RADIATIVE NEUTRON CAPTURE ON 9Be, 14C, 14N, 15N AND 16O AT THERMAL AND ASTROPHYSICAL ENERGIES

Dubovichenko, S. B.; Dzhazairov-Kakhramanov, A. V.; Afanasyeva, N.V.

doi:10.1142/s0218301313500754

Cited by 22 publications

(66 citation statements)

References 83 publications

(112 reference statements)

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“…Therefore, the cross section can be presented in the form of averaging by transitions from the mixed by spin D scattering waves to the mixed P excited states of 11 B in the n 10 B channel. This approach, suggested by us earlier at the consideration in the neutron radiative capture on 14 N [14], was used for some other reactions, and allows one to obtain good results for description of total cross sections for these reactions [13,14,[20][21][22][23][24].…”

Section: Classification Of the 11 B States According To Young Diagramsmentioning

confidence: 99%

“…Partial scattering potentials and BSs sometimes contain FS, constructed in the Gaussian form and obviously depend on all moments JLS of cluster system and orbital Young diagrams {f} of their relative motion [15]. Note that furthermore only BSs of 11 B of the negative parity are considered, which do not, apparently, halo-states [19].This, continually used by us approach, already justified itself at the considering more than 30 most different reactions of radiative capture type [13,14,[20][21][22][23][24][25][26][27].…”

Section: Introductionmentioning

confidence: 99%

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Influence of low-lying resonances on reaction rates for 10B(n,γ)11B capture

Dubovichenko

Burkova

Dzhazairov-Kakhramanov

2019

Nuclear Physics A

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The possibility of description available experimental data for total cross section for reaction of the neutron capture on 10 B 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 n 10 B 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 10 B at the temperature range from 0.01 to 10T 9 . The reaction rate rises essentially at temperatures above 0.3-0.4 T 9 , conditioned by the resonances at the energy above 100 keV.1. The first RS of 11 B at the excitation energy of 11.600(20) MeV or 146(20) keV relatively to the threshold of the n 10 B channel has J  = 5/2 + at the total width of 180(20) keV and neutron width of 4 keV [16,18]. It can be matched to the 6 S 5/2 scattering wave with FS or mixed by spin 6+8 D 5/2 scattering wave also with the bound FS.2. The second RS has the excitation energy of 11.893(13) MeV or 439(13) keV relatively to the threshold of the channel. Its total width of 194(6) keV, neutron width of 31 keV [18] and moment J  = 5/2 -. Therefore, it can be matched to the mixtured 6+8 P 5/2 scattering waves without FSs.3. The third RS has the excitation energy of 12.040(130) MeV or 586(13) keV relatively to the threshold. Its total width is about of 1000 keV [16,18], neutron width changing from 770 keV [18] to 1.34 MeV [16], and moment is equal to J  = 7/2 + -it can be matched to the 8 S 7/2 wave or 6+8 D 7/2 scattering waves with FS.4. The next resonance is located at the energy above 1 MeV, its moment does not fix unambiguously (see Table 11.18 in work [16]), and we do not consider it, because it is impossible to define its accessory to the certain partial wave.The resonance levels that can be matched to the P 3/2 or P 7/2 , P 9/2 states [16] are absence at the energy below 1 MeV in spectrum of 11 B. Therefore, their phase shifts can be equalized to zero, and because there are no FSs in these waves, so the depth of potentials can be equalized to zero too [13,14]. Consequently, we will consider E1 transitions the GS and four (2 nd , 3 rd , 4 th and 9 th ) ES in P waves from S and D scattering states and M1 process from the resonance 6 P 5/2 scattering wave. Methods of calculation of total cross sections

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Section: Classification Of the 11 B States According To Young Diagramsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Influence of low-lying resonances on reaction rates for 10B(n,γ)11B capture

Dubovichenko

Burkova

Dzhazairov-Kakhramanov

2019

Nuclear Physics A

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“…6 However, overcoming such a mass gap is possible through the chain of reactions 4 He(2n,γ) 6 He(2n,γ) 8 He(β -) 8 Li(n,γ) 9 Li(β -) 9 Be on this stage, 7,8 where the process considered here is also presented. This chain would provide an alternative way toward heavier isotopes such as 36 S, 40 Ar, 46 Ca, and 48 Ca. However, it is very important to know to what extent this chain can compete with the process 8 Li(β − ) 8 Be(2α).…”

Section: Astrophysical Aspects Of the Reviewmentioning

confidence: 99%

“…As usual, 37,38,42,[46][47][48][49][80][81][82] we use the potential of the Gaussian form with the point-like Coulomb term (2) in the capacity of the n 10 Be interaction in each partial wave with a given orbital angular moment L.…”

Section: The N 10 Be Interaction Potentialsmentioning

confidence: 99%

“…87 The total cross sections of the radiative capture (NJ,J f ) for the EJ-and M1-transitions in the potential cluster model are given elsewhere. 37,38,[46][47][48][49]58 For the neutron magnetic moment and 10 Be the following values were used:  n = -1.91304272µ 0 and ( 10 Be) = 0, 78 where µ 0 -nuclear magneton. The correctness of this expression for the М1 transition is pre-tested in our previous papers 37,38,42,80 on the basis of radiative neutron capture reaction on 7 Li and proton capture reaction on 2 Н at low and astrophysical energies.…”

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confidence: 99%

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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

Dubovichenko

Dzhazairov-Kakhramanov

2017

Int. J. Mod. Phys. E

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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...

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