Abstract
The determination of the involved reaction cross sections is essential for the understanding of how the big bang nucleosynthesis and nuclear reactions in stars contribute to the observed abundances. One of those, which has not been measured so far, is the 10Be(n,<i>γ<i>) cross section.A 10BeO sample, provided by PSI Villigen, was irradiated in a cyclic activation at the TRIGA reactor in Mainz. The characteristic <i>γ<i>-rays following the decay of 11Be were measured using LaBr3 scintillation detectors. The thermal neutron cross section and the resonance integral were experimentally determined for the first time.
Highlights
The pattern of the solar abundances of nuclides features a conspicuous minimum in the region of the light elements Li, Be, and B
Far the recommended capture cross sections are based on theoretical direct capture calculations and inverse reactions [1, 2, 3], as shown in figure 1, or the asymptotic normalization coefficient (ANC) of the wavefunction [4]
A layer of 1 mm cadmium was wrapped around the sample during some of the activations to determine the contribution by the non-thermal high energy tail of the neutron spectrum, using the energy dependent neutron transmission of cadmium, as shown in figure 2
Summary
The pattern of the solar abundances of nuclides features a conspicuous minimum in the region of the light elements Li, Be, and B. The understanding of the 10Be(n,γ) cross section is crucial for the modelling of the reaction rates of the light nuclei, which directly affect the abundances. Far the recommended capture cross sections are based on theoretical direct capture calculations and inverse reactions [1, 2, 3], as shown, or the asymptotic normalization coefficient (ANC) of the wavefunction [4]. The latter being used in a recent publication by S.
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