Physics
Scientific paper
Aug 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003phrvc..68b5801d&link_type=abstract
Physical Review C, vol. 68, Issue 2, id. 025801
Physics
14
Resonance Reactions, Radiative Capture, Hydrostatic Stellar Nucleosynthesis, X- And Gamma-Ray Spectroscopy
Scientific paper
The 22Ne(α,n) reaction is the main neutron source for neutron capture nucleosynthesis (s process) in massive stars and plays also a significant role for the s process in thermally pulsing asymptotic giant branch stars. In these scenarios, 22Ne is produced by the reaction sequence 14N(α,γ)18F(β+)18O(α,γ)22Ne. While the first reaction is well understood, α capture on 18O was affected by considerable uncertainties. At the temperatures of stellar He burning, the reaction rate is determined by two resonances at α energies of 470 and 566 keV. Since these resonances were not yet successfully measured, the rates had to be based on estimated resonance strengths. In the present work, the first direct measurement of the partial strengths of these extremely weak low-energy resonances is reported. The use of a high-efficiency segmented Ge detector in coincidence with bismuth germanate oxide counters covering a large solid angle led to a significantly improved experimental sensitivity, thus allowing for the clear identification of specific γ transitions. As a result, resonance strengths of 0.71±0.17 μeV and 0.48±0.16 μeV could be obtained for the 566- and 470-keV resonances, respectively. When compared to the previously reported upper limits of ⩽1.7 μeV, these results provide a reliable basis for the determination of the reaction rate during stellar He burning. Accordingly, these data reduce the uncertainties in the s process neutron balance.
Dababneh Saed
Görres Joachim
Heil Matthias
Käppeler Franz
Leiste Harald
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