Gamma decay in 19Ne

Davidson, J. M.; Roush, M.L.

doi:10.1016/0375-9474(73)90154-1

Cited by 14 publications

(24 citation statements)

References 8 publications

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“…The dashed and dotted lines in Fig. 3 The dot-dashed line simulates the peak shape for a 50-fs lifetime, corresponding to the upper limit from previous measurements [18] and very close to the suggested value in Ref. [19].…”

supporting

confidence: 86%

“…The dot-dashed line represents the previous upper limit of 50 fs set by Ref. [18], which is too broad and unable to account for both the peak height and the low-energy tail. The fit to the high-energy tailing or shoulder of the data is not sensitive to the input lifetime since it does not originate from the Doppler-shifted spectrum of 4.03 → 0 but results from the small contribution from the nearby single escape peak of the transition 4.55 → 0, which happens to hide the otherwise more pronounced asymmetry of the 4.03 → 0 line shape resulting from the Doppler effects.…”

mentioning

confidence: 98%

“…Previous attempts to determine the lifetimes have provided only upper limits for the lifetimes of the unbound states near the α threshold (see the TUNL compilation of Ref. [17]) with the Doppler-shift attenuation method (DSAM) [18]. A recent approach of a direct measurement of the lifetimes made using the the Coulomb excitation technique resulted only in an lower limit of 1.5 fs for the lifetime of the 4.03-MeV level [19].…”

mentioning

confidence: 99%

“…In less extreme cases such as the transition 1.62 → 0.28, the broadened peak shows a significant low-energy tailing down to about the unshifted γ energy. The simple DSAM approach [18,[20][21][22] widely used in the lifetime measurements takes into account only the Doppler shift of peak centroids and, therefore, is insufficient to study these cases. In this work, the improved DSAM is applied with full line-shape analysis using GEANT4 [23] simulation, which will be discussed later.…”

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confidence: 99%

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Lifetime of the astrophysically important 4.03-MeV state inNe19

et al. 2005

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The 15 O(α, γ ) 19 Ne reaction is one of the most important breakout reactions for the hot CNO cycles. However, the relevant states in 19 Ne at excitation energies of 4-5 MeV have not been well studied. The lifetimes of these states are not known and are only constrained by experimental upper and lower limits. In particular, accurate knowledge of the γ -and α-decay widths of the 4.03-MeV state of 19 Ne is important, since the resonance strength of this level dominates the reaction rate for the astrophysically relevant temperatures T 9 < 0.6. In this work, we employed an improved Doppler-shifted attenuation method to obtain lifetime values of this and other states via 17 O( 3 He, n-γ ) 19 Ne. For the 4.03-MeV state, the measured excitation energy is 4034.5 ± 0.8 keV and the mean lifetime, measured here for the first time, is 13 +9 −6 fs at the confidence level of 1σ and 13 +16 −9 fs at the confidence level of 2σ . This result is in excellent agreement with the 9-fs prediction by Langanke, Wiescher, Fowler, and Görres.

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supporting

confidence: 86%

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confidence: 98%

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confidence: 99%

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confidence: 99%

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Lifetime of the astrophysically important 4.03-MeV state inNe19

et al. 2005

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“…It has three decay branches [10,30]: an (80 ± 15)% branch to the ground state, a (15 ± 5)% branch to the level at 1536 keV, and a (5 ± 5)% branch to the level at 275 keV. The two strong transitions from this state were observed in this experiment.…”

Section: B the 3/2 + State At 4035 Kevmentioning

confidence: 48%