Finally, also the most important neutron sources for the s process, 13C(α,n)16O and 22Ne(α,n)25Mg, will be discussed.
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