Nuclear asymptotic normalization coefficients for 14N → 13C + p configurations and astrophysical S factor for radiative proton capture

Artemov, S. V.; Bajajin, A. G.; Igamov, S. B.; Nie, G. K.; Yarmukhamedov, R.

doi:10.1134/s1063778808060045

Cited by 17 publications

(21 citation statements)

References 29 publications

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“…Using a corrected value for C 3 He according to Ref. [36], one gets for 16 O C 2 exp = 175(29) fm −1 , which is much smaller than the value from Ref. [34].…”

Section: A = 16mentioning

confidence: 69%

Overlap functions, spectroscopic factors, and asymptotic normalization coefficients generated by a shell-model source term

Timofeyuk

2010

Phys. Rev. C

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Overlap functions for one-nucleon removal are calculated as solutions of the inhomogeneous equation. The source term for this equation is generated by the 0hω no-core shell-model wave functions and the effective nucleon-nucleon (NN) interactions that fit oscillator matrix elements derived from the NN scattering data. For the lightest A 4 nuclei this method gives reasonable agreement with exact ab initio calculations. For 4 < A 16, this method gives a fair agreement between the calculated and measured asymptotic normalization coefficients. The spectroscopic factors obtained show systematic deviation from the corresponding shell-model values. This deviation correlates with nucleon separation energies and follows a similar trend seen in the reduction factor of the nucleon knockout cross sections. Comparison with the overlap functions and spectroscopic factors obtained in the variational Monte Carlo method is presented and discussed.

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“…Using a corrected value for C 3 He according to Ref. [36], one gets for 16 O C 2 exp = 175(29) fm −1 , which is much smaller than the value from Ref. [34].…”

Section: A = 16mentioning

confidence: 69%

Overlap functions, spectroscopic factors, and asymptotic normalization coefficients generated by a shell-model source term

Timofeyuk

2010

Phys. Rev. C

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“…The C 2 dp value used in the present calculations was earlier refined in [23,29] and was taken to be 4.32 ± 0.35 fm −1 at b dp = 1.84 fm −1/2 . We disregarded channel-coupling effects since their contribution in the reaction 14 N( 3 He, d) 15 O is substantially smaller than the experimental errors and the uncertainties of the method [11].…”

Section: Methods For Analyzing Differential Crossmentioning

confidence: 99%

“…As was indicated in [23] and in the Introduction, the underestimated value of C 2 dp = 3.90 ± 0.06 fm −1 was employed in [7,11]. From the data in Table 3, one can see that, for the ground state, all three values of the square of the asymptotic normalization coefficient rescaled to the same value of C 2 dp lie within the overlapping intervals of the errors around their weighted-mean value of C 2 g.s.…”

Section: Procedures For Extracting the Asymptoticmentioning

confidence: 97%

“…Information obtained in this way is used to extrapolate the astrophysical S factor to the region of ultralow energies, including E = 0 (see Section 3). Previously, this approach was successfully used in [8,11,[21][22][23]. It is physically justified from the point of view of reducing the number of adjustable parameters (including resonance widths, resonance energies, and channel radius) inherent in the R-matrix method.…”

Section: Introductionmentioning

confidence: 99%

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Extrapolation of astrophysical S factors for the reaction 14N((p, γ) 15O to near-zero energies

et al. 2012

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The astrophysical S factors for the radiative-capture reaction 14 N(p, γ) 15 O in the region of ultralow energies were calculated on the basis of the R-matrix approach. The values of the radiative and protonic widths were fitted to new experimental data. The contribution of direct radiative capture to bound states of the 15 O nucleus was determined with the aid of asymptotic normalization coefficients, whose values were refined in the present study on the basis of the results obtained from an analysis of the reaction 14 N( 3 He, d) 15 O at three different energies of incident helium ions. A value of S(0) = 1.79 ± 0.31 keV b was obtained for the total astrophysical S factor, and the reaction rate was determined for the process 14 N(p, γ) 15 O.

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“…The known extrapolations of the measured S-factor to zero energy for the transitions to the ground state of 14 N lead to the following values: 5.25 keV b [34]; it was obtained 5.16±72 keV b, on the basis of results [34] in [35]; the value 5.36±71 keV b was found in [36]; the value 5.5 keV b was suggested in measurements [37]; and the value 5.06 keV b, for the S-factor at zero energy, was given in [38].…”

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confidence: 99%

Astrophysical S-factor for the radiative-capture reaction p 13C → 14Nγ

Dubovichenko

2012

Phys. Atom. Nuclei

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The phase shift analysis, done on the basis of the known measurements of the differential cross-sections of the р 13 С elastic scattering at the energy range 250750 keV, shows that it is enough to take into account only 3 S 1 wave in the considered energy region. The potential for the triplet 3 S 1 state in р 13 С system at the resonance energy 0.55 MeV corresponding to quantum numbers J  T = 1 -1 as well as the potential for the 3 Р 1 bound state of 14 N were constructed on the basis of the obtained scattering phase shifts. The possibility to describe the experimental data of the astrophysical S-factor of the р 13 С radiative capture at the energies 0.030.8 MeV was considered within the potential cluster model with the forbidden states. It was shown that we properly succeed in explanation of the energy behavior of the astrophysical S-factor for the р 13 С radiative capture at the resonance energy range 0.55 MeV (laboratory system). PACS number(s): 26.; 21.60.Gx; 02

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Nuclear asymptotic normalization coefficients for 14N → 13C + p configurations and astrophysical S factor for radiative proton capture

Cited by 17 publications

References 29 publications

Overlap functions, spectroscopic factors, and asymptotic normalization coefficients generated by a shell-model source term

Overlap functions, spectroscopic factors, and asymptotic normalization coefficients generated by a shell-model source term

Extrapolation of astrophysical S factors for the reaction 14N((p, γ) 15O to near-zero energies

Astrophysical S-factor for the radiative-capture reaction p 13C → 14Nγ

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