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Azuma, R.E.; Buchmann, L.; Barker, F.C.; Barnes, C. A.; D’Auria, J.M.; Dombsky, M.; Giesen, U.; Jackson, K. P.; King, J.D.; Korteling, R. G.; McNeely, P.; Powell, J.R.; Roy, G.; Vincent, J.; Wang, T. R.; Wong, S.S.M.; Wrean, P. R.

doi:10.1103/physrevc.56.1655

Cited by 24 publications

(37 citation statements)

References 9 publications

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“…It competes with the 8 Be(α, γ) 12 C reaction (that forms carbon) to yield oxygen during stellar helium burning, together determining the carbon/oxygen (C/O) ratio at the end of helium burning. The C/O ratio is of major importance for understanding type II [2] and apparently also the light curve of type Ia [3] supernovae.…”

Section: Introductionmentioning

confidence: 99%

Further measurement of the beta-delayed alpha-particle emission of 16N

et al. 1997

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Section: Introductionmentioning

confidence: 99%

Further measurement of the beta-delayed alpha-particle emission of 16N

et al. 1997

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“…Fig. 5 shows the fit to the normalized 16 N α spectrum together with the decomposition into p-and f-wave contributions, which suggests a significantly negative interference of the bound 1 surement of Azmua et al [27] most likely represents the currently closest approximation to the true α spectrum.…”

Section: Cmentioning

confidence: 99%

“…= 3 and 4 MeV, where the calculation underestimates total cross-section. The latest results of [27], and Zhao 1993: [28], together with the decomposition into p-(dashed line) and f-wave (dotted line) contributions. For comparison, the best fits of Tang 2010: [26], Azuma 1994: [27], and Schürmann 2012: [40] scaled by the corresponding coefficients are shown.…”

Section: B Total S Factormentioning

confidence: 99%

“…Included in this analysis are the three independent α spectra data of Refs. [25][26][27][28], and the normalization for probability spectrum is used in the practice to reduce the influence of systematical errors. Fig.…”

Section: Cmentioning

confidence: 99%

“…To investigate the specific role of the 16 O nucleus for the S factor, a wealth of experimental data have been accumulated over the past few decades, including the precise measurements of total cross-section of 12 C(α, γ) 16 O [7][8][9][10], γ-ray angular distributions of ground state transition [11][12][13][14][15][16][17][18][19][20][21][22], cascade transitions [8,12,23,24], β-delayed α spectra for 16 N [25][26][27][28], transfer reaction [29][30][31], elastic scattering 12 C(α, α) 12 C [32][33][34][35][36] and additional particle reaction 16±16 Kunz [15] 165±50 76±20 85±30 4±4 Brune [29] 159 101±17 42…”

Section: Introductionmentioning

confidence: 99%

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AstrophysicalSfactor of theC12(α,γ)O16
An
¹
,
Chen
²
,
Ma
³

et al. 2015
Phys. Rev. C
23
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8
0
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Determination of the accurate astrophysical S factor of 12 C(α, γ) 16 O reaction has been regarded as a holy grail of nuclear astrophysics for decades. In current stellar models, a knowledge of that value to better than 10% is desirable. Due to the practical issues, tremendous experimental and theoretical efforts over nearly 50 years are not able to reach this goal, and the published values contradicted with each other strongly and their uncertainties are 2 times larger than the required precision. To this end we have developed a Reduced R-matrix Theory, based on the classical Rmatrix theory of Lane and Thomas, which treats primary transitions to ground state and four bound states as the independent reaction channels in the channel spin representation. With the coordination of covariance statistics and error propagation theory, a global fitting for almost all available experimental data of 16 O system has been multi-iteratively analyzed by our powerful code. A reliable, accurate and self-consistent astrophysical S factor of 12 C(α, γ) 16 O was obtained with a recommended value Stot (300) = 162.7 ± 7.3 keV b (4.5%) which could meet the required precision.

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