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

Radiative capture p + N-13 -> O-14 + gamma 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 N-13 are higher than the beta decay rates of N-13. The hot CNO cycle initiates at stellar temperature T >= 0.11 x10(9) K. Within the frame work of potential model, we calculate the nuclear reaction rates and astrophysical S-factor for the reaction N-13(p, gamma)O-14. It is to be noted that the nuclear cross-section is calculated for the first resonance of p-N-13 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

Automated summary

The radiative capture process p + N-13 -> O-14 + gamma is crucial in the hot CNO cycle at stellar temperatures above 0.11 x10(9) K. Calculations of nuclear reaction rates and astrophysical S-factor for the N-13(p, gamma)O-14 reaction are done within the framework of potential model. The study focuses on the first resonance of the p-N-13 system within a proton energy range of (0-1) MeV where E1 transition dominates, with results showing good agreement with existing data.