First inverse kinematics measurement of key resonances in the 22Ne(p,γ)23Na reaction at stellar temperatures

Lennarz, A.; Williams, M.; Laird, A. M.; Battino, U.; Chen, A.A.; Connolly, D.; Davids, B.; Esker, N. E.; Garg, R.; Greife, U.; Hager, U.; Hutcheon, D.A.; José, J.; Lovely, M.; Lyons, S.; Psaltis, A.; Riley, J. E.; Tattersall, A.; Ruiz, C.

doi:10.1016/j.physletb.2020.135539

Cited by 12 publications

(14 citation statements)

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“…Here we present strength measurements for the three low-energy resonances at center of mass energies of 149, 181, and 248 keV, along with the important reference resonances at 458, 610, 632, and 1222 keV (center of mass). Results from this study on the three low-energy resonances, along with the 458-keV resonance, were highlighted in a recent publication [30]. This article presents a more in-depth discussion of these results, along with those obtained for the other aforementioned resonances, as well as a study of direct capture.…”

Section: Introductionmentioning

confidence: 62%

First inverse kinematics study of the Ne22(p,γ)Na23 reaction and its role in AGB star and classical nova nucleosynthesis

et al. 2020

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Background: Globular clusters are known to exhibit anomalous abundance trends such as the sodium-oxygen anticorrelation. This trend is thought to arise via pollution of the cluster interstellar medium from a previous generation of stars. Intermediate-mass asymptotic giant branch stars undergoing hot bottom burning (HBB) are a prime candidate for producing sodium-rich oxygen-poor material, and then expelling this material via strong stellar winds. The amount of 23 Na produced in this environment has been shown to be sensitive to uncertainties in the 22 Ne(p, γ ) 23 Na reaction rate. The 22 Ne(p, γ ) 23 Na reaction is also activated in classical nova nucleosynthesis, strongly influencing predicted isotopic abundance ratios in the Na-Al region. Therefore, improved nuclear physics uncertainties for this reaction rate are of critical importance for the identification and classification of pre-solar grains produced by classical novae. Purpose: At temperatures relevant for both HBB in AGB stars and classical nova nucleosynthesis, the 22 Ne(p, γ ) 23 Na reaction rate is dominated by narrow resonances, with additional contribution from direct capture. This study presents new strength values for seven resonances, as well as a study of direct capture. Method: The experiment was performed in inverse kinematics by impinging an intense isotopically pure beam of 22 Ne onto a windowless H 2 gas target. The 23 Na recoils and prompt γ rays were detected in coincidence using a recoil mass separator coupled to a 4π bismuth-germanate scintillator array surrounding the target. Results: For the low-energy resonances, located at center of mass energies of 149, 181, and 248 keV, we recover stength values of ωγ 149 = 0.17 +0.05 −0.04 , ωγ 181 = 2.2 ± 0.4, and ωγ 248 = 8.2 ± 0.7 μeV, respectively. These results are in broad agreement with recent studies performed by the LUNA and TUNL groups. However, for the important reference resonance at 458 keV we obtain a strength value of ωγ 458 = 0.44 ± 0.02 eV, which is significantly lower than recently reported values. This is the first time that this resonance has been studied completely independently from other resonance strengths. For the 632-keV resonance we recover a strength value of ωγ 632 = 0.48 ± 0.02 eV, which is an order of magnitude higher than a recent study. For reference resonances at 610-and 1222-keV, our strength values are in agreement with the literature. In the case of direct capture, we recover an S factor of 60 keV b, consistent with prior forward kinematics experiments. Conclusions: In summary, we have performed the first direct measurement of 22 Ne(p, γ ) 23 Na in inverse kinematics. Our results are in broad agreement with the literature, with the notable exception of the 458-keV

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Section: Introductionmentioning

confidence: 62%

First inverse kinematics study of the Ne22(p,γ)Na23 reaction and its role in AGB star and classical nova nucleosynthesis

et al. 2020

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“…On the experimental side, new accelerator laboratories deep underground (CASPAR in the US [100], LUNA-MV in Italy [9,16,101,102], and JUNA in China [103]) and novel approaches in above-ground facilities have greatly increased the sensitivity of direct reaction-rate measurements. The latter include the use of recoil separators such as ERNA at INFN/Naples [104], St. George at the University of Notre Dame [105], and DRAGON at TRIUMF [106,107]; as well as new detector technologies such as the use of high-resolution silicon detector arrays [108] or active targets that track individual reaction products at TUNL's HIγS [109], quasi-spectroscopic neutron detectors [110],…”

Section: How Did We Get Here?mentioning

confidence: 99%

“…Broadly, these techniques fall into the two categories of direct and indirect measurements. Direct measurements of explosive hydrogen and helium burning reactions at or near the astrophysical energies where they occur have been performed with rare isotope beams using recoil separators (DRAGON) [404,106,107,405], active targets (MUSIC, AT-TPC, ANASEN, and others) [189,406,190,192], or gas targets (JENSA) [407,408,409,406]. In many cases direct measurements have not been feasible due to limited radioactive ion beam intensities and the extremely small cross sections involved.…”

Section: How Did We Get Here?mentioning

confidence: 99%

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Horizons: Nuclear Astrophysics in the 2020s and Beyond

Schatz,

Reyes,

Best

et al. 2022

Preprint

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Nuclear Astrophysics is a field at the intersection of nuclear physics and astrophysics, which seeks to understand the nuclear engines of astronomical objects and the origin of the chemical elements. This white paper summarizes progress and status of the field, the new open questions that have emerged, and the tremendous scientific opportunities that have opened up with major advances in capabilities across an ever growing number of disciplines and subfields that need to be integrated. We take a holistic view of the field discussing the unique challenges and opportunities in nuclear astrophysics in regards to science, diversity, education, and the interdisciplinarity and breadth of the field. Clearly nuclear astrophysics is a dynamic field with a bright future that is entering a new era of discovery opportunities.

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“…The data taken for resonances in the 22 Ne(α,γ) 26 Mg reaction in 2019 are expected to be published in 2021. Further, the results from stable beam measurements to investigate reactions such as 22 Ne(p,γ) 23 Na [193,194], 76 Se(α,γ) [195], 34 S(p,γ) [196] and 19 F(p,γ) [197] have recently been published.…”

Section: Recent Measurementsmentioning

confidence: 99%

The Status and Future of Direct Nuclear Reaction Measurements for Stellar Burning

Aliotta,

Buompane,

Couder

et al. 2021

Preprint

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The study of stellar burning began just over 100 years ago. Nonetheless, we do not yet have a detailed picture of the nucleosynthesis within stars and how nucleosynthesis impacts stellar structure and the remnants of stellar evolution. Achieving this understanding will require precise direct measurements of the nuclear reactions involved. This report summarizes the status of direct measurements for stellar burning, focusing on developments of the last couple of decades, and offering a prospectus of near-future developments.

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First inverse kinematics measurement of key resonances in the 22Ne(p,γ)23Na reaction at stellar temperatures

Cited by 12 publications

References 36 publications

First inverse kinematics study of the Ne22(p,γ)Na23 reaction and its role in AGB star and classical nova nucleosynthesis

First inverse kinematics study of the Ne22(p,γ)Na23 reaction and its role in AGB star and classical nova nucleosynthesis

Horizons: Nuclear Astrophysics in the 2020s and Beyond

The Status and Future of Direct Nuclear Reaction Measurements for Stellar Burning

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