Astrophysical S-factor of T(4He, γ)7Li reaction at E cm = 15.7 keV

Bystritsky, V. M.; Дудкин, Г. Н.; Emets, E. G.; Filipowicz, M.; Krylov, A. R.; Nechaev, B. A.; Nurkin, A.; Padalko, V. N.; Philippov, A. V.; Sadovsky, A.

doi:10.1134/s1547477117040057

Cited by 11 publications

(3 citation statements)

References 28 publications

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“…The Bayesian curves In the 3 H(α, γ) 7 Li calculation we use Z ψ = 1 and mass M ψ = 2809.43 MeV for the incoming 3 H. The charge and mass for the α is the same as before. The data for the capture cross section are from Caltech [14] and Tomsk [15]. As in the case of 7 Be, if we associate the binding momenta for the ground and 1st excited of 7 Li γ 0 ∼ γ 1 ∼ 80-90 MeV with the scale Q, then for this system we expect the convergence to be slower compared to the previous 3 He-α system which had smaller γ 0 , γ 1 .…”

Section: Bementioning

confidence: 99%

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Bayesian analysis of capture reactions $^3\mathrm{He}(α,γ)^7\mathrm{Be}$ and $^3\mathrm{H}(α,γ)^7\mathrm{Li}$

Premarathna,

Rupak

2019

Preprint

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Bayesian analysis of the radiative capture reactions 3 He(α, γ) 7 Be and 3 H(α, γ) 7 Li are performed to draw inferences about the cross sections at threshold. We do a model comparison of two competing effective field theory power countings for the capture reactions. The two power countings differ in the contribution of two-body electromagnetic currents. In one power counting, two-body currents contribute at leading order, and in the other they contribute at higher orders. The former is favored for 3 He(α, γ) 7 Be if elastic scattering data in the incoming channel is considered in the analysis. Without constraints from elastic scattering data, both the power countings are equally favored. For 3 H(α, γ) 7 Li, the first power counting with two-body current contributions at leading order is favored with or without constraints from elastic scattering data.

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Section: Bementioning

confidence: 99%

“…The reaction 3 H(α, γ) 7 Li is important for calculating 7 Li abundances, constraining astrophysical models of Big Bang Nucleosynthesis [12,13]. There are less constraints on this reaction from recent measurements [14,15].…”

Section: Introductionmentioning

confidence: 99%

Bayesian analysis of capture reactions $^3\mathrm{He}(α,γ)^7\mathrm{Be}$ and $^3\mathrm{H}(α,γ)^7\mathrm{Li}$

Premarathna,

Rupak

2019

Preprint

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“…8: (a) Astrophysical S factor for the 3 H(α, γ) 7 Li direct capture reaction calculated with modified potential models V n D and V n M 1 in comparison with available experimental datafrom Refs. [39][40][41][42][43][44][45] and ab-initio calculations [32,33]. Panel (b) highlights the low-energy region.…”

Section: Nacre II Datamentioning

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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To the Nature of Dark Matter

Dudkin

2023

Russ Phys J

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Astrophysical S-factor of T(4He, γ)7Li reaction at E cm = 15.7 keV

Cited by 11 publications

References 28 publications

Bayesian analysis of capture reactions $^3\mathrm{He}(α,γ)^7\mathrm{Be}$ and $^3\mathrm{H}(α,γ)^7\mathrm{Li}$

Bayesian analysis of capture reactions $^3\mathrm{He}(α,γ)^7\mathrm{Be}$ and $^3\mathrm{H}(α,γ)^7\mathrm{Li}$

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

To the Nature of Dark Matter

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