Abstract
We report on our latest experimental study of the 2H(ρ,γ)3He reaction in the energy range of interest for big-bang nucleosynthesis. The differential cross section at 135° and γ)-ray angular distributions were measured and compared with the results deduced from the latest ab-initio calculation. The astrophysical S-factor for the 2H(ρ,γ)3He reaction was obtained in the center-of-mass energy range E = 97-210 keV, and it is found to be in reasonable agreement with that predicted by the ab-initio calculation.
Highlights
The 2 H(p,γ)3 He radiative capture reaction has a major role in big-bang nucleosynthesis (BBN)
There are only a few data points reported for the energy range of 30–300 keV [4,5,6,7,8], relevant for BBN, which seem to be in a disagreement with the latest ab-initio calculation of Marcucci et al [9]
Quantitative deuterium depth profiling [10] has shown that one of the targets had an effective thickness of 1.6 μm and was considered to be thick, while the other one had a thickness of nm
Summary
The 2 H(p,γ)3 He radiative capture reaction has a major role in big-bang nucleosynthesis (BBN). The uncertainty in this reaction rate has a strong impact on primordial abundances of 2 H, 3 He and 7 Li. In order to determine the reaction rate and its associated uncertainty, one requires the astrophysical S-factor, which is deduced either from the measured data or a nuclear reaction model. The latest BBN calculation of Coc et al [1] predicts the primordial deuterium to hydrogen ratio of 2 H/H = (2.45±0.10)×10−5 .
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