Abstract
The 12C(p,γ) and 13C(p,γ) reaction cross sections are currently under investigation in the low-background environment of the Laboratory for Underground Nuclear Astrophysics. Both reactions are being studied using different types of solid targets, and employing complementary detection techniques (HPGe spectroscopy, total absorption spectroscopy and activation counting). To reduce systematic uncertainties, targets must be accurately characterized and their degradation monitored under the intense (~ 400 µA) beam of the LUNA400 accelerator. We present the experimental techniques employed, and the analyses developed for the study of these reactions.
Highlights
Targets must be accurately characterized and their degradation monitored under the intense (∼ 400 μA) beam of the LUNA400 accelerator
The data start to differ up to 20%
The reactions 12C(p, γ)13N and 13C(p, γ)14N are the first two of the CNO cycle, which is active in the hydrogen burning regions of main sequence, Red Giant Branch (RGB) and Asymptotic Giant Branch stars (AGB)
Summary
The reactions 12C(p, γ)13N and 13C(p, γ)14N are the first two of the CNO cycle, which is active in the hydrogen burning regions of main sequence, Red Giant Branch (RGB) and Asymptotic Giant Branch stars (AGB). This contributes to the energy production, by converting four protons into one helium nucleus, and governs the abundances of several elements. Since the predictions depend on nuclear reaction rates, it is of particular interest to constrain the latter as much as possible This can help to study the mixing phenomena in more detail and to constrain theoretical models. The results are affected by large scattering and the statistical uncertainty ranges from 15% to 40%
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