Radiative n 14N capture at astrophysical energies

Abstract

The versions of intercluster interaction potentials describing the resonance nature of some phase shifts of the n 7 Li elastic scattering at low energies and the P 2 ground state of 8 Li in the n 7 Li cluster channel have been constructed. The possibility of describing the total cross sections of 7 Li(n, ) 8 Li within the energies from 5 meV (510 -3 eV) to 1 MeV, including resonance at 0.25 MeV, has been demonstrated for the potentials obtained in the potential cluster model with forbidden states.

Radiative Proton Capture on 3 H at Astrophysical Energies and Its Role in the Initial Stage of Star Formation

“…Known results on extraction of the asymptotic constant from experimental data give a value of 5.16 (13) for p 3 H channel [37]. For the asymptotic constant of n 3 He system in [37], a value of 5.10 (38) has been obtained that is very close to the constant of p 3 H channel for our GS potential from Table 3.…”

“…Earlier in our works [11][12][13][14][15][16] the possibility of description of astrophysical S-factors or total crosssections 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 [17] 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) [18] and classification of states according to Young tableaux (MPCM).…”

“…For instance, these can be the astrophysical S-factors of the radiative capture reactions [20] or the total cross sections of these reactions [21]. Including radiative capture cross sections at the astrophysical and thermal energy range which has been considered in our previous papers [11][12][13][14][15][16]. 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 [11][12][13][14][15][16].…”

“…Therefore, continuing studying the thermonuclear reactions [11][12][13][14][15][16] on the basis of the MPCM [16] 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 [17].…”

Radiative n 10B Capture at Thermal and Astrophysical Energies

“…Before proceeding to the total cross-sections analysis of the 15 N(n, ) 16 N capture reaction, let us note that the classification of orbital states of 15 N according to Young tableaux was qualitatively considered by us in works. 7,85 So for the n 15 N system we have {1}  {4443}  {5443} + {4444}. 46 The first of the obtained tableaux is compatible with the orbital moments L = 1, 3 and is forbidden as it has 5 boxes in the first row, 46 and the second one is allowed and compatible with the orbital moments L = 0 and 2.…”