Direct Capture Cross Section and the 
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 and 105 keV Resonances in the 
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Ferraro, F.; Takács, M. P.; Piatti, D.; Cavanna, F.; Depalo, R.; Aliotta, M.; Bemmerer, D.; Best, A.; Boeltzig, A.; Broggini, C.; Bruno, Carlo; Caciolli, A.; Chillery, T.; Ciani, G. F.; Corvisiero, P.; Davinson, T.; D’Erasmo, G.; Leva, A. Di; Elekes, Z.; Fiore, E. M.; Formicola, A.; Fülöp, Zs.; Gervino, G.; Guglielmetti, A.; Gustavino, C.; Gyürky, Gy.; Imbriani, G.; Junker, M.; Karakas, Amanda I.; Kochanek, I.; Lugaro, Maria; Marigo, Paola; Menegazzo, R.; Mossa, V.; Pantaleo, F. R.; Paticchio, V.; Perrino, R.; Prati, P.; Schiavulli, L.; Stöckel, K.; Straniero, O.; Szücs, T.; Trezzi, D.; Zavatarelli, S.

doi:10.1103/physrevlett.121.172701

Cited by 33 publications

(18 citation statements)

References 44 publications

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“…This resonance was amongst the three low-energy resonances reported by the LUNA collaboration [20,48]. Here we report a strength value that lies between the first LUNA measurement and a more recent study by the LUNA group [29], thus supporting a larger strength than previous upper limits [26,52].…”

Section: E Resonance At E CM = 248 Kevsupporting

confidence: 83%

“…ωγ 149 = 0.17 ± 0.02 syst +0.04 −0.03 stat μeV is lower than those reported by TUNL [21] and both LUNA measurements [29,49]. It is perhaps worth noting that for the TUNL result, given that this was measured relative to the 458-keV resonance strength reported in Ref.…”

Section: G Resonance At E CM = 149 Kevmentioning

confidence: 50%

“…Screening enhancement factors are taken from Ref. [29]. 1 2 .7 ± 0.7 1 1 .7 ± 1.4 1 1 .7 ± 0.5 11.0 ± 1.0 [42] targeted by Depalo et al [42].…”

Section: Resonance At E CM = 610 Kevmentioning

confidence: 99%

“…These resonances have thus not been considered for both the reaction rates put forward by Kelly et al and the present work. It is perhaps unsurprising that a subsequent attempt by the LUNA collaboration to measure these resonances directly, using a γ -ray spectrometer composed of BGO instead of HPGe detectors, could not positively identify any yield from these resonances [29]. Although their newly obtained upper limits effectively remove the 100-keV resonance from contention as a significant contributor to the 22 Ne(p, γ ) 23 Na reaction rate, the 68-keV resonance remains a potential contributor, thus defining the upper limit of the new LUNA rate at temperatures below 0.1 GK.…”

Section: Introductionmentioning

confidence: 99%

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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: E Resonance At E CM = 248 Kevsupporting

confidence: 83%

Section: G Resonance At E CM = 149 Kevmentioning

confidence: 50%

“…Screening enhancement factors are taken from Ref. [29]. 1 2 .7 ± 0.7 1 1 .7 ± 1.4 1 1 .7 ± 0.5 11.0 ± 1.0 [42] targeted by Depalo et al [42].…”

Section: Resonance At E CM = 610 Kevmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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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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“…The ionization of the target gas and the neutralization of the beam prevent the electrical reading of the beam current and a power compensation calorimeter with a constant temperature gradient is used to monitor the beam intensity (Ferraro et al, 2018a;Ferraro et al, 2018b). For the proper characterization of a windowless gas target, the density and the efficiency of the detectors profile along the beam path must be known.…”

Section: The MV Facility At Gran Sassomentioning

confidence: 99%

The Study of Key Reactions Shaping the Post-Main Sequence Evolution of Massive Stars in Underground Facilities

Ferraro

Ciani

Boeltzig

et al. 2021

Front. Astron. Space Sci.

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The chemical evolution of the Universe and several phases of stellar life are regulated by minute nuclear reactions. The key point for each of these reactions is the value of cross-sections at the energies at which they take place in stellar environments. Direct cross-section measurements are mainly hampered by the very low counting rate and by cosmic background; nevertheless, they have become possible by combining the best experimental techniques with the cosmic silence of an underground laboratory. In the nineties, the LUNA (Laboratory for Underground Nuclear Astrophysics) collaboration opened the era of underground nuclear astrophysics, installing first a homemade 50 kV and, later on, a second 400 kV accelerator under the Gran Sasso mountain in Italy: in 25 years of experimental activity, important reactions responsible for hydrogen burning could have been studied down to the relevant energies thanks to the high current proton and helium beams provided by the machines. The interest in the next and warmer stages of star evolution (i.e., post-main sequence and helium and carbon burning) drove a new project based on an ion accelerator in the MV range called LUNA-MV, able to deliver proton, helium, and carbon beams. The present contribution is aimed to discuss the state of the art for some selected key processes of post-main sequence stellar phases: 12C(α,γ)16O and 12C+12C are fundamental for helium and carbon burning phases, and 13C(α,n)16O and 22Ne(α,n)25Mg are relevant to the synthesis of heavy elements in AGB stars. The perspectives opened by an underground MV facility will be highlighted.

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Nuclear Data Sheets for A=23

Basunia

Chakraborty

2021

Nuclear Data Sheets

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Direct Capture Cross Section and the Ep=71 and 105 keV Resonances in the Ne22

Cited by 33 publications

References 44 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

The Study of Key Reactions Shaping the Post-Main Sequence Evolution of Massive Stars in Underground Facilities

Nuclear Data Sheets for A=23

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