W. P. Liu

Determination of astrophysical 11c(p, γ)12N reaction rate from the asymptotic normalization coefficients of 12B → 11B + n

The squares of the neutron asymptotic normalization coefficient (ANC) for the virtual decay 12B →11B + n are extracted to be 1.20 ± 0.26, 0.354 ± 0.107 and 1.98 ± 0.35 fm−1 from the angular distributions of the 11B(d, p)12B reaction leading to the ground, first and second excited states of 12B respectively, using the Johnson–Soper approach. According to charge symmetry of strong interaction, the square of proton ANC of virtual decay 12N →11C + p is determined to be 1.63 ± 0.35 fm−1 and then utilized to calculate the astrophysical S-factor and the rate of the direct capture contribution in the 11C(p, γ)12N reaction. The astrophysical S-factor at zero energy for the direct capture, S(0), is derived to be 0.088 ± 0.019 keV b. An evaluated S(0) of 0.092 ± 0.009 keV b is then given by using the present and pre-existing experimental results. In addition, the proton widths of the first and second excited states of 12N are derived to be 0.91 ± 0.29 and 99 ± 20 keV from the neutron ANCs of 12B and used to compute the contribution from the first two resonances of 12N, respectively. We have also calculated the contribution from the interference effect between the direct capture and the second resonance.

The 8Li(d, p)9Li reaction and the astrophysical 8Li(n, γ)9Li reaction rate

The

The Li 8 ( d , p ) Li 9 reaction and the astrophysical Li 8 ( n , γ ) Li 9 reaction rate

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Proton widths of the low-lying16Fstates from the15N(7Li,6Li)16Nreaction

Li(

Spectroscopic factors for low-lying

n,\gamma

^{16}

)

N levels and the astrophysical

^9

^{15}

Li reaction plays an important role in both the r-process nucleosynthesis and the inhomogeneous big bang models, its direct capture rates can be extracted from the

N

^8

(n,\gamma)^{16}

Li(