Study of the nucleon radiative captures 8Li(n,γ)9Li, 9Be(p,γ)10B, 10Be(n,γ)11Be, 10B(p,γ)11C, and 16O(p,γ)17F at thermal and astrophysical energies

We have studied the neutron-capture reactions 8Li([Formula: see text]Li and its role in the primordial nucleosynthesis. The [Formula: see text] reaction has a significant astrophysical interest because it includes one of the variants of chain of primordial nucleosynthesis processes of the Universe and thermonuclear reactions in type II supernovae. Furthermore, we consider the [Formula: see text] reaction in the astrophysical energy range in the modified potential cluster model (MPCM) with splitting of orbital states according to Young tableaux and, in some cases, with forbidden states (FS). The reaction [Formula: see text] plays an important role in primordial and stellar nucleosynthesis of light elements in the [Formula: see text] shell. Hydrogen burning in second-generation stars occurs via the proton–proton (pp) chain and CNO cycle, with the [Formula: see text] reaction serving as an intermediate link between these cycles. Furthermore, the possibility of describing available experimental data for the total reaction cross-sections of neutron radiative capture on [Formula: see text]Be at thermal and astrophysical energies has been shown. This reaction is a part of one of the variants of the chain of primordial nucleosynthesis of the Universe due to which the elements with a mass of [Formula: see text] may be formed. The results in the field of study of thermonuclear proton-capture reaction on [Formula: see text] at ultralow, i.e., astrophysical energies will be presented further. The possibility of description of the experimental data for the astrophysical [Formula: see text]-factor of the proton radiative capture on [Formula: see text]O to the ground state (GS) of [Formula: see text]F was considered in the frame of the MPCM with FS and classification of the states according to Young tableaux. It was shown that on the basis of the [Formula: see text] transitions from the states of [Formula: see text]O scattering to the GS of [Formula: see text]F in the [Formula: see text]O channel generally succeed to explain the value of measured cross-sections at astrophysical energies.