Reaction rate of radiative p14C capture in the region from 0.01 to 10 T9

Abstract

The ¹⁴C(p,γ)¹⁵N reaction is of considerable interest in nuclear astrophysics. This reaction is one of the reactions of ¹⁵N production in the stars. The rate of the ¹⁴C(p,γ)¹⁵N reaction plays an important role in the formation of nuclei with an atomic mass of more than 14. Currently, this reaction at low energies has not been studied well enough, both experimentally and theoretically. 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 p¹⁴C capture to the ground state of the ¹⁵N nucleus. The calculations carried out take into account the wide resonance at 1.4 MeV in c.m. and performed at energies up to 5 MeV. It is shown that only on the basis of the E1 transition from the p¹⁴C scattering state, it is quite possible to explain the magnitude and shape of the experimental astrophysical S-factor. The work presents comparisons of the astrophysical S-factors of the radiative p¹⁴C capture to the ground state of the ¹⁵N nucleus found by us with the experimental data available in the literature. Based on the obtained total cross sections, the rate of this reaction was calculated in the temperature range from 0.01 to 10.0 T₉. The calculated results for rates are approximated by a simple expression, which simplifies their use in applied thermonuclear and astrophysical research.