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The 10B(p,{\gamma})11C reaction is of significant interest in nuclear astrophysics and in the field of controlled thermonuclear fusion. This reaction is one of the reactions of 11B production, which is carried out through the 10B(p,{\gamma})11C(\b{eta}+{\nu})11B chain. The rate of the 10B(p,{\gamma})11C reaction (occurring in the interiors of first-generation stars) can be of great importance for the amount of 10B and 11B observed today in the interstellar medium and in the Earth's crust. In thermonuclear reactors, structural elements containing boron can be used as neutron absorbers, etc. Therefore, in this work, within the framework of a modified potential cluster model with a classification of orbital states according to Young's diagrams and taking into account allowed and forbidden states, we examined the possibility of describing the available experimental data for the total cross sections of the radiative p10B capture to the ground state of the 11C nucleus at energies up to 1 MeV. It is shown that only on the basis of E1 and M1 transitions from the p10B scattering states, taking into account the first resonance for the ground state of the 11C nucleus, it is quite possible to explain the magnitude and shape of the experimental astrophysical S-factor. The work presents comparisons the astrophysical S-factors of the radiative p10B capture to the ground state of the 11C nucleus found by us with the experimental data available in the literature. Based on the obtained theoretical S-factor, the rate of this reaction was calculated in the temperature range from 0.01 to 1 T9. The calculated results for rates are approximated by a simple expression, which simplifies their use in applied thermonuclear and astrophysical research., Comment: 10 P., 2 FIG., 1 TAB

We explicitly present the comparison of the results for the astrophysical S-factor and reaction rate for the $^6$Li($p,\gamma$)$^7$Be capture process at astrophysical energies, presented in Phys. Rev. Phys. Rev. C 105, 065806 (2022) and Phys. Rev. C 108. 065801 (2023) obtained within the famework of potential models. We demonstrate that both potential model approaches describe successfully the astrophysical S-factor and reaction rate simultaneously and reproduce the LUNA Collaboration [Phys. Rev. C 102, 052802(R) (2020)] results., Comment: 2 page, 2 fig, 13 ref

We study a radiative $p^{15}$N capture on the ground state of $^{16}$O at stellar energies within the framework of a modified potential cluster model (MPCM) with forbidden states, including low-lying resonances. The investigation of the $^{15}$N($p,\gamma _{0}$)$^{16}$O reaction includes the consideration of $^{3}S_{1}$ resonances due to $E1$ transitions and the contribution of $^{3}P_{1}$ scattering wave in $p$ + $^{15}$N channel due to $^{3}P_{1}\longrightarrow $ $^{3}P_{0}$ $M1$ transition. We calculated the astrophysical low-energy $S-$factor, and extrapolated $S(0)$ turned out to be within $34.7-40.4$ keV$\cdot $b. The important role of the asymptotic constant (AC) for the $^{15}$N($p,\gamma _{0}$)$^{16}$O process with interfering $^{3}S_{1}$(312) and $^{3}S_{1}$(962) resonances is elucidated. A comparison of our calculation for $S-$factor with existing experimental and theoretical data is addressed, and a reasonable agreement is found. The reaction rate is calculated and compared with the existing rates. It has negligible dependence on the variation of AC, but shows a strong impact of the interference of $^{3}S_{1}$(312) and $^{3}S_{1}$(962) resonances, especially at temperatures, referring to the CNO Gamow windows. We estimate the contribution of cascade transitions to the reaction rate based on the exclusive experimental data by \textit{Imbriani, et al. 2012}. The reaction rate enhancement due to the cascade transitions is observed from $T_{9} > 0.3 $ and reaches the maximum factor $\sim $\ 1.3 at $T_{9}=1.3$. We present the Gamow energy window and a comparison of rates for radiative proton capture reactions $^{12}$N($p,\gamma $)$^{13}$O, $^{13}$N($p,\gamma $) $^{14}$O, $^{14}$N($p,\gamma $)$^{15}$O, and $^{15}$N($p,\gamma $)$^{16}$O obtained in the framework of the MPCM and give temperature windows, prevalence, and significance of each process., Comment: 17 pages, 9 figures

