Determination of the<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mi>E</mml:mi><mml:mn>1</mml:mn></mml:mrow></mml:math>component of the low-energy<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mmultiscripts><mml:mi mathvariant="normal">C</mml:mi><mml:mprescripts /><mml:none /><mml:mrow><mml:mn>12</mml:mn></mml:mrow></mml:mmultiscripts></mml:math>(<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mm

Tang, Xiaodong; Rehm, K. E.; Ahmad, I.; Brune, C. R.; Champagne, Arthur E; Greene, J. P.; Hecht, A. A.; Henderson, D. J.; Janssens, R. V. F.; Jiang, C. L.; Jisonna, L.; Kahl, D.; Moore, E. F.; Notani, M.; Pardo, R. C.; Patel, N.; Paul, M.; Savard, G.; Schiffer, J. P.; Segel, R. E.; Sinha, S.; Wuosmaa, A. H.

doi:10.1103/physrevc.81.045809

Cited by 43 publications

(69 citation statements)

References 47 publications

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“…The χ 2 value of the Tang et al (2010) data decreased substantially, demonstrating the tension between the two data sets. It is interesting to note that the χ 2 of the fit to the data of Azuma et al (1994) actually becomes larger.…”

Section: Refmentioning

confidence: 96%

“…Another measurement of the 16 N(βα) 12 C spectrum was made soon after at Argonne National Laboratory by Tang et al (2010). This experiment attempted to lessen the effects of β background and contaminant reactions by using the in-flight technique (Harss et al, 2000) to create the 16 N beam.…”

Section: Return To Indirect Techniques ('93-present)mentioning

confidence: 99%

“…16 N(βα) 12 C spectra for Azuma et al (1994) and Tang et al (2010). For the other measurements, the convolution parameters are estimated from the best fits to the data of Azuma et al (1994) and Tang et al (2010).…”

Section: Table IX Summary Of Convolution and Energy Shift Correctionsmentioning

confidence: 99%

“…σ ( For the current analysis, because of the above issues, the data are limited to that of Azuma et al (1994) and Tang et al (2010). These data sets have the most detailed documentation of how to simulate their remaining resolution effects and claim that they can be accurately done so using the simple method given by Eq.…”

Section: Refmentioning

confidence: 99%

“…A comparison is made using the best fit parameters from the simultaneous fit to the data of Azuma et al (1994) and Tang et al (2010) with the remaining data sets from the Mainz, Seattle, and Yale experiments, where the data have been taken from France III et al (2007). Since these three data sets retain significant experimental effects, the convolution value of each data set was varied while the R-matrix parameters where kept constant.…”

Section: Refmentioning

confidence: 99%

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The C12(α,γ)O16
deBoer
¹
,
Görres
²
,
Wiescher
³

et al. 2017
Rev. Mod. Phys.
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The creation of carbon and oxygen in our universe is one of the forefront questions in nuclear astrophysics. The determination of the abundance of these elements is key to both our understanding of the formation of life on earth and to the life cycles of stars. While nearly all models of different nucleosynthesis environments are affected by the production of carbon and oxygen, a key ingredient, the precise determination of the reaction rate of 12 C(α, γ) 16 O, has long remained elusive. This is owed to the reaction's inaccessibility, both experimentally and theoretically. Nuclear theory has struggled to calculate this reaction rate because the cross section is produced through different underlying nuclear mechanisms. Isospin selection rules suppress the E1 component of the ground state cross section, creating a unique situation where the E1 and E2 contributions are of nearly equal amplitudes. Experimentally there have also been great challenges. Measurements have been pushed to the limits of state of the art techniques, often developed for just these measurements. The data have been plagued by uncharacterized uncertainties, often the result of the novel measurement techniques, that have made the different results challenging to reconcile. However, the situation has markedly improved in recent years, and the desired level of uncertainty, ≈10%, may be in sight. In this review the current understanding of this critical reaction is summarized. The emphasis is placed primarily on the experimental work and interpretation of the reaction data, but discussions of the theory and astrophysics are also pursued. The main goal is to summarize and clarify the current understanding of the reaction and then point the way forward to an improved determination of the reaction rate.

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Section: Refmentioning

confidence: 96%

Section: Return To Indirect Techniques ('93-present)mentioning

confidence: 99%

Section: Table IX Summary Of Convolution and Energy Shift Correctionsmentioning

confidence: 99%

Section: Refmentioning

confidence: 99%

Section: Refmentioning

confidence: 99%

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The C12(α,γ)O16
deBoer
¹
,
Görres
²
,
Wiescher
³

et al. 2017
Rev. Mod. Phys.
190
8
143
1
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show abstract

Weak Interference Between the 1 $$^-$$ States in the Vicinity of $$\alpha $$ -Particle Threshold of $$^{16}$$ O

Katsuma

2019

Springer Proceedings in Physics

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The subthreshold 1 − 1 state at an excitation energy Ex = 7.12 MeV in 16 O has been believed to enhance the S-factor of 12 C(α,γ) 16 O. The enhancement seems to originate from strong interference between 1 − 1 and 1 − 2 (Ex ≈ 9.6 MeV) in the vicinity of the α-particle threshold. However, weak interference between them and a resulting small E1 Sfactor are exemplified with R-matrix theory. Including a higher-order correction of the resonance parameters, the present example appears to reproduce the experimental data consistently. It would therefore be possible that the E1 S-factor is reduced at low energies.

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Calculable Microscopic Theory for $$^{12}$$C($$\alpha , \gamma $$)$$^{16}$$O Cross Section near Gamow Window

Suzuki

2021

Few-Body Syst

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Determination of theE1component of the low-energyC12(

Cited by 43 publications

References 47 publications

The C12(α,γ)O16
deBoer
¹
,
Görres
²
,
Wiescher
³

et al. 2017
Rev. Mod. Phys.
190
8
143
1
View full text Add to dashboard Cite

The C12(α,γ)O16
deBoer
¹
,
Görres
²
,
Wiescher
³

et al. 2017
Rev. Mod. Phys.
190
8
143
1
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Weak Interference Between the 1 $$^-$$ States in the Vicinity of $$\alpha $$ -Particle Threshold of $$^{16}$$ O

Calculable Microscopic Theory for $$^{12}$$C($$\alpha , \gamma $$)$$^{16}$$O Cross Section near Gamow Window

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Determination of theE1component of the low-energyC12(

Cited by 43 publications

References 47 publications

The C12(α,γ)O16deBoer1, Görres2, Wiescher3 et al. 2017Rev. Mod. Phys.19081431View full textAdd to dashboardCite

The C12(α,γ)O16deBoer1, Görres2, Wiescher3 et al. 2017Rev. Mod. Phys.19081431View full textAdd to dashboardCite

Weak Interference Between the 1 $$^-$$ States in the Vicinity of $$\alpha $$ -Particle Threshold of $$^{16}$$ O

Calculable Microscopic Theory for $$^{12}$$C($$\alpha , \gamma $$)$$^{16}$$O Cross Section near Gamow Window

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Resources

About

The C12(α,γ)O16
deBoer
¹
,
Görres
²
,
Wiescher
³

et al. 2017
Rev. Mod. Phys.
190
8
143
1
View full text Add to dashboard Cite

The C12(α,γ)O16
deBoer
¹
,
Görres
²
,
Wiescher
³

et al. 2017
Rev. Mod. Phys.
190
8
143
1
View full text Add to dashboard Cite