Аңдатпа
Abstract The study of the 3H(1H, γ)4He reaction is of relevance for both nuclear physics and nuclear astrophysics. In nuclear astrophysics, more accurate data should be obtained on the rate of primordial nucleosynthesis reactions that lead to the production of 4He. In nuclear physics, there are theoretical models in which the behavior of the cross section and the S-factor of this reaction in the energy range of the order of tens of keV are in poor agreement with experiment. Thereby, more accurate experimental study of S-factor behavior should be performed in the astrophysical energy range. The experimentally obtained values of the yields for various energies of 1H+ ions were used to describe the behavior of the 3H(1H, γ)4He reaction S-factor depending on the energy. As a result, the accuracy of determination of the S-factor of the 3H(1H, γ)4He reaction has been improved several times.