We present new calculations of the astrophysical $S-$factor and reaction rate for the $^{6}$Li$(p,\gamma )^{7}$Be reaction at energies of 10 keV to 5 MeV in the framework of a modified potential cluster model with forbidden states, including low lying resonances. The astrophysical $S(E)-$factor is compared with the available experimental data and calculations done within different models. The results for the $S-$factor are in good agreement with the data set (for $E<0.3$ MeV) and calculations (for $E<0.6$ MeV) of LUNA collaboration (Phys. Rev. C 102$,$ 052802, 2020). The recommended extrapolated zero value $S(0)$ turned out to be 101 eV $\cdot $ b. Using the theoretical total cross-sections$,$ the $^{6}$Li$(p,\gamma)^{7} $Be capture reaction rate is calculated at temperatures ranging from 0.01 to 10 $T_{9}$ and compared with NACRE and NACRE II. Analytical expressions for the $S-$factor and reaction rate are given, and the effect of low-lying resonances on the reaction rate is estimated. We suggest to update the NACRE and NACRE II databases in light of the new LUNA data and present calculations., Comment: 17 pages, 10 figures

Within the framework of the modified potential cluster model with forbidden states and their classification according to Young diagrams, the possibility of describing experimental data on the total cross sections of the neutron radiative capture on 7Li is considered. It is shown that the model used and the methods for constructing potentials make it possible to correctly describe the behavior of experimental cross sections at energies of 5 meV (5 10-3 eV) to 1 MeV(1 10+6 eV), where experimental data are available. Based on the obtained total cross sections up to 5 MeV, the reaction rate was calculated and its analytical approximation was carried out. It was shown that the 7Li(n,g)8Li reaction dominates at T9 < 0.1-0.2 as against with the burning of 7Li in reactions 7Li(3H,n)9Be and 7Li(4He,g)11B., Comment: 17p., 6 fig., 2 tab., 60 ref

The total cross sections of the neutron radiative capture on 12B at astrophysical energies to the ground state of 13B have been calculated in the energy range of 10E-8 to 10 MeV within the framework of a modified potential cluster model with the classification of orbital states according to Young diagrams. Reaction rates in the temperature range of 0.01 to 10 T9 and their analytical parameterization were obtained. The calculated rates of 12B(n,gamma)13B excess the previous results by approximately to one order. Cross sections and reaction rates of 12C(n,gamma)13C are calculated and compared to the n10B, n11B, n12B, and p12C reaction rates. It is proposed that obtained rates of the 12B(n,gamma)13B reaction should be taken into account in novel scenarios of stable isotope 13C synthesis without of 12C hydrogen burning., Comment: 18p., 5 fig., 4 tabl., 48 ref

Within the framework of the modified potential cluster model with forbidden states, the $^{13}$N($p,\gamma $)$^{14}$O reaction rate and the astrophysical $S$-factor are considered. It is shown that the first $p^{13}$% N resonance determines the $S$-factor and contributions of the $M1$ and $E2$ transitions are negligible at energies $E<1$ MeV, but are significant at high energies. The $S$-factor strongly depends on the $^{3}S_{1}$ resonance parameters. The influence of the width of \ the $^{3}S_{1}$ resonance on $S$% -factor is demonstrated. The reaction rate is calculated and an analytical approximation for the reaction rate is proposed. A comparison of our calculation with existing data is addressed. Results of our calculations for the $^{13}$N($p,\gamma )^{14}$O reaction rate provide the contribution to the steadily improving reaction rate database libraries. Our calculations of the $% ^{13}$N($p,\gamma )^{14}$O reaction rate along with results for the rates of $^{14}$N($% p,\gamma )^{15}$O and $^{12}$C$(p,\gamma )^{13}$N processes provide the temperature range $0.13

