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

Abstract

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.

Determination of the 3He(α, γ)7Be and 6Li(p, γ)7Be astrophysical factors down to zero energy using the asymptotic normalization coefficients

“…The uncertainties given here includes both experimental errors in the dσ exp /dΩ (first term in square parentheses), as well as the model uncertainties (second term in square parentheses). Then, the direct capture contribution to the 3 He( 4 He,γ) 7 Be astrophysical factor at energies corresponding to the core temperature of the Sun was derived within the modified two-body potential model (MTBPM) framework [42,43], and the resulting S 3 4 (0) and S 3 4 (23 keV) factors were found to be S 3 4 (0) = 0.534 ± 0.025 [0.015; 0.019] keVb and S 3 4 (23 keV) = 0.525 ± 0.022 [0.016; 0.016] keVb. The comparison with the values in the literature is performed in fig.…”

Determination of the astrophysical factor of the 3He(α,γ)7Be down to zero energy using the asymptotic normalization coefficient method

“…The total errors shown here are calculated by summing the uncertainties in quadrature, taking into accout both experimental errors in the dσ exp /dΩ (first term in square parentheses) and the indetermination from the ANC for d + 4 He → 6 Li, and the model uncertainties (second term in square parentheses). Next, the direct capture term of the 3 He( 4 He,γ) 7 Be astrophysical factor at the Gamow energy of the core of the Sun was deduced using the modified two-body potential model (MTBPM) [41,42], and the resulting S 3 4 (0) and S 3 4 (23 keV) factors were established to be S 3 4 (0) = 0.534 ± 0.025 [0.015; 0.019] keVb and S 3 4 (23 keV) = 0.525 ± 0.022 [0.016; 0.016] keVb. The juxtaposition with the values in the literature shown in Fig.…”