α-capture on ^18O and its astrophysical implications

Details α-capture on ^18O and its astrophysical implications α-capture on ^18O and its astrophysical implications

Oct 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aps..haw.sb006g&link_type=abstract

American Physical Society, First Joint Meeting of the Nuclear Physicists of the American and Japanese Physical Societies October

Physics

Scientific paper

The ^22Ne(α,n) reaction is the dominant neutron source for the weak s-process in massive stars and plays also a significant role in the s-process nucleosynthesis in AGB stars. ^22Ne is produced by the reactions sequence ^14N(α,γ)^18F(β^+) ^18O(α,γ)^22Ne. While the α-capture on ^14N is well understood, considerable uncertainties exist for the ^18O(α,γ)-reaction. The reaction rate is dominated by two resonances at α-energies of 470 keV and 566 keV at the temperatures of interest. These two resonances have not been observed directly and the rates are based on estimates for the resonance strength. We have searched for these resonances using an intense α-beam and a Ge-clover detector in combination with BGO detectors. The first results of this experiment will be reported and the implications for the neutron production will be discussed.

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