Within the framework of the modified potential cluster model with a classification of orbital states according to Young diagrams, the possibility of data description of the radiative neutron capture on 11B to the second excited state of 12B at 1.67365 MeV (2-) and prediction absentee of experimental data for the total cross sections to the third and fourth excited state of 12B at 2.6208 MeV (1-) and 2.723 MeV (0+) for reaction energy of 10 meV (1 meV = 10-3 eV) to 7 MeV was considered. The reaction rate in the temperature range of 0.01 to 10.0 T9 is calculated on the basis of obtained cross sections, which take into account resonances up to 5 MeV. It is shown, that low-lying resonances exercise a significant influence to the capture reaction rate. The approximation of the calculation reaction rate is carried out by the simple analytic formula., Comment: 20p., 32 ref., 9 fig., 5 tabl. arXiv admin note: substantial text overlap with arXiv:1911.00331, arXiv:1907.06832

Within the framework of the modified potential cluster model with a classification of orbital states according to Young diagrams, the possibility of prediction absentee experimental data for the total cross sections of the radiative neutron capture on 11B to the first excited state 12B at 0.95 MeV (2+) for reaction energy of 10 meV (1 meV = 10-3 eV) to 7 MeV. The reaction rate in the temperature range of 0.01 to 10.0 T9 is calculated on the basis of obtained cross sections, which take into account resonances up to 5 MeV. It is shown that low-lying resonances exercise a significant influence to the capture reaction rate. The approximation of the calculation reaction rate is carried out by the simple analytic formula., Comment: 16p., 4 fig., 32 ref

The total cross sections of the radiative proton capture on 8Li at astrophysical energies were considered in the framework of the modified potential cluster model with forbidden states, with the classification of the orbital cluster states according to Young diagrams. The recalculation of total cross sections for the 9Be({\gamma},p0)8Li photodisintegration was used as experimental data. In whole, it is possible to obtain the available data on cross sections at energies to 7.0 MeV. Astrophysical S-factors and reaction rates at the temperature range of 0.01 to 10 T9 were calculated. It was shown that the resonances in the p8Li scattering channel considerably influence to the reaction rate and, in the first place, the first - at 87 keV. The analytical parametrization was obtained for calculated reaction rate., Comment: tabl.7, fig.4, 43 ref. 15p

Within the framework of the modified potential cluster model with a classification of orbital states according to Young diagrams, the possibility of describing experimental data for total cross sections of the neutron radiative capture on 11B to the ground state of 12B at energies of 10 meV (1 meV = 10-3 eV) to 7 MeV was considered. It was shown that, taking into account only the E1 transition from the S state of the n11B scattering to the ground state of 12B, it is quite possible to explain the magnitude of the known experimental cross sections at energies of 25.3 meV to 70 keV. Furthermore, on the basis of the total cross sections of 10 meV to 7 MeV, but excluding resonances above 5 MeV, the reaction rate is calculated in the temperature range of 0.01 to 10.0 T9. It is shown that the inclusion of low-lying resonance states makes a significant contribution to the reaction rate, starting already with temperatures of 0.2-0.3 T9., Comment: 9 fig., 55 ref. 2 tabl., 23 pages

We present the analytical expressions for the differential cross sections and independent partial amplitudes for elastic scattering of nuclear particles for channels with a spin value of 1/2, 1, 3/2, 2 and 5/2. The independent partial amplitudes are presented for arbitrary orbital angular momentum $l$ and taking into account spin-orbit splitting. The analytical expressions allow one to carry out full phase shift analyses using experimental data for differential cross sections for processes with channel spins 1/2, 1, 3/2, 2 and 5/2., Comment: 33 pages

The possibility of description available experimental data for total cross section for reaction of the neutron capture on 10B at energies from 25.3 meV to 1.0 MeV was considered in the frame of the modified potential cluster model with forbidden states, classification of the orbital cluster states according to Young diagrams and taking into account the resonance behavior of phase shifts of the n10B elastic scattering. The obtained results agree with the experimental measurements. The calculated total cross sections are used for obtaining the reaction rate of the neutron capture on 10B at the temperature range from 0.01 to 10 T9. The reaction rate rises essentially at temperatures above 0.3 - 0.4 T9, conditioned by the resonances at the energy above 100 keV., Comment: 10 fig., 4 tabl., 16p

