Reaction rate of radiative capture of proton by 11B nucleus

The B-11(p,gamma)C-12 reaction is of considerable interest in the field of controlled thermonuclear fusion and in nuclear astrophysics. In thermonuclear reactors, structural elements containing boron can be used as neutron absorbers. This reaction is one of the reactions of B-11 production in the stars (sic). The rate of the B-11(p,gamma)C-12 reaction (occurring in the interiors of first-generation stars) can be of great importance for the amount of B-11 and B-10 observed today in the Earth's crust and in the interstellar medium. Therefore, in this work, within the framework of a modified potential cluster model with a classification of orbital states according to Young's diagrams and taking into account allowed and forbidden states, we examined the possibility of describing the available experimental data for the total cross sections of the radiative p(11)B capture to the ground state of the C-12 nucleus at energies up to 1.5 MeV. It is shown that only on the basis of E1 and M1 transitions from the p(11)B scattering states, taking into account the first resonance for the ground state of the C-12 nucleus, it is quite possible to explain the magnitude and shape of the experimental astrophysical S-factor. The work presents comparisons the astrophysical S-factors of the radiative p(11)B capture to the ground state of the C-12 nucleus found by us with the experimental data available in the literature. Based on the obtained theoretical S-factor, the rate of this reaction was calculated in the temperature range from 0.01 to 1 T-9. The calculated results for rates are approximated by a simple expression, which simplifies their use in applied thermonuclear and astrophysical research.