New Study of the Astrophysical Reaction [sup 12]C(α,γ)[sup 16]O via the [sup 12]C([sup 7]Li,t)[sup 16]O Transfer Reaction

Oulebsir, N.; Hammache, F.; Roussel, Pierre; Audouin, L.; Beaumel, D.; Bouda, A.; Fortier, S.; Gaudefroy, L.; Kiener, J.; Lefèbvre, A.; Tatischeff, V.; Mebarki, N.; Mimouni, J.

doi:10.1063/1.3518344

Cited by 2 publications

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“…The ( 7 Li, t) reaction is somewhat less affected by multi-step contributions, and is therefore more selective in the population of levels compared to the ( 6 Li, d) reaction. Also, it has been argued that the population of lower spins states is enhanced with the ( 7 Li, t) reaction [72]. The reactions have been applied to many astrophysical studies including 12 C( , a g) 16 O [72-74], 13 C( n , a ) 16 O [75, 76], and 22 Ne( , a g) 26 Mg [77], for example.…”

Section: Other Reaction Channelsmentioning

confidence: 99%

Transfer reactions in nuclear astrophysics

Bardayan

2016

J. Phys. G: Nucl. Part. Phys.

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To a high degree many aspects of the large-scale behavior of objects in the Universe are governed by the underlying nuclear physics. In fact the shell structure of nuclear physics is directly imprinted into the chemical abundances of the elements. The tranquility of the night sky is a direct result of the relatively slow rate of nuclear reactions that control and determines a star's fate. Understanding the nuclear structure and reaction rates between nuclei is vital to understanding our Universe. Nuclear-transfer reactions make accessible a wealth of knowledge from which we can extract much of the required nuclear physics information. A review of transfer reactions for nuclear astrophysics is presented with an emphasis on the experimental challenges and opportunities for future development.

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Section: Other Reaction Channelsmentioning

confidence: 99%

Transfer reactions in nuclear astrophysics

Bardayan

2016

J. Phys. G: Nucl. Part. Phys.

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“…) Reaction Brune (1999) [31] 2.08(20) × 10 14 1.14(10) × 10 5 12 C( 6 (7) Li,d(t)) 16 O Belhout (2007) [32] 1.87(54) × 10 14 1.40(50) × 10 5 12 C( 6 Li,d) 16 O Oulebsir (2012) [33] 2.00(35) × 10 14 1.44(28) × 10 5 12 C( 7 Li,t) 16 O Avila (2015) [34] 2.09(14) × 10 14 1.22(7) × 10 5 6 Li( 12 C,d) 16 O Adhikari (2017) [35] 2.55(35) × 10 14 1.67(23) × 10 5 12 C( 7 Li,t) 16 O Orlov (2017) [36] 2.073 × 10 14 0.5050 × 10 5 12 C(α,α) 12 C This work [25] 1.727(3) × 10 14 0.31(6) × 10 5 12 C(α,α) 12 C tion normalization factors, which are calculated by employing the formula in Eq. (12).…”

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ANCs of the bound states of 16O deduced from elastic α-12C scattering data

Ando

2023

Preprint

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Asymptotic normalization coefficients (ANCs) of the $0_1^+$, $0_2^+$, $1_1^-$, $2_1^+$, $3_1^-$ ($l_{i th}^\pi$) bound states of $^{16}$O are deduced from the phase shift data of elastic $\alpha$-$^{12}$C scattering at low energies. $S$ matrices of elastic $\alpha$-$^{12}$C scattering are constructed within cluster effective field theory (EFT), in which both bound and resonant states of $^{16}$O are considered. Parameters in the $S$ matrices are fitted to the precise phase shift data below the $p$-$^{15}$N breakup energy for the partial waves of $l=0,1,2,3,4,5,6$, and the ANCs are calculated by using the wave function normalization factors of $^{16}$O propagators for $l=0,1,2,3$. We review the values of ANCs, which are compared with other results in the literature, and discuss uncertainties of the ANCs obtained from the elastic $\alpha$-$^{12}$C scattering data in cluster EFT.

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New Study of the Astrophysical Reaction [sup 12]C(α,γ)[sup 16]O via the [sup 12]C([sup 7]Li,t)[sup 16]O Transfer Reaction

Cited by 2 publications

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Transfer reactions in nuclear astrophysics

Transfer reactions in nuclear astrophysics

ANCs of the bound states of 16O deduced from elastic α-12C scattering data

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