Big Bang Nucleosynthesis (BBN) relevance reactions 3He(2H,{\gamma})5Li, 3H(3He,{\gamma})6Li, 5Li(n,{\gamma})6Li as a key to approach for scenario of 6Li formation are treated. The rates of reaction for these processes are analyzed. Comparison of the reactions rates and the prevalence of light elements leads to the assumption that the two-step process 2H + 3He --> 5Li + {\gamma} and n + 5Li --> 6Li + {\gamma} can make a significant contribution to the formation of 6Li at the BBN at least at temperatures T9 of the order of unity. Calculations of the total cross sections, astrophysical S-factor, and reaction rates have been performed for 3He(2H,{\gamma})5Li radiative capture within the modified potential cluster model with forbidden states, which follow from the classification of the orbital cluster states according to Young diagrams. Numerical data and corresponding parametrizations cover the energy range up to 5 MeV and temperature range T9<10. An updated compilation of detailed data for the reaction 3He(2H,{\gamma})5Li are presented., Comment: 33p., 7 tabl., 11 fig

Within the modified potential cluster model with forbidden states effectively taking into account the Pauli Exclusion Principle the astrophysical S-factor of radiative p14N capture to 15O ground state has been calculated. The calculation was performed at the proton energy up to 5 MeV in the center of mass system (c.m.) with taking into account broad resonances up to 3.4 MeV in c.m. To explain reasonably the available experimental data it is required to admit the existence of 14N cluster in excited state 14N* with the excitation energy equal to 5.69 MeV and momentum JP = 1-. It is assumed that in this case the 4D1/2 state wave function of the p14N* clusters relative motion may be used. There was shown that it is succeeded to describe the S-factor of p14N capture in the resonance region only under the assumption that all low-lying resonances at 260(1/2+), 987(3/2+), 1447(1/2+), 2187(3/2+), and 3211(3/2+) keV in c.m. are the 4D1/2 and 4D3/2 scattering waves., Comment: 7p., 5 nsbl., 2 fig., 31 ref. arXiv admin note: text overlap with arXiv:0906.1097 by other authors

It is shown that in the framework of the modified potential cluster model we succeeded in correct describing the available experimental data for neutron radiative capture on 10Be total cross-sections at low, astrophysical and thermal energies. All interaction potentials for different partial waves are constructed by describing the basic characteristics of the bound states and spectra of final nucleus. Experimental data for the total cross-sections of the neutron radiative capture on 10Be were obtained by using known data for reduced probabilities of 11Be Coulomb dissociation., Comment: 8 fig., 6 tabl., 47 ref. 22 p

In the frame of modified potential cluster model based on the classification of orbital states by Young diagrams and revised interaction potential parameters for the bound states of 7Be in 3He4He cluster model with forbidden states the astrophysical S-factor for the radiative capture reaction has been calculated from the 10 keV. Obtained results S(23 keV) = 0.561 keV b reproduce the latest experimental data at 23 keV. Calculated and parametrized reaction rate is compared to some results known in the range of temperatures from 0.05 to 5 T9., Comment: 7p., 4 fig., 1 tabl

Calculations of the reaction rate of the proton radiative capture on 3H at temperatures from 0.01 T9 up to 5 T9, 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 3H 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., Comment: 16p., 3 fig, 55 ref

Within the framework of the modified potential cluster model with the forbidden states and the classification of states according to Young tableaux the possibility of describing the available experimental data for the total reaction cross sections of the neutron radiative capture on 10Be at thermal and astrophysical energies was shown., Comment: 15p., 2 tabl., 4 fig., 62 ref. arXiv admin note: text overlap with arXiv:1506.07954

Within the framework of the modified potential cluster model with the state classification of nuclear particles according to Young tableaux the possibility of describing the available experimental data for the total cross sections of the neutron radiative capture on 8Li at thermal and astrophysical energies was considered., Comment: 19p., 1 tabl., 5 fig

