Radiative Capture of Neutrons on 12C at Astrophysical Energies

Abstract

The total cross sections of the 16 O(n, γ) 17 O radiative capture process is described in the framework of the modified potential cluster model with the classification of orbital states according to Young tableaux. The possibility to describe the experimental data for the total cross sections of the neutron radiative capture on 16 O at the energies from 0.025 eV to 1.5 MeV is shown on the basis of E1 and M1 processes. The transitions to the bound states of 17 O in the n 16 O channel from 2 S 1/2 , 2 Р 3/2 and 2 D 3/2 waves of the n 16 O scattering have been considered. These transitions have been considered in the resonance energy region at 433 and 1000 keV.PACS numbers: 21.60. Gx, 25.40.Lw, 26.20.Np, 26.35.+c, 26.50.+x, 26.90.+n, 98.90Here, m is mass of the nucleus,  1 ,  2 are the magnetic moments of clusters and the remaining symbols are the same as in the previous expression. The value of

ASTROPHYSICAL S-FACTOR AND REACTION RATE OF THE RADIATIVE 3 H(p,) 4 He CAPTURE

“…Earlier in our works [13,[35][36][37][40][41][42] the possibility of description of astrophysical S-factors or total cross-sections of the radioactive capture for three dozens of processes on the basis of two-body potential cluster model (PCM) was shown and also the preliminary results [43] for p 3 H-capture at astrophysical energies have been obtained. The calculations of these reactions are carried out on the basis of the modified variant of PCM with forbidden states (FSs) [44] and classification of states according to Young tableaux (MPCM).…”

“…For instance, these can be the astrophysical S-factors of the radiative capture reactions [46] or the total cross sections of these reactions [47]. Including radiative capture cross sections at the astrophysical and thermal energy range which has been considered in our previous papers [13,[35][36][37][40][41][42]. On the basis of such conception we succeeded in the correct description of the total cross sections of the radiative capture processes of almost thirty reactions for light nuclei at thermal and astrophysical energies [13,[35][36][37][40][41][42].…”

“…Therefore, continuing studying the thermonuclear reactions [13,[35][36][37][40][41][42] on the basis of the MPCM [13,35] with separation of orbital states according to Young tableaux let us consider description of the astrophysical S-factor of the radiative proton capture on 3 H at energies of 1 keV-10 MeV and rate of this reaction from T 9 = 0.05 to T 9 = 2. Preliminary results on S-factor of this reaction at astrophysical energies in the frame of the MPCM were given in our previous work [43].…”

“…All of this directly applies to the detailed study of the 3 H(p,γ) 4 He capture reaction in the astrophysical energy region on the basis of the modern nuclear model. This model, as shown below, has already demonstrated its efficiency in the description of the characteristics of almost 30 such reactions [13,[35][36][37][38][39][40][41].…”