Indirect Methods and ANCs for Nuclear Astrophysics

Yarmukhamedov, R.; Tojiboev, O. R.; Artemov, S. V.

doi:10.7566/jpscp.14.021003

Cited by 3 publications

(7 citation statements)

References 13 publications

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“…As mentioned above, the V M 1 and V M 2 potentials were adjusted to the empirical ANC values from Refs. [38] and [40], respectively.…”

Section: B Cross Sections Of the Radiative Capture Processmentioning

confidence: 99%

“…Required empirical values of the asymptotic normalization coefficient can be extracted from the scattering data within different approaches, e.g. analytic continuation to the S-matrix pole [34], the effective range method [35][36][37] and distorted-wave Born approximation (DWBA) [38].…”

Section: Introductionmentioning

confidence: 99%

“…The two-body Gaussian potentials [21] which reproduce the bound states energies and the phase shifts in each partial wave will be examined. The potential parameters will be adjusted to reproduce the empirical values of the asymptotic normalization coefficient in the p 3/2 -and p 1/2 -bound states of the 7 Be nucleus, recently extracted from the phase-shift analysis within the DWBA method [38] and from the analysis of the experimental S-factor [40]. The d-and f-wave potentials from Ref.…”

Section: Introductionmentioning

confidence: 99%

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Astrophysical He3(α,γ)Be7 and
Tursunov
¹
,
Turakulov
²
,
Kadyrov
³

2018
Phys. Rev. C
12
5
16
0
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The astrophysical 3 He(α, γ) 7 Be and 3 H(α, γ) 7 Li direct capture processes are studied in the framework of the two-body model with the potentials of a simple Gaussian form, which describe correctly the phase-shifts in the s-, p-, d-, and f-waves, as well as the binding energy and the asymptotic normalization constant of the ground p 3/2 and the first excited p 1/2 bound states. It is shown that the E1-transition from the initial s-wave to the final p-waves is strongly dominant in both capture reactions. On this basis the s-wave potential parameters are adjusted to reproduce the new data of the LUNA collaboration around 100 keV and the newest data at the Gamov peak estimated with the help of the observed neutrino fluxes from the Sun, S 34 (23 +6 −5 keV)=0.548±0.054 keV b for the astrophysical S-factor of the capture process 3 He(α, γ) 7 Be. The resulting model describes well the astrophysical S-factor in low-energy Big Bang nucleosynthesis region of 180-400 keV, however has a tendency to underestimate the data above 0.5 MeV. The energy dependence of the S-factor is mostly consistent with the data and the results of the no-core shell model with continuum, but substantially different from the fermionic molecular dynamics model predictions. Two-body potentials, adjusted on the properties of the 7 Be nucleus, 3 He + α elastic scattering data and the astrophysical S-factor of the 3 He(α, γ) 7 Be direct capture reaction, are able to reproduce the properties of the 7 Li nucleus, the binding energies of the ground 3/2 − and first excited 1/2 − states, and phase shifts of the 3 H + α elastic scattering in partial waves. Most importantly, these potential models can successfully describe both absolute value and energy dependence of the existing experimental data for the mirror astrophysical 3 H(α, γ) 7 Li capture reaction without any additional adjustment of the parameters.

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“…As mentioned above, the V M 1 and V M 2 potentials were adjusted to the empirical ANC values from Refs. [38] and [40], respectively.…”

Section: B Cross Sections Of the Radiative Capture Processmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Astrophysical He3(α,γ)Be7 and
Tursunov
¹
,
Turakulov
²
,
Kadyrov
³

2018
Phys. Rev. C
12
5
16
0
View full text Add to dashboard Cite

show abstract

“…extracted from the analysis of the experimental data using the DWBA method [35]. B. Astrophysical S factor of the 3 He(α, γ) 7 Be reaction…”

Section: A Details Of the Calculations And Phase-shift Descriptionsmentioning

confidence: 99%

“…[22] the potential parameters in the s wave were adjusted to reproduce the astrophysical S factor of the α + 3 He direct capture reaction at low energies in addition to the phase shift data. In the p 3/2 and p 1/2 partial waves the potential parameters were additionally adjusted to reproduce the bound state properties: binding energies and the values of the asymptotic normalization coefficients (ANC) for the 7 Be(3/2 − ) ground and 7 Be(3/2 − ) excited states extracted from the analysis of the experimental data within the DWBA method [35]. This article is organized as follows.…”