The manuscript is devoted to the description of the results obtained in the frame of the modified potential cluster model with the classification of states according to Young tableaux for neutron and proton radiative capture processes on 2H at thermal and astrophysical energies. It demonstrates methods of application that were obtained on the basis of phase shift analysis and characteristics of the bound states of 2H potentials for consideration of the radiative capture processes. First reaction of the proton capture directly takes part in the pp solar cycle, where it is the second reaction. The neutron capture is not a part of usual thermonuclear cycles in the Sun and stars, but can take part in the processes of primordial nucleosynthesis, following at formation and evolution of our entire Universe., Comment: arXiv admin note: text overlap with arXiv:1202.1995

The phase shift analysis for determination of the 2S1/2 resonance at 1.5 MeV was carried out on the basis of the known experimental measurements of the excitation functions of the p14C elastic scattering at four angles from 90 to 165 grad. and more than 100 energy values in the range from 600-800 to 2200-2400 keV. The obtained shape of the resonance 2S1/2 phase shift coincides with the characteristics of the corresponding level of 15N in whole, and the suggested potential acceptably describe this scattering phase shift., Comment: 8 fig., 29 ref., 7 p. arXiv admin note: substantial text overlap with arXiv:1405.6295, arXiv:1402.5236

The phase shift analysis for position location of the 2S1/2 resonance at 1,5 MeV was carried out on the basis of the known experimental measurements. Also, the possibility to describe the available experimental data on the astrophysical S-factor for the proton capture reaction on 14C to the ground state of 15N at astrophysical energies was considered in the frame of modified potential cluster model., Comment: 10 fig., 1 tab., 64 ref., 16p

Basing on the kwon experimental measurements of differential cross sections on n3He elastic scattering in the angular energy range 200 - 1600 the standard phase shifts analysis was performed at the energies from 1 MeV up to 5 MeV., Comment: 11p, 7 fig, 29 ref

In the framework of the modified potential cluster model with forbidden states the possibility of describing the available experimental data on the total cross sections and astrophysical S-factor for p11B radiative capture to the ground state of 12C was treated at astrophysical energies., Comment: 10p., 4 fig., 30 ref. arXiv admin note: text overlap with arXiv:1312.4274

The possibility of description of the experimental data for the astrophysical S-factor of the radiative proton capture on 15N at the energies from 50 to 1500 keV was considered in the framework of the modified potential cluster model with the classification of the orbital states according to Young tableaux. It was shown that, on the basis of the M1 and the E1 transitions from different states of the p15N scattering to the ground state of 16O in the p15N channel, it is quite succeed to explain general behavior of the S-factor in the considered energy range in the presence of two resonances., Comment: 11p, 3 fig, 47 ref

In the framework of the modified potential cluster model the possibility of describing the available experimental data for the total cross sections for n11B radiative capture at thermal and astrophysical energies were considered with taking into account the 21 and 430 keV resonances.

The total cross sections of the n9Be --> gamma10Be radiative capture are described in the framework of the modified potential cluster model (MPCM) with the classification of orbital states according to Young tableaux at thermal and astrophysical energies., Comment: 14 p., 3 fig., 36 ref

The total cross sections of the 16O(n,gamma)17O 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 16O 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 17O in the n16O channel from 2S1/2, 2P3/2 and 2D3/2 waves of the n16O scattering have been considered. These transitions have been considered in the resonance energy region at 433 and 1000 keV., Comment: 20p, 8 fig, 1 tabl. 77 ref

Within the potential cluster model with the forbidden states and an orbital states classification according to the Young diagrams the possibility of description of experimental data for the total cross-sections of radiative n15N-capture at energies from 25 to 370 keV was considered. It was shown that only on basis of the E1-transitions from the different states of n15N-scattering to the ground state of 16N nucleus in n15N-channel it is well succeed to explain the value of the total cross-sections in the considered energy range and to prognosticate its behavior at energy E 1 eV. These cross-sections at energies E 10 keV are approximated by the simple analytical form., Comment: 12 p., 2 fig., 1 tabl. 43 ref

