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

Dubovichenko, S. B.; Burkova, N. А.; Dzhazairov-Kakhramanov, A. V.; Beysenov, Bekmurza

doi:10.1142/s0218301319300078

Cited by 6 publications

(14 citation statements)

References 58 publications

(265 reference statements)

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“…[11]: 0.14 < T 9 < 0.64. One should mentioned that the reaction rates for 13 N(p, γ) 14 O in the present work and 14 N(p, γ) 15 O [34] are obtained in the framework of the same theoretical approach.…”

Section: Cno and Hot Cno Cyclesmentioning

confidence: 67%

“…To carry out calculations of astrophysical S-factors for various reactions, we usually use the modified potential cluster model (MPCM) of light atomic nuclei [29,[31][32][33][34] with the classification of orbital states according to Young diagrams [36,37]. The model provides relatively many simple possibilities for performing calculations of various astrophysical characteristics.…”

Section: Theoretical Model and Formalismmentioning

confidence: 99%

“…For the 13 N(p, γ) 14 O reaction we use results of the present calculations and data from Ref. [11], for the reaction 14 N(p, γ) 15 O data [51] and [34] are used, while for the 12 C(p, γ) 13 N we employed data [51], which are very close to data given in the NACRE II database [26]. Let us comment on the difference in the data for the 14 N(p, γ) 15 O reaction (curves 3 and 5 in Fig.…”

Section: Cno and Hot Cno Cyclesmentioning

confidence: 99%

“…[51], in Ref. [34] the 14 N(p, γ) 15 O reaction rate was calculated by taking into account radiative capture of protons both in the GS of 14 N nucleus and in all four excited bound levels. Such consideration allows to describe experimental data for the astrophysical S-factors of the radiative proton capture on 14 N to five excited states of the 15 O nucleus at the excitation energies of 5.18 MeV to 6.86 MeV under the assumption, that all five resonances are D scattering waves.…”

Section: Cno and Hot Cno Cyclesmentioning

confidence: 99%

“…Continuing our studies of the processes of radiative capture on light atomic nuclei (see Refs. [29,31,33,34] for concise summaries), we consider the reaction of p+ 13 N→ 14 O+γ at astrophysical energies. This process is clearly not included in thermonuclear standard CNO cycle, but it makes a certain contribution to accumulation processes of a stable 14 N nucleus, which is further involved in other reactions of this cycle [35] and belongs to hot CNO cycle [1].…”

Section: Introductionmentioning

confidence: 99%

See 4 more Smart Citations

Reanalysis of $^{13}$N($p,γ$)$^{14}$O reaction and its role in stellar CNO cycle

Dubovichenko,

Kezerashvili,

Burkova

et al. 2020

Preprint

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Within the framework of the modified potential cluster model with forbidden states, the 13 N(p, γ) 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 M 1 and E2 transitions are negligible at energies E < 1 MeV, but are significant at high energies. The S-factor strongly depends on the 3 S1 resonance parameters. The influence of the width of the 3 S1 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, γ) 14 O reaction rate provide the contribution to the steadily improving reaction rate database libraries. Our calculations of the 13 N(p, γ) 14 O reaction rate along with results for the rates of 14 N(p, γ) 15 O and 12 C(p, γ) 13 N processes provide the temperature range 0.13 < T9 < 0.97 for the conversion of CNO cycle to the HCNO cycle. Our results demonstrate that at early stages of a nova explosion at temperatures about 0.1 T9 and at late stages of evolution of supermassive stars at temperatures about 1.0 T9 the ignition of the HCNO cycle could occur at much lower densities of a stellar medium.

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Section: Cno and Hot Cno Cyclesmentioning

confidence: 67%

Section: Theoretical Model and Formalismmentioning

confidence: 99%

Section: Cno and Hot Cno Cyclesmentioning

confidence: 99%

Section: Cno and Hot Cno Cyclesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Reanalysis of $^{13}$N($p,γ$)$^{14}$O reaction and its role in stellar CNO cycle

Dubovichenko,

Kezerashvili,

Burkova

et al. 2020

Preprint

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Comparative role of the ⁷Li(n, γ ) reaction in Big Bang nucleosynthesis

Burkova¹,

Dubovichenko²,

Dzhazairov-Kakhramanov³

et al. 2021

J. Phys. G: Nucl. Part. Phys.

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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 1 meV to 1.5 MeV, where experimental data are available. Based on the calculated total cross sections up to 5 MeV, the reaction rate is calculated and its analytical approximation is carried out. Resonance structure of 7Li(n, γ)8Li cross section and its impact on the reaction rate is examined. It is shown that the 7Li(n, γ)8Li reaction dominates at T 9 < 0.1 as opposed to the burning of 7Li in the 7Li(3H, n)9Be and 7Li(4Нe, γ)11B reactions, but comparable to (d, γ), (d, p), and (p, γ) at T 9 ∼ 1.

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Astrophysical S-factor and reaction rate for ¹⁵N(p,γ)¹⁶O within the modified potential cluster model*

Dubovichenko,

Tkachenko,

Kezerashvili

et al. 2024

Chinese Phys. C

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We study a radiative p 15N capture on the ground state of 16O at stellar energies within the framework of a modified potential cluster model (MPCM) with forbidden states, including low-lying resonances. The investigation of the 15N(p,γ0)16O reaction includes the consideration of 3 S 1 resonances due to E1 transitions and the contribution of 3 P 1 scattering wave in p + 15N channel due to 3 P 1 → 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·b. The important role of the asymptotic constant (AC) for the 15N(p,γ0)16O 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 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 ∼ 1.3 at T 9 = 1.3.We present the Gamow energy window and a comparison of rates for radiative proton capture reactions 12N(p,γ)13O, 13N(p,γ)14O, 14N(p,γ)15O, and 15N(p,γ)16O obtained in the framework of the MPCM and give temperature windows, prevalence, and significance of each process.

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

Cited by 6 publications

References 58 publications

Reanalysis of $^{13}$N($p,γ$)$^{14}$O reaction and its role in stellar CNO cycle

Reanalysis of $^{13}$N($p,γ$)$^{14}$O reaction and its role in stellar CNO cycle

Comparative role of the ⁷Li(n, γ ) reaction in Big Bang nucleosynthesis

Astrophysical S-factor and reaction rate for ¹⁵N(p,γ)¹⁶O within the modified potential cluster model*

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

Cited by 6 publications

References 58 publications

Reanalysis of $^{13}$N($p,γ$)$^{14}$O reaction and its role in stellar CNO cycle

Reanalysis of $^{13}$N($p,γ$)$^{14}$O reaction and its role in stellar CNO cycle

Comparative role of the 7Li(n, γ ) reaction in Big Bang nucleosynthesis

Astrophysical S-factor and reaction rate for 15N(p,γ)16O within the modified potential cluster model*

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Product

Resources

About

Comparative role of the ⁷Li(n, γ ) reaction in Big Bang nucleosynthesis

Astrophysical S-factor and reaction rate for ¹⁵N(p,γ)¹⁶O within the modified potential cluster model*