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Vernotte, J.; Khendriche, A.; Berrier-Ronsin, G.; Grafeuille, S.; Kalifa, J.; Rotbard, G.; Tamisier, R.; Wildenthal, B. H.

doi:10.1103/physrevc.41.1956

Cited by 31 publications

(62 citation statements)

References 25 publications

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“…Sources of uncertainty on spectroscopic factors are statistics (negligible), normalization to elastic scattering data (≈ 10 %) but the major one is the DWBA method itself. This last one is difficult to evaluate but using statistics of ratios between the directly measured proton widths and the ones extracted from a DWBA analysis [12], we estimate this error to 25% (r.m.s.) for spectroscopic factors greater than 0.01.…”

Section: Forward Center-of-mass Angles Between 12mentioning

confidence: 99%

2H(18F,pα)15
Séréville
¹
,
Coc
²
,
Angulo
³

et al. 2003
Phys. Rev. C
46
3
27
0
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The 18 F(p,α) 15 O reaction is recognized to be one of the most important reactions for nova gammaray astronomy as it governs the early E ≤ 511 keV gamma emission. However in the nova temperature regime, its rate remains largely uncertain due to unknown low-energy resonance strengths. We report here the measurement of the D( 18 F,p) 19 F(α) 15 N one-nucleon transfer reaction, induced by a 14 MeV 18 F radioactive beam impinging on a CD2 target; outgoing protons and 15 N (or α-particles) were detected in coincidence in two silicon strip detectors. A DWBA analysis of the data resulted in new limits to the contribution of low-energy resonances to the rate of the 18 F(p,α) 15 O reaction.

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Section: Forward Center-of-mass Angles Between 12mentioning

confidence: 99%

2H(18F,pα)15
Séréville
¹
,
Coc
²
,
Angulo
³

et al. 2003
Phys. Rev. C
46
3
27
0
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show abstract

“…In Table III the exit channel parameters used for the calculations from Daehnick et al [10] are denoted as sets D0, D1, D2, and D3 for the ground state 20 Ne. The black solid curve is generated by the optical potential set FT and the black dashed curve by T. Potentials are given in Table I. and first three excited states, respectively, and similarly as V0, V1, V2, and V3 for parameters from Vernotte et al [11]. The angular distributions corresponding to the four states in 21 Na calculated with different combinations of the optical-model parameters are given in Fig.…”

Section: Optical-model Potentials and Distorted-wave Born Approxmentioning

confidence: 99%

“…Optical-model parameters used for the output channel are given in Table II. They were calculated from the global formulas derived by Daehnick et al [10], set D, and Vernotte et al [11], set V.…”

Section: Optical-model Potentials and Distorted-wave Born Approxmentioning

confidence: 99%

Asymptotic normalization coefficients from theNe20(He3
Mukhamedzhanov
¹
,
Bém
²
,
Burjan
³

et al. 2006
Phys. Rev. C
27
2
32
0
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The 20 Ne(p, γ ) 21 Na reaction rate at stellar energies is dominated by capture to the ground state through the tail of a subthreshold resonance state at an excitation energy of 2425 keV in 21 Na. Both resonant and direct capture contribute to the reaction rate while direct captures to other bound states are negligible. The overall normalization of direct capture to the subthreshold state is determined by the asymptotic normalization coefficient (ANC). Simultaneously this ANC determines the proton partial width of the subthreshold resonance state. To determine the ANC, the 20 Ne( 3 He, d) 21 Na proton transfer reaction has been measured, at an incident energy of 25.83 MeV. Angular distributions for proton transfer to the ground and first three excited states were measured, and ANCs were then extracted from comparison with distorted-wave Born approximation calculations. Using these ANCs, we calculated the astrophysical factor for 20 Ne(p, γ ) 21 Na. Our total astrophysical factor is S(0) = 5900 ± 1200 keV b. Our analysis confirms that only nonresonant and resonant captures through the subthreshold state are important.

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“…To date, this is the lowest-lying, directly observed resonance in this reaction. For the E cm R = 439.1 keV resonance, the proton partial width, Γ p , was determined indirectly via the 30 Si( 3 He, d) 31 P reaction (Vernotte et al 1990). The other three resonances, E cm R = 144.3, 169.1, and 418.1 keV, have not yet been measured.…”

Section: 1mentioning

confidence: 99%

Sensitivity to Thermonuclear Reaction Rates in Modeling the Abundance Anomalies of NGC 2419

Dermigny

Iliadis

2017

ApJ

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Abundance anomalies in globular clusters provide strong evidence for multiple stellar populations within each cluster. These populations are usually interpreted as distinct generations, with the currently observed second-generation stars having formed in part from the ejecta of massive, firstgeneration "polluter" stars, giving rise to the anomalous abundance patterns. The precise nature of the polluters and their enrichment mechanism are still unclear. Even so, the chemical abundances measured in second-generation stars within the globular cluster NGC 2419 provide insight into this puzzling process. Previous work used Monte Carlo nuclear reaction network calculations to constrain the temperature-density conditions that could reproduce the observed abundances, thereby placing robust limits on the origins of the polluter material. The effect of individual reaction rates on these conditions has not been studied, however. Thus, we perform an exhaustive sensitivity study on the nuclear physics input to determine which reactions have the greatest impact on these predictions. We find that the 30 Si(p,γ) 31 P, 37 Ar(p,γ) 38 K, 38 Ar(p,γ) 39 K, and 39 K(p,γ) 40 Ca reactions are all critical in determining the temperature-density conditions, and ultimately, the origin of the polluter material. We conclude with recommendations for future experiments.

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Si30(3He,

Cited by 31 publications

References 25 publications

2H(18F,pα)15
Séréville
¹
,
Coc
²
,
Angulo
³

et al. 2003
Phys. Rev. C
46
3
27
0
View full text Add to dashboard Cite

2H(18F,pα)15
Séréville
¹
,
Coc
²
,
Angulo
³

et al. 2003
Phys. Rev. C
46
3
27
0
View full text Add to dashboard Cite

Asymptotic normalization coefficients from theNe20(He3
Mukhamedzhanov
¹
,
Bém
²
,
Burjan
³

et al. 2006
Phys. Rev. C
27
2
32
0
View full text Add to dashboard Cite

Sensitivity to Thermonuclear Reaction Rates in Modeling the Abundance Anomalies of NGC 2419

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Si30(3He,

Cited by 31 publications

References 25 publications

2H(18F,pα)15Séréville1, Coc2, Angulo3 et al. 2003Phys. Rev. C463270View full textAdd to dashboardCite

2H(18F,pα)15Séréville1, Coc2, Angulo3 et al. 2003Phys. Rev. C463270View full textAdd to dashboardCite

Asymptotic normalization coefficients from theNe20(He3Mukhamedzhanov1, Bém2, Burjan3 et al. 2006Phys. Rev. C272320View full textAdd to dashboardCite

Sensitivity to Thermonuclear Reaction Rates in Modeling the Abundance Anomalies of NGC 2419

Contact Info

Product

Resources

About

2H(18F,pα)15
Séréville
¹
,
Coc
²
,
Angulo
³

et al. 2003
Phys. Rev. C
46
3
27
0
View full text Add to dashboard Cite

2H(18F,pα)15
Séréville
¹
,
Coc
²
,
Angulo
³

et al. 2003
Phys. Rev. C
46
3
27
0
View full text Add to dashboard Cite

Asymptotic normalization coefficients from theNe20(He3
Mukhamedzhanov
¹
,
Bém
²
,
Burjan
³

et al. 2006
Phys. Rev. C
27
2
32
0
View full text Add to dashboard Cite