The total cross-sections of the radiative neutron capture processes on 9 Be, 14 C, 14 N, 15 N and 16 O are described in the framework of the modified potential cluster model with the classification of orbital states according to Young tableaux. The continued interest in the study of these reactions is due, on the one hand, to the important role played by this process in the analysis of many fundamental properties of nuclei and nuclear reactions, and, on the other hand, to the wide use of the capture cross-section data in the various applications of nuclear physics and nuclear astrophysics, and, also, to the importance of the analysis of primordial nucleosynthesis in the Universe. This article is devoted to the description of results for the processes of the radiative neutron capture on certain light atomic nuclei at thermal and astrophysical energies. The considered capture reactions are not part of stellar thermonuclear cycles, but involve in the reaction chains of inhomogeneous Big Bang models.Keywords: Nuclear astrophysics; primordial nucleosynthesis; light atomic nuclei; low and astrophysical energies; phase shift analysis of the n 16 O scattering; radiative capture; total cross-section; thermonuclear processes; potential cluster model; forbidden states. PACSNumber(s): 21.60.Gx, 25.20.Lj, 25.40.Lw, 26.20.Np, 26.35.+c, 26.50.+x, 26.90.+n, 98.80.Ft 1350075-1 Int. J. Mod. Phys. E 2013.22. Downloaded from www.worldscientific.com by STOCKHOLM UNIVERSITY on 08/14/15. For personal use only. 1350075-2 Int. J. Mod. Phys. E 2013.22. Downloaded from www.worldscientific.com by STOCKHOLM UNIVERSITY on 08/14/15. For personal use only. 1350075-4 Int. J. Mod. Phys. E 2013.22. Downloaded from www.worldscientific.com by STOCKHOLM UNIVERSITY on 08/14/15. For personal use only. Radiative Neutron Capture on 9 Be, 14 C, 14 N , 15 N and 16 O Model and Calculation MethodsThe expressions for the total radiative capture cross-sections σ(NJ , J f ) in the PCM are given, for example, in Refs. 29 and 30 are written aswhere for the electric orbital EJ(L) transitions (S i = S f = S) we have 29 :

Calculations of the reaction rate of the proton radiative capture on 3 H at temperatures from 0.01 Т 9 up to 5 Т 9 , which are based on the theoretical results for the astrophysical S-factor and take into account the latest experimental data, were carried out. Theoretical results for the S-factor at energies from 1 keV up to 5 MeV were obtained in the framework of the modified potential cluster model with the classification of orbital states according to Young tableaux. On the basis of used nuclear model of the interaction of p and 3 H particles there was shown possibility of description the latest experimental data for the S-factor at the energy range from 50 keV up to 5 MeV. Numbers: 21.60.Gx, 25.40.Lx, 26.35.+c, 26. Reaction No.12 proceeds with comparatively low probability, since the E1 process is forbidden by the isospin selection rules. This leads to the factor   J J J

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Abstract. The systematization of cluster analogies for nuclei with A=6, 7, 9 is given. The isobar