Indirect study of the C13(α,n)O16 reaction via the C13(Li7,t)O17 transfer reaction

Details Indirect study of the C13(α,n)O16 reaction via the C13(Li7,t)O17 transfer reaction Indirect study of the C13(α,n)O16 reaction via the C13(Li7,t)O17 transfer reaction

Apr 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008phrvc..77d2801p&link_type=abstract

Physical Review C, vol. 77, Issue 4, id. 042801

Astronomy and Astrophysics

Astrophysics

4

Transfer Reactions, Transfer Reactions, Hydrostatic Stellar Nucleosynthesis, 6<=A<=19

Scientific paper

The C13(α,n)O16 reaction is considered the main neutron source for the s process in low mass asymptotic giant branch (AGB) stars. In the Gamow peak, the cross section sensitively depends on the 1/2+ subthreshold state of O17 (Ex=6.356 MeV). In this work, we determined the astrophysical S factor through an evaluation of the α spectroscopic factor and the corresponding asymptotic normalization factor (ANC) of the 6.356 MeV state using the transfer reaction C13(Li7,t)O17 at two different incident energies. Our result confirms that the contribution of the 1/2+ state is dominant at astrophysical energies. Our reaction rate at T=0.09 GK is slightly lower than the value adopted in the Nuclear Astrophysics Compilation of REaction rates (NACRE), but two times larger than the one obtained in a recent ANC measurement.

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