Vector-polarization measurements and phase-shift analysis for d-α scattering between 3 and 11 MeV

Keller, L.G.; Haeberli, W.

doi:10.1016/0375-9474(70)90244-7

Cited by 53 publications

(11 citation statements)

References 22 publications

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“…The method for the single-channel scattering problem is straightforward, as the Numerov's outgoing solution from r = 0 to the final grid point is matched to the function ϕ(r) = cos δ l F l (η; kr) + sin δ l G l (η; kr), (28) which is normalized to the unitary flux. Here F l (η; kr) and G l (η; kr) are the regular and irregular Coulomb functions, and k the α + d relative momentum.…”

Section: Methodsmentioning

confidence: 99%

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α+d→Li6+γ astrophysical S factor and its implications for Big Bang nucleosynthesis

et al. 2017

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The α + d → 6 Li + γ radiative capture is studied in order to predict the 6 Li primordial abundance. Within a two-body framework, the α particle and the deuteron are considered the structureless constituents of 6 Li. Five α + d potentials are used to solve the two-body problem: four of them are taken from the literature, only one having also a tensor component. A fifth model is here constructed in order to reproduce, besides the 6 Li static properties as binding energy, magnetic dipole, and electric quadrupole moments, also the S-state asymptotic normalization coefficient (ANC). The two-body bound and scattering problem is solved with different techniques, in order to minimize the numerical uncertainty of the present results. The long-wavelength approximation is used, and therefore only the electric dipole and quadrupole operators are retained. The astrophysical S factor is found to be significantly sensitive to the ANC, but in all the cases in good agreement with the available experimental data. The theoretical uncertainty has been estimated of the order of few percent when the potentials which reproduce the ANC are considered, but increases up to 20% when all five potential models are retained. The effect of this S-factor prediction on the 6 Li primordial abundance is studied, using the public code PArthENoPE. For the five models considered here we find 6 Li/H = (0.9-1.8) × 10 −14 , with the baryon density parameter in the 3-σ range of Planck 2015 analysis, b h 2 = 0.022 26 ± 0.000 23.

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Section: Methodsmentioning

confidence: 99%

“…In order to do so, the depth V J 0 has been fitted to the experimental scattering phase shifts for every initial channel, minimizing the χ 2 of the calculated phase shifts with respect to the available experimental data taken from Refs. [24][25][26][27][28]. In this procedure, we minimized the χ 2 changing the value of V J 0 .…”

Section: Potentialmentioning

confidence: 99%

α+d→Li6+γ astrophysical S factor and its implications for Big Bang nucleosynthesis

et al. 2017

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“…The results of the calculations of the phase shifts for the 2 S 1 , 3 P j (j = 0, 1 and 2) and 3 D j (j = 2 and 3) waves show rather a well agreement with the experimental data. [32][33][34][35] Besides, the calculated values of phase shifts with respect to variation of the r 0 and a parameters within the intervals above are changed within the uncertainty of about ∼2-3%.…”

Section: Asymptotic Normalization Coefficient (Respective Nuclearmentioning

confidence: 93%

Determination of the asymptotic normalization coefficient (nuclear vertex constant) for α + d →6Li from the new direct measured d(α,γ)6Li data and its implication for extrapolating the d(α,γ)6Li astrophysical S factor at Big Bang energies

Tursunmakhatov

Yarmukhamedov

2019

Int. J. Mod. Phys. Conf. Ser.

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The results of the analysis of the new experimental astrophysical S factors [Formula: see text] [D. Trezzi et al., Astropart. Phys. 89, 57 (2017)] and those measured earlier [R. G. Robertson et al., Phys. Rev. Lett. 47, 1867 (1981)] for the nuclear-astrophysical [Formula: see text] reaction directly measured at extremely low energies [Formula: see text], which is derived within the modified two-body potential method, are presented. New estimates and their uncertainties have been obtained for values of the asymptotic normalization coefficient for [Formula: see text] and for the direct astrophysical [Formula: see text] factors at Big Bang energies.

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“…where c" ~ s-(1/2/1;) q"', (18) As can be seen in Shanley's paper, we must solve 9-or 10-coupled integral equations for each J". Hereafter.…”

Section: Y Koikementioning

confidence: 99%

Three-Body Calculation of d- Elastic Scattering

Koike

1978

Progress of Theoretical Physics

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S-, P-, D-waves and some higher wave phase shifts of d-a elastic scattering are calculated by solving the Amado-Lovelace equations in order to discuss the mechanism of this scattering and breakup reaction. Equations are solved by applying Pade technique. It is shown that this technique is especially useful to calculate elastic scattering. An interesting example of the convergence of the Born series is given. Remarkable improvements on Shanley's results are obtained in all partial waves. Effects of 'Li resonances are discussed and it is shown that the 1 + resonance play,; an important role to understand this scattering. It is suggested that the recently observed peak of the imaginary eigenphase by Griiebler et a!. does not suggest a new resonance of 'Li, but can be understood by this well-k~own resonance. In order to investigate the role of the Pauli principle, sensitivity to the s-wave a-nucleon interaction is discussed. § 1. IntroductionThe six-nucleon system, bound states (resonances) of 6 Li ( 6 He) and d-a scattering, can be considered a three-body problem, if the a-particle is regarded as a spinless boson which is justified by its unusually stable structure. In this viewpoint, several calculations of 6 Li levels have been done by using the Faddeev formalism with fairly good results.1l~4) As for d-a scattering, on the other hand, there had been for a long time only one calculation of d-a elastic scattering by Shanley,!) because it was much more difficult to solve the Faddeey equations in the sea ttering region.It has become relatively easy to solve the equations even m the scattering region because of the recently deYeloped Pade technique'),a) to study the threenucleon problem. Recently, Charnomordic et al.n have calculated the d-a elastic scattering observables with a noticeable improyement on Shanley's results. The calculation of the D(o:., ap)n reaction was started by the present author.s) ln contrast to the three-nucleon problem where each pair is dominated by a bound state and a virtual state, p-wave resonances play important roles in the present system. Furthermore, the three-body system itself is dominated by resonances of 6 Li. We can expect some different features of reaction mechanisms compared with N-d scattering. In this paper, we calculate real and imaginary parts of the phase shifts of d-a elastic scattering in order to know the effects of these resonances explicitly.One of the shortcomings in the present calculation is that the effect of the at University

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Vector-polarization measurements and phase-shift analysis for d-α scattering between 3 and 11 MeV

Cited by 53 publications

References 22 publications

α+d→Li6+γ astrophysical S factor and its implications for Big Bang nucleosynthesis

α+d→Li6+γ astrophysical S factor and its implications for Big Bang nucleosynthesis

Determination of the asymptotic normalization coefficient (nuclear vertex constant) for α + d →6Li from the new direct measured d(α,γ)6Li data and its implication for extrapolating the d(α,γ)6Li astrophysical S factor at Big Bang energies

Three-Body Calculation of d- Elastic Scattering

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