Re-examination of proton capture 13N(p, γ)14O in stellar matter

Abstract

Abstract Radiative capture p + 13N → 14O + γ at energies bearing astrophysical importance is one of the key processes in the hot CNO cycle. The transition from normal CNO to hot CNO takes place when the proton capture rates on 13N are higher than the β decay rates of 13N. The hot CNO cycle initiates at stellar temperature T ≥ 0.11 ×109 K. Within the frame work of potential model, we calculate the nuclear reaction rates and astrophysical S-factor for the reaction 13N(p, γ)14O. It is to be noted that the nuclear cross-section is calculated for the first resonance of p–13N system within the proton energy range (0–1) MeV, where the E1 transition plays a dominant role. Our calculated radiative capture rates are in nice comparison with the existing data. Based on the radiative capture rates we further estimate the temperature at which the normal CNO turns into a hot CNO cycle