Matter radii of<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:msup><mml:mrow /><mml:mrow><mml:mn>29</mml:mn><mml:mo>–</mml:mo><mml:mn>35</mml:mn></mml:mrow></mml:msup></mml:math>Mg

Fortune, H. T.; Sherr, R.

doi:10.1103/physrevc.86.064322

Cited by 3 publications

(2 citation statements)

References 25 publications

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“…A simple phenomenological approach [25] using two level mixing between pure 3p-3h and 1p-1h states have been used to determine the extent of configuration mixing existing in the states near the band crossing. In this calculation the 19/2 − state has been assumed to be a 3p-3h state (100%) with no mixing from 1p-1h (0%).…”

Section: Gamma Energy (Kev) Angular Momentum (I)mentioning

confidence: 99%

Superdeformation andα-cluster structure in35Cl

Bisoi¹,

Sarkar²,

Sarkar³

et al. 2013

Phys. Rev. C

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A superdeformed (SD) band has been identified in a non -alpha -conjugate nucleus 35 Cl. It crosses the negative parity ground band above 11/2 − and becomes the yrast at 15/2 − . Lifetimes of all relevant states have been measured to follow the evolution of collectivity. Enhanced B(E2), B(E1) values as well as energetics provide evidences for superdeformation and existence of parity doublet cluster structure in an odd-A nucleus for the first time in A≃ 40 region. Large scale shell model calculations assign (sd) 16 ( The superdeformed bands observed in the even-even nuclei in upper sd shell have provided favourable condition to describe the collective rotation microscopically involving the cross-shell correlations [1,2]. Complementary descriptions in terms of particle-hole excitations in the shell model [2,3], and α-clustering configurations within various cluster models [4][5][6] have been utilised to interpret the data. Till now no such band has been observed in non -alpha -conjugate odd-A, N =Z isotopes in this region [7]. If a nucleus clusterizes into fragments of different charge to mass ratios, the center of mass does not coincide with its center of charge. As a result a sizeable static E1 moment may arise in the intrinsic frame [8], resulting in several distinctive features in the spectra. Two adjacent opposite parity deformed ∆I = 2 bands connected by strong E2 intra-band transitions in turn are connected by strong E1 inter-band transitions [8] forming an apparent ∆I = 1 rotational band with alternating parity states. Since early seventies [9][10][11], a number of similar alpha-cluster bands have been studied extensively. In the spectrum of 19 F , cluster-model calculations have shown that coupling of a proton hole in the p shell coupled with four nucleons in the sd shell (a proton hole coupled to 20 N e) gives rise to alpha-cluster bands. The lowest alpha + 15 N parity partner bands built on K π = 1/2 + ground-state band, lowest lying famous K π = 1/2 − at 110 keV and some other bands lying above 5 MeV have been observed. So far no similar clustering have been observed in odd A nuclei in the A≃ 40 region, where evidences of clustering have been manifested in even-even nuclei through superdeformation.According to Ikeda [12], in the spectra of light nuclei, cluster like configurations would appear near the threshold energy needed for breakup into proper sub-nuclei. For the nucleus of our interest 35 Cl, the threshold energy [13] to appear as a composite of 32 S and a triton (t) ( 32 S + t) is around 18 MeV. On the other hand, threshold for the decay of the composite system 35 Cl into ( 31 P + α) clusters is around 6.5 MeV. The SD rotational band observed in 36 Ar has been shown to have cluster structure. So one may expect to find deformed cluster bands in the excitation spectra of 35 Cl also generated by coupling a proton hole to SD states in 36 Ar. In this letter, we report the observation of a superdeformed band for the first time in the odd A 35 Cl isotope. The reduced transition probabilities for all...

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Section: Gamma Energy (Kev) Angular Momentum (I)mentioning

confidence: 99%

Superdeformation andα-cluster structure in35Cl

Bisoi¹,

Sarkar²,

Sarkar³

et al. 2013

Phys. Rev. C

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“…6. 14 O(α, p) 17 F was decreased by a factor of 10 based roughly on the systematic change in the reaction rate caused by assuming constructive or destructive interference between resonances (Hu et al 2014) and on the fact that some disagreement exists as to relevant resonance properties (Fortune 2012). This reaction connects hot CNO cycles, speeding up the breakout process marking burst ignition.…”

mentioning

confidence: 99%

Influence of Nuclear Reaction Rate Uncertainties on Neutron Star Properties Extracted from X-Ray Burst Model–Observation Comparisons

Meisel

Merz

Medvid

2019

ApJ

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Type-I X-ray bursts can be used to determine properties of accreting neutron stars via comparisons between model calculations and astronomical observations, exploiting the sensitivity of models to astrophysical conditions. However, the sensitivity of models to nuclear physics uncertainties calls into question the fidelity of constraints derived in this way. Using X-ray burst model calculations performed with the code MESA, we investigate the impact of uncertainties for nuclear reaction rates previously identified as influential and compare them to the impact of changes in astrophysical conditions, using the conditions that are thought to best reproduce the source GS 1826-24 as a baseline. We find that reaction rate uncertainties are unlikely to significantly change conclusions about the properties of accretion onto the neutron star surface for this source. However, we find that reaction rate uncertainties significantly hinder the possibility of extracting the neutron star mass-radius ratio by matching the modeled and observed light curves due to the influence of reaction rates on the modeled light curve shape. Particularly influential nuclear reaction rates are 15 O(α, γ) and 23 Al(p, γ), though other notable impacts arise from 14 O(α, p), 18 Ne(α, p), 22 Mg(α, p), 24 Mg(α, γ), 59 Cu(p, γ), and 61 Ga(p, γ). Furthermore, we find that varying some nuclear reaction rates within their uncertainties has an impact on the neutron star crust composition and thermal structure that is comparable to relatively significant changes accretion conditions. arXiv:1812.07155v1 [astro-ph.HE]

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Matter radii of N16−23

Fortune

2018

Phys. Rev. C

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Matter radii of29–35Mg

Cited by 3 publications

References 25 publications

Superdeformation andα-cluster structure in35Cl

Superdeformation andα-cluster structure in35Cl

Influence of Nuclear Reaction Rate Uncertainties on Neutron Star Properties Extracted from X-Ray Burst Model–Observation Comparisons

Matter radii of N16−23

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