The possibility of description of the experimental data on total cross sections of the radiative neutron capture on 14C and 14N is considered within the frame of the potential cluster model with forbidden states and their classification according to Young schemes. It is shown that the using model and the potential construction methods allow to reproduce correctly the behavior of experimental cross sections at the energies from 10 meV (0.01 eV) to 1 MeV., Comment: 18 p., 3 fig., 3 tabl, 42 ref

The continued interest to the study of the radiative neutron capture on atomic nuclei is caused, on the one hand, by the important role of this process in the analysis of many fundamental properties of nuclei and nuclear reactions, and, on the other hand, by the wide use of the capture cross section data in the various applications of nuclear physics and nuclear astrophysics, and, also, by the analysis of the processes of primordial nucleosynthesis in the Universe. This review is devoted to description of the results obtained for the processes of the radiative neutron capture at thermal and astrophysical energies on certain light atomic nuclei. The consideration of these processes is done in the frame of the potential cluster model, the general principles of which and calculation methods were described earlier. The methods of usage of the obtained on the basis of the phase shift analysis intercluster potentials will be directly demonstrated for calculations of the radiative capture characteristics. The considered capture reactions are not a part of stellar thermonuclear cycles, but they get in the basic reaction chain of primordial nucleosynthesis, taken place in the time of the Universe formation., Comment: 52p., 14 fig., 10 tabl., 140 ref. arXiv admin note: substantial text overlap with arXiv:1201.1741, arXiv:1202.1420

Within the potential cluster model with Pauli forbidden states the possibility of description of the experimental data on the total radiative n12C- and n13C-capture cross sections in the astrophysical energy range from 25 meV to 1.0 MeV is presented. The E1-transition covers the capture data from the scattering states to the ground one of 13C and 14C nuclei. Capture on the three low laying excited states 1/2+, 3/2- and 5/2+ of 13C was calculated., Comment: 17 page, 8 fig., 50 ref

The book covers the certain questions of nuclear physics and nuclear astrophysics of light atomic nuclei and their processes at low and ultralow energies. Some methods of calculation of nuclear characteristics of the thermonuclear processes considered in nuclear astrophysics are given here. The obtained results are directly applicable to the solution of certain nuclear astrophysics problems in the field of description of the thermonuclear processes in the Sun, the stars and the Universe. The book is based on the results of approximately three-four tens of scientific papers generally published in recent five-seven years and consists of three sections. The first of them covers the description of the general methods of calculation of certain nuclear characteristics for the bound states or the continuum of quantum particles. The second section deals with the methods, the computer programs and the results of the phase shift analysis of elastic scattering in the p3He, p6Li, p12C, n12C, p13C, 4He4He and 4He12C nuclear systems at low and ultralow energies. The results obtained on the basis of three-body models of certain light atomic nuclei are given in the third section, notably the 7Li, 9Be and 11B nuclei which are used for examination of the conjugated intercluster potentials determined on the basis of the phase shifts of elastic scattering and using then in the nuclear astrophysics problems connected with the description of the thermonuclear processes in the Universe. The book will be useful for advanced students, postgraduate students and PhD doctoral candidates in universities and research institutes in the field of astrophysics and nuclear physics. The book is presented in Russian with a few inserts into English., Comment: 311p

The variants of intercluster interaction potentials were constructed for description of the resonance nature of some phase shifts of the n7Li elastic scattering at low energies and the P2 ground state of 8Li in the n7Li cluster channel. The possibility of describing the total cross sections of 7Li(n,g)8Li in the region from 5 meV (5 10-3 eV) to 1 MeV including resonance at 0.25 MeV was shown with the potentials obtained in the potential cluster model taking into account forbidden states., Comment: 18 p., 5 fig., 72 ref

