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The  3 He(α,γ) 7 Be reaction plays an important role in two astrophysical scenarios. It is a key reaction in lithium production during the Big Bang Nucleosynthesis and one of the central reaction in the p-p chain in stars. In the case of the former event, the Gamow energy of the reaction is around 0.2 MeV, while in the case of the p-p chain in the Sun, an order of magnitude less, around 0.023 MeV. Experimental investigation at such low energies is very difficult, if possible at all, thus low energy extrapolation inevitable to predict the reaction rate at these energies. The extrapolation and its uncertainty are inuenced by the precision and covered energy range of the data used. There are many precision datasets between E  c.m.   = 0.3–3.1 MeV, but only one below and one above. At higher energies known levels of  7 Be exist, which motivates the study of that energy range. Therefore, we performed investigations in the energy range of E  c.m.   = 4.3–8.3 MeV, where the radiative cross section has not been studied so far. For the cross section determination, the activation technique was used utilising a thin-windowed gas cell and the MGC-20 cyclotron of ATOMKI.

3He(α,γ)7Be cross section measurement around 7Be known energy levels

³He(α,γ)⁷Be cross section measurement around ⁷Be known energy levels