Neutron cross sections --- clues for s-process nucleosynthesis

Details Neutron cross sections --- clues for s-process nucleosynthesis Neutron cross sections --- clues for s-process nucleosynthesis

Sep 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aspc..336..255k&link_type=abstract

Cosmic Abundances as Records of Stellar Evolution and Nucleosynthesis in honor of David L. Lambert, ASP Conference Series, Vol.

Physics

Nuclear Physics

Scientific paper

The slow neutron capture process, which is responsible for about half of the elemental abundances between Fe and Bi, is of utmost interest for stellar evolution models, since the abundance patterns reflect the physical conditions at the stellar site. These abundances are essentially determined by the respective neutron capture cross sections, which are accessible by laboratory experiments. Correspondingly, the s-process provides a unique window to the stellar interior. The status of the relevant nuclear physics data for quantitative analyses, the available experimental techniques and facilities as well as the remaining experimental quests are briefly outlined. The potential of s-process analyses for testing current models of He burning in low mass AGB stars is illustrated at the example of the branching at A=127/128.

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