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

2016

Russ Phys J

:The possibility of description of the experimental data for the astrophysical S-factor of the proton radiative capture on 16 O to the ground and first excited states of 17 F was considered in the frame of the modified potential cluster model with forbidden states and classification of the states according to Young tableaux. It was shown that on the basis of the E1 transitions from the P states of p 16 O scattering to the bound states of 17 F in the p 16 O channel, it generally succeed to explain the value of measured astrophysical S-factors and reaction rates at astrophysical energies.

Section: The Astrophysical S-factorsupporting

confidence: 86%

“…Note that in our previous S-factor calculations [51] for the capture to the GS all matrix elements (ME) of transitions were calculated only up to 30 fm. Therefore, slightly other results were obtained for total cross sections at the capture to the GS.…”

Section: The Astrophysical S-factormentioning

confidence: 99%

Radiative p 16O Capture at Astrophyiscal Energies

2016

Russ Phys J

“…Turning to analysis of cluster states of N+ 14 N system with formation of 15 N or 15 О, we note that classification of orbital states of 14 C in the n 13 C system or 14 N in the p 13 C channel according to Young diagrams were considered by us earlier in Ref. 22. However, since we do not have total tables of Young diagrams products for system with more than eight particles, 23 which we used earlier for similar calculations, 1,2 results obtained further should be considered only a qualitative assessment of possible orbital symmetries in the BS of 15 О and 15 N nuclei for channels under consideration.…”

Section: Analysis Of Cluster States Of N+ 14 N Systemmentioning

confidence: 99%

“…Thus, limited with only the lowest partial waves with orbital momenta L = 0, 1, 2, we can say that for the n 14 C system 22 (for 14 С we have J  ,Т = 0 + 1 Ref. 26) in potential 2 S 1/2 wave there are forbidden and allowed state.…”

Section: State Classification By Young Diagramsmentioning

confidence: 99%

“…28 The potentials of the 2 Р waves of elastic scattering do not have the FS, and the bound FS may be present in the 2 D waves. 22 For the p 14 C system, 22,25 potential of the S-scattering wave contains a forbidden bound state, and the Р 1/2 wave has an allowed bound state, which corresponds to the GS of 15 N with J  = 1/2and is at binding energy of the p 14 C system, equals -10.2074 MeV. 26 In case of the n 14 N system 22 (for 14 N we have J  ,Т = 1 + 0 Ref.…”

Section: State Classification By Young Diagramsmentioning

confidence: 99%

See 1 more Smart Citation

Reaction rate of p14N →15Oγ capture to all bound states in potential cluster model

Burkova

Dzhazairov-Kakhramanov

et al. 2020

Int. J. Mod. Phys. E

Self Cite

Review of calculation results for astrophysical S-factor of the 14 N(р,  15 О capture reaction in the p 14 N channel of 15 O was presented. It was carried out in the frame of the modified potential cluster model, taking into account resonances in the 15 O spectrum up to 3.2 MeV at energy of incident protons varying from 30 keV to 5 MeV. It is possible to describe experimental data for the astrophysical Sfactors of the radiative proton capture on 14 N to five excited states of 15 O at excitation energies from 5.18 MeV to 6.86 MeV, only under assumption, that all five resonances are D scattering waves. Quality new physical interpretation of the capture mechanism is discussed in this channel to the ground state of 15 O. Carried out by us assumption that the ground state of 15 O is determined by the p 14 N * channel with excited 14 N * cluster, immediately allowed us to correctly describe order of values of the experimental S-factor for capture to this state. Taking into account these results, the total S-factor of the proton capture on 14 N and the reaction rates to the ground and five excited states of 15 O were determined at temperatures from 0.01 to 10 T 9 . The parametrization of the total reaction rate with a simple form is performed, which allows to obtain  2 equal to 0.06 with 5% errors of the calculated rate.1. With an excitation energy of 5.183(1) MeV above BS or -2.1141 MeV in c.m. Ref. 26 relative to threshold of the р 14 N channel, there is a first excited, but bound in this channel, state with the moment J  = 1/2 + , which can be matched to the doublet 2 S 1/2 wave with FS. Although such state can, of course, be considered as a quartet 4 D 1/2 wave with FS.2. The second ES (2 nd ES) with an excitation energy of 5.2409(3) MeV Ref. 26 relative to the GS or -2.0562 MeV relative to the threshold of the р 14 N channel has J  = 5/2 + and it can be matched to the mixture of doublet and quartet 2+4 D 5/2 waves with FS.3. The third excited state (3 rd ES) at an excitation energy of 6.1763(17) MeV Ref. 26 relative to the GS or -1.1208 MeV relative to channel threshold has J  = 3/2and it can be compared to a mixture of doublet and quartet 2+4 Р 3/2 -waves without an associated FS.4. The fourth excited state (4 th ES) has an excitation energy of 6.7931(17) MeV relative to the GS or -0.504 MeV Ref. 26 or relative to the channel threshold has J  = 3/2 + and it can be compared with the quartet 4 S 3/2 wave with the FS. Of course, this state may also be a mixture of doublet and quartet 2+4 D 3/2 waves with the FS.5. The fifth excited state (5 th ES) with an excitation energy of 6.8594(9) MeV Ref. 26 relative to the GS or -0.4377 MeV relative to the channel threshold has J  = 5/2 + and it can also be compared to a mixture of doublet and quartet 2+4 D 5/2 wave with the FS 6. There is another bound state in the р 14 N channel with J  = 7/2 + at an excitation energy of 7.2759(6) MeV Ref. 26 relative to the GS or -0.0212 MeV relative to the threshold of the considered channel, which can be compared to the 4 D 7/2 s...

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

Recent Progress in Few-Body Physics

Burkova

Dzhazairov-Kakhramanov

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