Measurement of the reaction 180(α,n)21Ne.

Background: The reaction 180(α,n)21Ne is a part of the reaction chains leading to the production of 19F and 22Ne during He burning in low-mass and massive AGB stars, respectively. Additionally, it has been observed as a strong background source in the measurement of other (α,n) reactions. Purpose: Previously low-energy 180(α,n)21Ne cross section data have only been available in a non-peer-reviewed form. An improved measurement of this reaction has been done to both clarify its astrophysical influence as well as to provide background yield data for future (α,n) experiments. Method: The 180(α,n(0+1)) reaction has been measured with a moderating neutron detector. In addition the (α,n1γ) channel has been measured independently by observation of the characteristic 350.7 keV γ transition in 21Ne. The reaction cross section at energies above Eα = 1100 keV was determined by a simultaneous R-matrix fit to both channels. The strengths of the two lowest-energy resonances at Eα = 959 keV and Eα = 1066 keV were analyzed separately using individual Breit-Wigner fits. Results: The cross section of both reaction channels, 180(α; n0)21Ne and 180(α,n1γ)21Ne, was determined from the threshold energies at 851 keV and 1280 keV, respectively, to 2300 keV. A new reaction rate has been deduced for the temperature range of 0.1 GK to 10 GK. A previously reported resonance at Eα = 888 keV is explained as background from the contaminant.reaction 17O(α,n)20Ne. Conclusions: In general, our reaction rate is slightly lower than the reaction rates in recent compilations. At temperatures below 0.2 GK the present rate is significantly lower because it could be shown that the lowest reported resonance is background from the reaction 17O(α,n)20Ne that has been wrongly assigned to 18O(α,n)21Ne. [ABSTRACT FROM AUTHOR]