NACRE II: an update of the NACRE compilation of charged-particle-induced thermonuclear reaction rates for nuclei with mass number <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" altimg="si1.gif" overflow="scroll"><mml:mi>A</mml:mi><mml:mo>&lt;</mml:mo><mml:mn>16</mml:mn></mml:math>

Xu, Y.; Takahashi, Kohji; Goriely, Stéphane; Arnould, M.; Ohta, M.; Utsunomiya, H.

doi:10.1016/j.nuclphysa.2013.09.007

Cited by 294 publications

(208 citation statements)

References 362 publications

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“…Data are taken from Refs. [13] (open squares), [14] (filled circles), and [15] (filled triangles). The solid line represents the exact, fully antisymmetrized GSM-CC calculation for capture to both the ground state J π = 3/2 − 1 and the first excited state J π = 1/2 − 1 of 7 Be.…”

Section: Discussion Of Resultsmentioning

confidence: 99%

AstrophysicalS-factor for⁶Li(ρ, γ)⁷Be in the coupled-channel Gamow shell model

Dong

Fossez

Michel

et al. 2016

EPJ Web of Conferences

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Abstract. We have applied the Gamow shell model (GSM) in the coupled-channel representation to study the astrophysical S -factor for the proton radiative capture reaction of 6 Li. Reaction channels are built by coupling the proton wave function expanded in different partial waves with the GSM wave functions of the ground state (1 + ) and the excited states (3 + 1 , 0 + 1 and 2 + 1 ) of 6 Li. All relevant E1, M1, and E2 transitions from the initial continuum states in 7 Be to the final bound states (3/2 − 1 and 1/2 − 1 ) are included. It is found that the calculated total astrophysical S factor for this reaction agrees well with the experimental data.

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Section: Discussion Of Resultsmentioning

confidence: 99%

AstrophysicalS-factor for⁶Li(ρ, γ)⁷Be in the coupled-channel Gamow shell model

Dong

Fossez

Michel

et al. 2016

EPJ Web of Conferences

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“…Present d(p,γ) 3 He astrophysical S factors S (p,γ) are plotted together with previous experimental values referred from Refs. [5,8] and calculated values [4,9] in Fig. 3.…”

Section: Methodsmentioning

confidence: 99%

Measurements of Radiative Capture Cross Sections at Big Bang Energies

Tanaka¹,

Fukuda²,

Tanaka³

et al. 2017

Proceedings of the 14th International Symposium on Nuclei in the Cosmos (NIC2016)

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“…We calculated the resonant reaction rate and compare it with the total reaction rate evaluated in NACRE [17,18]. In the evaluation reported in NACRE, only 2 resonances at 8.1045 and 8.420 MeV are included.…”

Section: Alpha Resonant Scatteringmentioning

confidence: 99%

“…Direct measurement of (α, p) reactions, such as 14 O(α, p) [19], 11 C(α, p) [20], 21 Na(α, p), 18 Ne(α, p), 30 S(α, p), and 22 Mg(α, p), have also been performed with the TTIK method using RI beams at CRIB. Several (α, p) reactions have been studied at CRIB.…”

Section: Direct Measurement Of (α P) Reactionsmentioning

confidence: 99%

Experimental Studies of Light-Ion Nuclear Reactions Using Low-Energy RI Beams

Kahl¹,

Hayakawa²,

Sakaguchi³

et al. 2017

Proceedings of the 14th International Symposium on Nuclei in the Cosmos (NIC2016)

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CRIB (CNS Radio-Isotope Beam separator) is a low-energy RI beam separator of Center for Nuclear Study (CNS), the University of Tokyo. Studies on nuclear astrophysics, nuclear structure, and other interests have been performed using the RI beams at CRIB, forming international collaborations. A striking method to study astrophyiscal reactions involving radioactive nuclei is the thick-target method in inverse kinematics. Several astrophysical alpha-induced reactions have been be studied with that method at CRIB. A recent example is on the α resonant scattering with a radioactive 7 Be beam. This study is related to the astrophysical 7 Be(α,γ) reactions, important at hot p-p chain and νp-process in supernovae. There have been measurements based on several indirect methods, such as the asymptotic normalization coefficient (ANC) and Trojan horse method (THM). The first THM measurement using an RI beam has been performed at CRIB, to study the 18 F(p, α) 15 O reaction at astrophysical energies via the three body reaction 2 H( 18 F, α 15 O)n. The 18 F(p, α) 15 O reaction rate is crucial to understand the 511-keV γ-ray production in nova explosion phenomena, and we successfully evaluated the reaction cross section at novae temperature and below experimentally for the first time.

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NACRE II: an update of the NACRE compilation of charged-particle-induced thermonuclear reaction rates for nuclei with mass number A<16

Cited by 294 publications

References 362 publications

AstrophysicalS-factor for⁶Li(ρ, γ)⁷Be in the coupled-channel Gamow shell model

AstrophysicalS-factor for⁶Li(ρ, γ)⁷Be in the coupled-channel Gamow shell model

Measurements of Radiative Capture Cross Sections at Big Bang Energies

Experimental Studies of Light-Ion Nuclear Reactions Using Low-Energy RI Beams

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NACRE II: an update of the NACRE compilation of charged-particle-induced thermonuclear reaction rates for nuclei with mass number A<16

Cited by 294 publications

References 362 publications

AstrophysicalS-factor for6Li(ρ, γ)7Be in the coupled-channel Gamow shell model

AstrophysicalS-factor for6Li(ρ, γ)7Be in the coupled-channel Gamow shell model

Measurements of Radiative Capture Cross Sections at Big Bang Energies

Experimental Studies of Light-Ion Nuclear Reactions Using Low-Energy RI Beams

Contact Info

Product

Resources

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AstrophysicalS-factor for⁶Li(ρ, γ)⁷Be in the coupled-channel Gamow shell model

AstrophysicalS-factor for⁶Li(ρ, γ)⁷Be in the coupled-channel Gamow shell model