Widths of astrophysically important resonances in<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:msup><mml:mrow /><mml:mrow><mml:mn>18</mml:mn></mml:mrow></mml:msup></mml:mrow><mml:mi mathvariant="normal">Ne</mml:mi></mml:math>

Harss, B.; Jiang, C. L.; Rehm, K. E.; Schiffer, J. P.; Caggiano, J. A.; Collon, P.; Greene, J. P.; Henderson, D. J.; Heinz, A.; Janssens, R. V. F.; Nolen, J.A.; Pardo, R. C.; Pennington, T.; Siemssen, R.H.; Sonzogni, A. A.; Uusitalo, J.; Wiedenhöver, I.; Paul, M.; Wang, T. F.; Borasi, F.; Segel, R. E.; Blackmon, J. C.; Smith, M. S.; Chen, A.; Parker, P. D.

doi:10.1103/physrevc.65.035803

Cited by 36 publications

(59 citation statements)

References 12 publications

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“…Inverse-kinematics resonant proton scattering measurements have been performed, for example, with the thick-target technique at the TUDA facility at TRIUMF/ISAC, 21 Na + p [369,370] and 20 Na + p [371]; with the thin and thick-target approach at HRIBF/ORNL, 17 F + p [366,367] and 18 F + p [347,372]; at Louvain-la-Neuve with the thick-target technique, 13 [383]; as well as at Texas A&M [384,382], Notre Dame [385,386], ANL [387] and Spiral/GANIL [388].…”

Section: Resonance Properties From Elastic and Inelastic Scattering Ementioning

confidence: 99%

Nuclear astrophysics with radioactive beams

2010

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a b s t r a c tThe quest to comprehend how nuclear processes influence astrophysical phenomena is driving experimental and theoretical research programs worldwide. One of the main goals in nuclear astrophysics is to understand how energy is generated in stars, how elements are synthesized in stellar events and what the nature of neutron stars is. New experimental capabilities, the availability of radioactive beams and increased computational power paired with new astronomical observations have advanced the present knowledge. This review summarizes the progress in the field of nuclear astrophysics with a focus on the role of indirect methods and reactions involving beams of rare isotopes.

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Section: Resonance Properties From Elastic and Inelastic Scattering Ementioning

confidence: 99%

Nuclear astrophysics with radioactive beams

2010

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“…The 3 − α-cluster states in 16 O and 20 Ne are members of the well known α-cluster rotational bands with negative parity and with 1 − states as the band heads. The band head is 2 MeV below the 3 − state in 16 O and 1.3 MeV in 20 Ne. Presumably, this difference is proportional to the square root of the effective radii of the systems.…”

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confidence: 99%

“…Some progress in the study of the states with a lower excitation energy could be made with a longer experiment or through the use of the 17 F(p, α) reaction [20]. However results for the lowest relevant energies still will be difficult to obtain by these techniques involving beams of the radioactive nuclei.…”

mentioning

confidence: 99%

“…Still it is important in providing for the dimensionless reduced α particle width of 0.017 ± 0.03 [8,17,18] for the 7.12 MeV state (and also corresponding interference). The 14 O(α, p) reaction, involving the 18 Ne states near the α particle threshold (5.1 MeV), is an important issue in nuclear astrophysics [19,20] 14 O reaction [20] using a radioactive 17 F beam gave 0.04(+0.05; −0.025) for the reduced width in question at the same as in [17], 6.5 fm, channel radius. We believe that the accumulation of similar data will allow the possibility of predicting the α-cluster widths for experimentally difficult cases just as is done for single particle widths.…”

mentioning

confidence: 99%

“…There are well known [16]3 − α-cluster states in the nearby self-conjugate nuclei 16 O (E ex = 11.6 MeV), and 20 Ne (E ex = 7.2 MeV). The excitation energy of the level in 18 Ne is just in between these two values.…”

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confidence: 99%

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First observation ofα-cluster states in the14O + 4
Fu
¹
,
Goldberg
²
,
Rogachev
³

et al. 2008
Phys. Rev. C

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We measured 14 O + 4 He excitation functions for elastic scattering which demonstrate, for the first time, a well developed α-cluster structure in the proton rich nucleus, 18 Ne. We present the excitation energies and estimates of the spins for the dominant resonances using an R-matrix approach. A resonance at 9.2 MeV excitation energy in 18 Ne is particularly interesting. The spin-parity of the state is found to be 3 − and the α particle reduced width for the state appears to be comparable to the single particle limit. We have found indications for unusually large size of the observed α-cluster configuration. [2,3] have suggested that clustering remains in systems composed of a collection of α particles and valence nucleons. The available data on the α-cluster states in neutron rich nuclei are scarce [4][5][6][7], but they give indications for the developed cluster structures with very large moments of inertia. The study of non-self-conjugate nuclei has an advantage in that one can investigate isobaric analog states in mirror systems. Comparison of the results for both systems can bring new spectroscopic information and shed light on such properties as the radii of the cluster states. At present the data on the α-cluster states in proton rich nuclei are absent. There is no clear understanding of what will happen to cluster structure when valence protons are substituted for valence neutrons [3].α clustering may play a role in helium burning in astrophysical systems. Indeed, even if astrophysical reactions involving helium do not proceed through strong α-cluster states (because of high excitation energy), these states can provide an α width to the states that are closer to the region of astrophysical interest through configuration mixing [8]. For many systems, the information needed to understand this can be obtained only in the reactions induced by radioactive beams. This paper presents the first results on α-cluster states in 18

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