The probability for transitions between the first 2+ and the first 0+ excited states of O16

Fuchs, H.; Hagemann, K.A.; Gaarde, C.

doi:10.1016/0029-5582(65)90791-1

Cited by 12 publications

(2 citation statements)

References 5 publications

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“…Interest in the measurement has been heightened by detailed theoretical work to which we refer later. Two further measurements have appeared 6,7 giving values of R in essential agreement with our figure, confirming that the transition is strongly enhanced. We have nevertheless thought it worthwhile to repeat our experiment in essentially the same conditions and by the same method as before since the experiment is somewhat delicate, uses a different technique from the other workers, and the result is of some importance.…”

supporting

confidence: 90%

6.92- to 6.05-MeVE2Transition inO16

1966

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supporting

confidence: 90%

6.92- to 6.05-MeVE2Transition inO16

1966

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“…Past measurements of the different cascade γ rays have been made by Fuchs et al (1965); Lowe et al (1967); Miska et al (1975);and Wilkinson et al (1968). A recent measurement by Matei et al (2008) investigated the branching ratios of the decay from E x = 7.12 MeV state, giving a more accurate value for the branching to the E x = 6.13 MeV state and an upper limit to the E x = 6.92 MeV state.…”

Section: Omentioning

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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The Giant Dipole Resonance

Spicer¹

1969

Advances in Nuclear Physics

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The probability for transitions between the first 2+ and the first 0+ excited states of O16

Cited by 12 publications

References 5 publications

6.92- to 6.05-MeVE2Transition inO16

6.92- to 6.05-MeVE2Transition inO16

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

The Giant Dipole Resonance

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The probability for transitions between the first 2+ and the first 0+ excited states of O16

Cited by 12 publications

References 5 publications

6.92- to 6.05-MeVE2Transition inO16

6.92- to 6.05-MeVE2Transition inO16

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

The Giant Dipole Resonance

Contact Info

Product

Resources

About

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