Generalized potential-model description of mutual scattering of the lightestp+d,d<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:msup><mml:mrow><mml:mo>+</mml:mo></mml:mrow><mml:mrow><mml:mn>3</mml:mn></mml:mrow></mml:msup></mml:mrow></mml:math>He nuclei and the corresponding photonuclear reactions

2017

Int. J. Mod. Phys. E

Abstract:We have studied the neutron-capture reactions 8 Li(n,) 9 Li and its role in the primordial nucleosynthesis. The n+ 8 Li 9 Li+ reaction has a significant astrophysical interest, because it includes into one of the variants of chain of primordial nucleosynthesis processes of the Universe and thermonuclear reactions in type II supernovae. Furthermore, we consider the 9 Be(p,) 10 B reaction in the astrophysical energy range in the modified potential cluster model with splitting of orbital states according to Young tableaux and, in some cases, with forbidden states. The reaction 9 Be(p,) 10 B plays an important role in primordial and stellar nucleosynthesis of light elements in the p shell. Hydrogen burning in secondgeneration stars occurs via the proton-proton (pp) chain and CNO cycle, with the 9 Be(p,) 10 B reaction serving as an intermediate link between these cycles. Furthermore, the possibility of describing available experimental data for the total reaction cross sections of neutron radiative capture on 10 Be at thermal and astrophysical energies has been shown. This reaction is a part of one of the variants of the chain of primordial nucleosynthesis of the Universe due to which the elements with a mass of A > 11-12 may be formed. The results in the field of study of thermonuclear proton capture reaction on 10 B at ultralow, i.e., astrophysical energies will be presented further. The possibility of description of the experimental data for the astrophysical S-factor of the proton radiative capture on 16 O to the ground state of Keywords: Nuclear astrophysics; primordial nucleosynthesis; light atomic nuclei; low and astrophysical energies; radiative capture; total cross section; thermonuclear processes; potential cluster model; forbidden states. 21.60.Gx, 25.20.Lj, 25.40.Lw, 26.20.Np, 26.35.+c, 26.50.+x, 26.90.+n PACS Number(s): IntroductionThis review is the logical continuation of our works devoted to the radiative proton and neutron capture on light nuclei that were published in Int. J. Mod. Phys. E 21, 1250039 (2012); 22, 1350028 (2013); 22, 1350075 (2013); 23, 1430012 (2014). Astrophysical aspects of the reviewAs we know, light radioactive nuclei play an important role in many astrophysical environments. In addition, such parameter as cross section of the capture reactions as 2 a function of energy and reaction rates are very important for investigation of many astrophysical problems such as primordial nucleosynthesis of the Universe, main trends of stellar evolution, novae and super-novae explosions, X-ray bursts etc. The continued interest in the study of processes of radiative neutron capture on light nuclei at thermal (> 10 meV) and astrophysical (> 1 keV) energies is caused by several reasons. Firstly, this process plays a significant part in the study of many fundamental properties of nuclear reactions, and secondly, the data on the capture cross sections are widely used in a various applications of nuclear physics and nuclear astrophysics, for example, in the process of studying of...

Section: B(p) 11 C Reactionmentioning

confidence: 99%

“…Furthermore, potentials obtained by the same way can be used in any calculations connected with the solution of nuclear-physical and astrophysical problems of low, lowest and thermal interaction energies. 36,130,160 …”

Section: B(p) 11 C Reactionmentioning

confidence: 99%

Study of the nucleon radiative captures 8Li(n,γ)9Li, 9Be(p,γ)10B, 10Be(n,γ)11Be, 10B(p,γ)11C, and 16O(p,γ)17F at thermal and astrophysical energies

2017

Int. J. Mod. Phys. E

“…Using this concept, the potentials of the p 2 H interaction for scattering processes were received, parameters of such potentials were fully given in works [4,6]. Then "pure" phases [3] were separated in the doublet channel and on their basis potentials of inter-cluster interaction -"pure" in accordance with Young's schemes {3}-were constructed [4,6].The calculations of the E1 transition [4] show that the best results for the description of the total crosssections of the 3 He nucleus photodecay for the γ-quanta energy range 6-28 MeV, including the maximum value at E γ = 10-13 MeV, can be found if the potentials with peripheric repulsion of the 2 P -wave of the p 2 H scattering (table 1) and the S-interaction of the bound state (BS) with parameters −34.75 MeV and 0.15 fm −2 are used. However,…”

mentioning

confidence: 99%

“…This approach allows us to analyse the structure of inter-cluster interactions, detecting allowed and forbidden states in the interaction potential, and thus, the number of WF nodes of the relative motion of clusters [3,4].…”

