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

Wilds, E. L.; Jevtić, N.; McDonald, James E.; Gai, M.

doi:10.1016/s0375-9474(97)00231-5

Cited by 16 publications

(51 citation statements)

References 10 publications

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“…Two new measurements of the spectrum have recently been done at the University of Washington in Seattle (Zhao et al, 1995), and at Yale/UConn (France et al, 1997). These new measurements are said to agree well with each other, being as much as a factor of 2 higher than the TRIUMF data in the minimum between the two peaks.…”

Section: A Direct Measurementsmentioning

confidence: 90%

Synthesis of the elements in stars: forty years of progress

et al. 1997

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Forty years ago Burbidge, Burbidge, Fowler, and Hoyle combined what we would now call fragmentary evidence from nuclear physics, stellar evolution and the abundances of elements and isotopes in the solar system as well as a few stars into a synthesis of remarkable ingenuity. Their review provided a foundation for forty years of research in all of the aspects of low energy nuclear experiments and theory, stellar modeling over a wide range of mass and composition, and abundance studies of many hundreds of stars, many of which have shown distinct evidence of the processes suggested by B 2 FH. In this review we summarize progress in each of these fields with emphasis on the most recent developments. [S0034-6861(97)

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Section: A Direct Measurementsmentioning

confidence: 90%

Synthesis of the elements in stars: forty years of progress

et al. 1997

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“…But later it was shown by Hale [111] that the interpretation of the experimental data on the beta-delayed alpha-particle emission of 16 N is inconclusive and the astrophysical S-factor (S E1 ) is still ill determined by at least a factor of 4 and as much as a factor of 8. A recent measurement of the spectrum of beta-delayed alpha-particle emission of 16 N carried out at Argonne National Lab [112] was found to be in disagreement with the TRIUMF data [107,108], but in agreement with the Yale-UConn data [106,109,110]. This disagreement further complicates the attempt to indirectly extract the E1 astrophysical cross section factor (S E1 ) and mandates a direct measurement(s) of the cross section at low energies.…”

Section: Recent Measurements Of 12 C(α γ ) 16 Omentioning

confidence: 99%

Research opportunities at the upgraded HIγS facility

Weller

Ahmed

et al. 2009

Progress in Particle and Nuclear Physics

413

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“…The 16 N(βα) 12 C spectrum was concurrently measured by the Yale group, Zhao et al (1993). These measurements were subsequently extended by France III et al (1997). Another 16 N(βα) 12 C measurement was performed by the Seattle group shortly after but the results were not published.…”

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

confidence: 99%

“…V. However, the different spectra are can not be compared directly since all of them suffer from experimental resolution effects to different degrees. This point was the subject of an analysis by Gai (1998) where it was determined that the spectra of the Yale (France III et al, 1997), Seattle (unpublished), and Mainz (Hättig et al, 1970) groups were inconsistent with that of TRIUMF (Azuma et al, 1994). This began a long debate regarding the consistency between the data sets that still remains unresolved.…”

Section: β Delayed α Emissionmentioning

confidence: 99%

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

et al. 2017
Rev. Mod. Phys.
208
8
143
1
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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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Further measurement of the beta-delayed alpha-particle emission of 16N

Cited by 16 publications

References 10 publications

Synthesis of the elements in stars: forty years of progress

Synthesis of the elements in stars: forty years of progress

Research opportunities at the upgraded HIγS facility

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

et al. 2017
Rev. Mod. Phys.
208
8
143
1
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Further measurement of the beta-delayed alpha-particle emission of 16N

Cited by 16 publications

References 10 publications

Synthesis of the elements in stars: forty years of progress

Synthesis of the elements in stars: forty years of progress

Research opportunities at the upgraded HIγS facility

The C12(α,γ)O16deBoer1, Görres2, Wiescher3 et al. 2017Rev. Mod. Phys.20881431View full textAdd to dashboardCite

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

et al. 2017
Rev. Mod. Phys.
208
8
143
1
View full text Add to dashboard Cite