Stellar cross sections for 33S(n,α)30Si, 36Cl(n,p)36S, and 36Cl(n,α)33P and the origin of 36S

Details Stellar cross sections for 33S(n,α)30Si, 36Cl(n,p)36S, and 36Cl(n,α)33P and the origin of 36S Stellar cross sections for 33S(n,α)30Si, 36Cl(n,p)36S, and 36Cl(n,α)33P and the origin of 36S

Jan 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995phrvc..51..379s&link_type=abstract

Physical Review C (Nuclear Physics), Volume 51, Issue 1, January 1995, pp.379-391

Physics

Nuclear Physics

22

Resonance Reactions, Stellar Structure, Interiors, Evolution, Nucleosynthesis, Ages, 20<=A<=38, Gas-Filled Counters: Ionization Chambers, Proportional, And Avalanche Counters

Scientific paper

The cross section of the 33S(n,α)30Si reaction was measured in a neutron energy spectrum yielding the stellar rate for a thermal energy of kT=25 keV. For the 36Cl(n,p)36S reaction, the experiment was performed in the neutron energy range from 10 to 260 keV. Our new result for 33S resolves the problem of a large discrepancy between two previous experiments. In case of 36Cl it could be shown that the (n,α) channel is negligibly small compared to the (n,p) reaction at s-process conditions. The present results are used for a detailed discussion of a possble s-process origin of the rare neutron-rich isotope 36S.

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