mentioning

confidence: 99%

“…E1 transitions resulting from the orbital part of the electric operator Q Jm (L) were taken into account in these calculations of the photodecays of 3 He and 3 H a e-mail: albert-j@yandex.ru nuclei into p 2 H and n 2 H channels. The values of E2 crosssections and cross-sections depending on the spin part of the electric operator turned out to be several times less.…”

mentioning

confidence: 99%

See 1 more Smart Citation

Astrophysical S -factor of p2H radiative capture

2009

Eur. Phys. J. A

179

Abstract. The astrophysical S-factor of p 2 H radiative capture in the energy range down to 1 keV is considered in the potential cluster model with the classification of orbital states according to Young's scheme symmetry. It is shown that the approach used, which takes into account the E1 transition only, gives a good description of the new experimental data for two potentials of the bound state of the The radiative p + 2 H → 3 He + γ capture is a part of the hydrogen cycle and gives a considerable contribution to the energy efficiency of thermonuclear reactions [1] which account for burning of the Sun and stars of our Universe. The interacting nuclear particles of the hydrogen cycle have a minimal value which is a potential barrier. Thus, it is the first chain of nuclear reactions which can take place at ultralow energies and star temperatures. Then, for this chain, the process of the radiative p 2 H capture is the basic process for the transition from the primary proton fusion p + p → 2 H + e − + ν e to the final process 3 He+ 3 He → 4 He+2p [2] in the p-p chain. That is why the theoretical and experimental investigation of the radiative p 2 H capture in detail is of fundamental interest not only for nuclear astrophysics, but also for nuclear physics of ultralow energies and lightest atomic nuclei.We will discuss the astrophysical S-factors on the basis of a potential cluster model which takes into account the supermultiplet symmetry of wave functions (WF) with the splitting of orbital states according to Young's schemes. This approach allows us to analyse the structure of inter-cluster interactions, detecting allowed and forbidden states in the interaction potential, and thus, the number of WF nodes of the relative motion of clusters [3,4].The total cross-sections of the photoprocesses of the lightest nuclei were considered in this approach in our work [4]. E1 transitions resulting from the orbital part of the electric operator Q Jm (L) were taken into account in these calculations of the photodecays of 3 He and 3 H a e-mail: albert-j@yandex.ru nuclei into p 2 H and n 2 H channels. The values of E2 crosssections and cross-sections depending on the spin part of the electric operator turned out to be several times less. Further, it was assumed that E1 electric transitions in the N 2 H system are possible between the "pure" (scheme {3}) 2 S state of 3 H and 3 He nuclei and the doublet 2 P scattering state mixed according to Young's schemes {3} + {21}.To calculate photonuclear processes in the systems under consideration the nuclear part of the potential of intercluster p 2 H and n 2 H interactions is represented aswith a point-like Coulomb potential, V 0 -the Gaussian attractive part, and V 1 -the exponential repulsive part. The potential of each partial wave was constructed so that it would correctly describe the respective partial phase shift of the elastic scattering [5]. Using this concept, the potentials of the p 2 H interaction for scattering processes were received, parameters of such potentials were ful...

Radiative 3He(2H,γ)5Li Capture at Astrophysical Energy and Its Possible Role in Accumulation of 6Li at the BBN

Burkova

Recent Progress in Few-Body Physics

et al. 2020

Big Bang Nucleosynthesis (BBN) relevance reactions 3 He( 2 H,γ) 5 Li, 3 H( 3 He,γ) 6 Li, 5 Li(n,γ) 6 Li as a key to approach for scenario of 6 Li 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 2 H + 3 He  5 Li +  and n + 5 Li  6 Li +  can make a significant contribution to the formation of 6 Li at the BBN at least at temperatures T 9 of the order of unity.Calculations of the total cross sections, astrophysical S-factor, and reaction rates have been performed for 3 He( 2 H,γ) 5 Li 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 T 9 <10. An updated compilation of detailed data for the reaction 3 He( 2 H,γ) 5 Li are presented.Let us now examine in more detail the various aspects of the 3 He( 2 H, γ) 5 Li reaction, including the experimental data presented in the data base (EXFOR, 2013) and the original references cited therein, and the role of this process in various fields of application. Nuclear astrophysics aspectsOur parametrization of the experimental data for 2 H capture in 3 He (Buss et al. 1968) for the Sfactor at energies from 0.2 to 1.0 MeV according to Breit-Wigner and its further extrapolation 8 ) , ( J J I J J NJ P K NJ A J J J J J J J J