In this review we have considered the possibility to describe the astrophysical S-factors of radiative capture reactions with light atomic nuclei on the basis of the potential two-cluster model by taking into account the splitting the orbital states according to Young's schemes. Within this model, interaction of the nucleon clusters is described by local two-particle potential determined by fit to the scattering data and properties of bound states of these clusters. Many-body character of the problem is taken into account under some approximation, in terms of the allowed or forbidden by the Pauli principle states in intercluster potentials. An important feature of the approach is accounting for a dependence of interaction potential between clusters on the orbital Young scheme, which determines the permutation symmetry of the nucleon system. The astrophysical S-factors of the radiative capture processes in the p2H, p7Li and p12C systems are analyzed on the basis of this approach. It is shown that the approach allows one to describe quite reasonably experimental data available at low energies, when the phase shifts of cluster-cluster scattering are extracted from the data with minimal errors. In this connection the problem of experimental error decrease is exclusively urgent for the differential cross-sections of elastic scattering of light atomic nuclei at astrophysical energies and to perform a more accurate phase shift analysis. The increase in the accuracy will allow, in future, making more definite conclusions regarding the mechanisms and conditions of thermonuclear reactions, as well as understanding better their nature in general., Comment: arXiv admin note: substantial text overlap with arXiv:1005.1794 and arXiv:1005.1983

The phase shift analysis, done on the basis of the known measurements of the differential cross-sections of the p13C elastic scattering at the energy range 250-750 keV, shows that it is enough to take into account only 3S1 wave in the considered energy region. The potential for the triplet 3S1 state in p13C system at the resonance energy 0.55 MeV corresponding to quantum numbers JpT = 1-1 as well as the potential for the 3P1 bound state of 14N were constructed on the basis of the obtained scattering phase shifts. The possibility to describe the experimental data of the astrophysical S-factor of the p13C radiative capture at the energies 0.03-0.8 MeV was considered within the potential cluster model with the forbidden states. It was shown that we properly succeed in explanation of the energy behavior of the astrophysical S-factor for the p13C radiative capture at the resonance energy range 0.55 MeV (laboratory system)., Comment: 8 p., 2 fig

In the book the mathematical methods of nuclear cross sections and phases of elastic scattering, energy and characteristics of bound states in two- and three-particle nuclear systems, when the potentials of interaction contain not only central, but also tensor component, are presented. Are given the descriptions of the mathematical numerical calculation methods and computer programs in the algorithmic language "BASIC" for "Turbo Basic" of firm "Borland" for the computers of the type IBM PC AT. For the numerical solutions of the initial Schroedinger equations are used finite- difference and variational methods, and also method of Runge-Kutta with the automatic calling sequence on the assigned accuracy of results for the scattering phase shifts and binding energy. Is given the description not of the standard methods of solving the system of equations of Schroedinger to the bound states and the alternative to Schmidt's method, method of solution of the generalized matrix problem at the eigenvalues. The developed programs make it possible to determine the wave functions of relative motion of nuclear fragments, calibrated to the correct asymptotic behavior taking into account Coulomb interaction. The programs of the extraction of nuclear phases (phase shift analysis) from the differential elastic cross sections are given. The book can be used as the textbook according to the numerical mathematical methods for the students and the graduate students of the physical and mathematical specialties of higher educational institutions. This Book is written in Russian, but will perhaps present certain interest., Comment: 311 p

Monograph includes the results of the scientific work of the author for approximately 10 years and it is dedicated to theoretical studies of the structure of light atomic nuclei on the basis of potential cluster model with the forbidden states. Are examined questions of the single-valued construction of the intercluster potentials, which contain the forbidden states and simultaneously applied in the continuous and discrete spectra for the light nuclear systems with a mass of from 2 to 16. Is presented the mathematical apparatus and some calculation methods, utilized in the cluster model. Many questions, until now, considered here did not be reflected in the monographic literature. The book can represent interest for the students of elder courses, probationers, graduate students and scientific workers, who work in the field of theoretical nuclear physics. This Book is written in Russian, but will perhaps present certain interest., Comment: 247 p