The level structure of 20Na and the impact upon the stellar reaction rate for 19Ne(p, γ)20Na

Lamm, L. O.; Browne, C.P.; Görres, J.; Graff, S.; Wiescher, M.; Rollefson, A.A.; Brown, B. A.

doi:10.1016/0375-9474(90)90063-r

Cited by 54 publications

(38 citation statements)

References 21 publications

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“…The excitation energies were calculated assuming proton decay to the ground state of ' Ne and are in good agreement with the results of the ( He, t) experiments [7][8][9]. An upper limit (10 ) of~0.2% has been determined for the branching ratio of the decay to the 2645 keV state, expected at a proton energy of 446 keV.…”

Section: The Detection Efficiencies For Particles Emitted Inside Asupporting

confidence: 74%

“…The situation was improved when two independent experiments observed states above the proton threshold in Na. Lamm et al [7] studied the Ne( He, t) reaction at 25.5 MeV, while Kubono et al [8] studied the ( He, t) reaction at 55 MeV and the (p, n) reaction at 35 MeV. The resulting excitation energies of both experiments agree within the errors and have been recently confirmed by a high-resolution measurement of the ( He, t) reaction [9].…”

Section: Nucleosynthesismentioning

confidence: 73%

“…All experiments report a state at an energy of 2645 keV, which is the weighted average of these measuretnents (Table I) threshold. It has been shown [7,8] that this state will dominate the reaction rate for temperatures between 0.1 and 1 GK. However, the exact structure of this state is unclear, which leads to an estimated uncertainty of an order of magnitude for the reaction rate.…”

Section: Nucleosynthesismentioning

confidence: 99%

“…Kubono et al [8] assigned a spin of 1+ on the basis of their ( He, t) and (p, n) angular distribution and the strong population of the state in the (p, n) reaction and also identified it with the 1+ in the mirror nucleus F at 3488 keV. The ( He, t) angular distributions at lower energy showed little structure and Lamm et al [7] made spin assignments mainly on the basis of the analog structure of F and Ne. The level shifts were calculated with the isobaricmass-multiplet equation, where the coefficients were calculated with the global empirical isospin nonconserving interaction of Ormand and Brown [10].…”

Section: Nucleosynthesismentioning

confidence: 99%

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β-delayed proton decay ofMg20and its astrophysical implications

et al. 1992

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We have studied the P-delayed proton decay of 2OMg to search for the 2645 keV state in t Na. This state is of astrophysical interest, because any proton capture through this state would dominate the stellar reaction rate of the reaction ' Ne(p, y) Na. This reaction determines the break out from the hot CNO cycle. Several proton groups have been observed and their logft values have been determined. No protons from the 2645 keV state were seen and a lower limit of logft~5. 85 has been established. The impact of this result on the ' Ne(p, y) rate is discussed. PACS number(s): 23.40.s, 23.90.+w, 27.30.+t, 97.10.Cv

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Section: The Detection Efficiencies For Particles Emitted Inside Asupporting

confidence: 74%

Section: Nucleosynthesismentioning

confidence: 73%

Section: Nucleosynthesismentioning

confidence: 99%

Section: Nucleosynthesismentioning

confidence: 99%

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β-delayed proton decay ofMg20and its astrophysical implications

et al. 1992

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“…However, for over twenty years, the exact strength and energy of this resonance state have been a subject of intense debate [8][9][10][11][12][13][14][15][16][17][18][19][20][21].…”

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confidence: 99%

Constraining the ¹⁹Ne(p,γ)²⁰Na Reaction Rate Using a Direct Measurement at DRAGON

et al. 2017

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Abstract. A direct measurement of the 19 Ne(p, γ) 20 Na reaction has been performed in inverse kinematics at the DRAGON recoil separator, at an energy ∼ 10 keV higher than previous measurements. The key resonance in the 19 Ne +p system relevant for ONe novae and Type-I X-ray burst temperatures have been successfully measured for the first time. Preliminary estimates of the resonance energy and strength are reported as E c.m. ≈ 458 keV and ωγ ≈ 18 meV. These results are consistent with previous direct measurements, but disagree with the most recent study of the 19 Ne(p, γ) 20 Na reaction rate. These preliminary results will be finalised after a forthcoming negative log-likelihood analysis.Classical novae and X-ray bursts are among the most common types of explosive stellar phenomena observed in our Galaxy. These cataclysmic binary systems are stellar environments with high temperatures and densities, thought to be active regions of ongoing nucleosynthesis which energetically impact the surrounding interstellar medium (ISM).Classical novae are binary systems where hydrogen-rich material is accreted from a main sequence or red giant branch star onto the surface of a companion white dwarf. As the accreted material mixes with the heavier elements already present on the surface of the white dwarf, a thermonuclear runaway is triggered, which leads to explosive mass ejections from the white dwarf's surface, with the process recurring over a time-scale of ∼ 10 4 -10 5 years [1]. The composition of the white dwarf star has a significant impact on the composition of the nova ejecta; novae with more massive oxygen-neon (ONe) white dwarfs are characterised by higher peak temperatures (∼ 0.4 GK) than less massive carbon-oxygen (CO) white dwarfs (∼ 0.2 GK), and are thus thought to synthesise elements up to the Si-Ca mass region [2]. Therefore, determining the nature of the underlying white dwarf is crucial to meaningfully compare theoretical calculations with astronomical data.

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11-Sodium

Sukhoruchkin

Soroko

2004

Tables of Proton and Α-Particle Resonance Parameters. Part 1

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The level structure of 20Na and the impact upon the stellar reaction rate for 19Ne(p, γ)20Na

Cited by 54 publications

References 21 publications

β-delayed proton decay ofMg20and its astrophysical implications

β-delayed proton decay ofMg20and its astrophysical implications

Constraining the ¹⁹Ne(p,γ)²⁰Na Reaction Rate Using a Direct Measurement at DRAGON

11-Sodium

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The level structure of 20Na and the impact upon the stellar reaction rate for 19Ne(p, γ)20Na

Cited by 54 publications

References 21 publications

β-delayed proton decay ofMg20and its astrophysical implications

β-delayed proton decay ofMg20and its astrophysical implications

Constraining the 19Ne(p,γ)20Na Reaction Rate Using a Direct Measurement at DRAGON

11-Sodium

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Constraining the ¹⁹Ne(p,γ)²⁰Na Reaction Rate Using a Direct Measurement at DRAGON