Section: Introductionmentioning

confidence: 99%

Analysis of the $^{3}{\rm He}(α, γ)^{7}{\rm Be}$ and $^{3}{\rm H}(α,γ)^{7}{\rm Li}$ astrophysical direct capture reactions in a modified potential-model approach

Tursunov,

Turakulov,

Kadyrov

2020

Preprint

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Astrophysical S factors and reaction rates of the direct radiative capture processes 3 He(α, γ) 7 Be and 3 H(α, γ) 7 Li, as well as the primordial abundance of the 7 Li element, are estimated in the framework of a modified two-body potential model. It is shown that suitable modification of phase-equivalent α− 3 He potentials in the d waves can improve the description of the astrophysical S factor for the direct 3 He(α, γ) 7 Be radiative capture reaction at energies above 0.5 MeV. An estimated 7 Li/H abundance ratio of (4.89 ± 0.18) × 10 −10 is in very good agreement with the recent measurement of (5.0 ± 0.3) × 10 −10 by the LUNA collaboration.

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Potential cluster calculations for the astrophysical S-factor and reaction rate of the radiative 3He(4He,γ)7Be capture

Dubovichenko¹,

Burkova²,

Dzhazairov-Kakhramanov³

2018

Indian J Phys

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In the frame of a modified potential cluster model based on the classification of orbital states according to Young diagrams and revised interaction potential parameters for the bound states of 7 Be in the 3 He 4 He cluster model with forbidden states, the astrophysical S-factor for the radiative capture reaction 3 Не( 4 Не,) 7 Bе has been calculated from 10 keV. The result obtained, S(23 keV) = 0.561 keVb, reproduces the latest experimental data at 23 keV. The calculated and parametrized reaction rate is compared with some known results in the range of temperatures from 0.05 to 5T9.

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Indirect Methods and ANCs for Nuclear Astrophysics

Cited by 3 publications

References 13 publications

Astrophysical He3(α,γ)Be7 and
Tursunov
¹
,
Turakulov
²
,
Kadyrov
³

2018
Phys. Rev. C
12
5
16
0
View full text Add to dashboard Cite

Astrophysical He3(α,γ)Be7 and
Tursunov
¹
,
Turakulov
²
,
Kadyrov
³

2018
Phys. Rev. C
12
5
16
0
View full text Add to dashboard Cite

Analysis of the $^{3}{\rm He}(α, γ)^{7}{\rm Be}$ and $^{3}{\rm H}(α,γ)^{7}{\rm Li}$ astrophysical direct capture reactions in a modified potential-model approach

Potential cluster calculations for the astrophysical S-factor and reaction rate of the radiative 3He(4He,γ)7Be capture

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Indirect Methods and ANCs for Nuclear Astrophysics

Cited by 3 publications

References 13 publications

Astrophysical He3(α,γ)Be7 and Tursunov1, Turakulov2, Kadyrov3 2018Phys. Rev. C125160View full textAdd to dashboardCite

Astrophysical He3(α,γ)Be7 and Tursunov1, Turakulov2, Kadyrov3 2018Phys. Rev. C125160View full textAdd to dashboardCite

Analysis of the $^{3}{\rm He}(α, γ)^{7}{\rm Be}$ and $^{3}{\rm H}(α,γ)^{7}{\rm Li}$ astrophysical direct capture reactions in a modified potential-model approach

Potential cluster calculations for the astrophysical S-factor and reaction rate of the radiative 3He(4He,γ)7Be capture

Contact Info

Product

Resources

About

Astrophysical He3(α,γ)Be7 and
Tursunov
¹
,
Turakulov
²
,
Kadyrov
³

2018
Phys. Rev. C
12
5
16
0
View full text Add to dashboard Cite

Astrophysical He3(α,γ)Be7 and
Tursunov
¹
,
Turakulov
²
,
Kadyrov
³

2018
Phys. Rev. C
12
5
16
0
View full text Add to dashboard Cite