Constraints on the 22Ne(α, n)25Mg Reaction Rate from natMg+n Total and 25Mg(n, γ) Cross Sections

Details Constraints on the 22Ne(α, n)25Mg Reaction Rate from natMg+n Total and 25Mg(n, γ) Cross Sections Constraints on the 22Ne(α, n)25Mg Reaction Rate from natMg+n Total and 25Mg(n, γ) Cross Sections

Jun 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003cgrs.conf..318k&link_type=abstract

CAPTURE GAMMA-RAY SPECTROSCOPY AND RELATED TOPICS. Proceedings of the Eleventh International Symposium. Held 2-6 September 2002

Physics

Scientific paper

The 22Ne(α, n)25Mg reaction is the neutron source during the s process in massive and intermediate mass stars as well as a secondary neutron source during the s process in low mass stars. Therefore, an accurate determination of this rate is important for a better understanding of the origin of nuclides heavier than iron as well as for improving s-process models. Also, because the s process produces seed nuclides for a later p process in massive stars, an accurate value for this rate is important for a better understanding of the p process. Because the lowest observed resonance in direct 22Ne(α, n)25Mg measurements is considerably above the most important energy range for s-process temperatures, the uncertainty in this rate is dominated by the poorly known properties of states in 26Mg between this resonance and threshold. Neutron measurements can observe these states with much better sensitivity and determine their parameters much more accurately than direct 22Ne(α, n)25Mg measurements. I have analyzed previously reported natMg+n total and 25Mg(n, γ) cross sections to obtain a much improved set of resonance parameters for states in 26Mg in this region, and an improved estimate of the uncertainty in the 22Ne(α, n)25Mg reaction rate.

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