Toward precise<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:msub><mml:mi>Q</mml:mi><mml:mrow><mml:mi mathvariant="normal">EC</mml:mi></mml:mrow></mml:msub></mml:mrow></mml:math>values for the superallowed<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:msup><mml:mn>0</mml:mn><mml:mrow><mml:mo>+</mml:mo></mml:mrow></mml:msup><mml:mo>→</mml:mo><mml:msup><mml:mn>0</mml:mn><mml:mrow><mml:mo>+</mml:mo></mml:mrow></mml:msup></mml:

Wrede, C.; Clark, J. A.; Deibel, C. M.; Hertenberger, R.; Parikh, A.; Wirth, H.-F.; Bishop, S.; Chen, A. A.; Eppinger, K.; Garcı́a, A.; Krücken, R.; Lepyoshkina, O.; Rugel, G.; Setoodehnia, Kiana

doi:10.1103/physrevc.81.055503

Cited by 41 publications

(56 citation statements)

References 49 publications

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“…This thickness was determined to be 53 ± 5 µg/cm 2 through the reanalysis of the data of a previous scattering experiment [36], where an 8-MeV 4 He + beam along with the Enge spectrograph at WNSL and a silicon surface barrier detector were used to determine the composition and thickness of the CdS target. The theoretical angular distributions of the cross sections were then computed via (i) Distorted Wave Born Approximation (DWBA) calculations using the one-step finite range transfer formalism for the natural-parity states, and (ii) [14].…”

Section: Results: Both Phases Combinedmentioning

confidence: 99%

Nuclear structure of30S and its implications for nucleosynthesis in classical novae

Setoodehnia¹,

Chen²,

Kahl³

et al. 2013

Phys. Rev. C

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Background:The uncertainty in the 29 P(p, γ) 30 S reaction rate over 0.1 ≤ T ≤ 1.3 GK was previously determined to span ∼4 orders of magnitude due to the uncertain location of two previously unobserved 3 + and 2 + resonances in the E x = 4.7 -4.8 MeV region in 30 S. Therefore, the abundances of silicon isotopes synthesized in novae, which are relevant for the identification of presolar grains of putative nova origin, were uncertain by a factor of 3.

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Section: Results: Both Phases Combinedmentioning

confidence: 99%

Nuclear structure of30S and its implications for nucleosynthesis in classical novae

Setoodehnia¹,

Chen²,

Kahl³

et al. 2013

Phys. Rev. C

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“…The A = 32, T = 2 quintet is currently the most precisely measured quintent. Here, a precise Penning trap measurement of 32 Si [11] led to an observed breakdown of the IMME, requiring a small, but very significant, cubic term d = 1.00(9) keV, which was supported by a measurement of the 32 Cl mass using the 32 S( 3 He,t) 32 Cl reaction [12]. A later precision measurement of the 31 S mass [13] led to an even greater precision on the 32 Cl mass excess and found that no combination of various literature values could produce a fit that validated the IMME for the A = 32, T = 2 quintet.…”

Section: Introductionmentioning

confidence: 97%

Isobaric multiplet mass equation in theA=31,T=3/2quartets

Bennett¹,

Wrede²,

Brown³

et al. 2016

Phys. Rev. C

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Background: The observed mass excesses of analog nuclear states with the same mass number A and isospin T can be used to test the isobaric multiplet mass equation (IMME), which has, in most cases, been validated to a high degree of precision. A recent measurement (Kankainen et al., Phys. Rev. C 93 041304(R) (2016)) of the ground-state mass of 31 Cl led to a substantial breakdown of the IMME for the lowest A = 31, T = 3/2 quartet. The second-lowest A = 31, T = 3/2 quartet is not complete, due to uncertainties associated with the identity of the 31 S member state.Purpose: To populate the two lowest T = 3/2 states in 31 S and use the data to investigate the influence of isospin mixing on tests of the IMME in the two lowest A = 31, T = 3/2 quartets.Methods: Using a fast 31 Cl beam implanted into a plastic scintillator and a high-purity Ge γ-ray detection array, γ rays from the 31 Cl(βγ) 31 S sequence were measured. Shell-model calculations using USDB and the recently-developed USDE interactions were performed for comparison.Results: Isospin mixing between the 31 S isobaric analog state (IAS) at 6279.0(6) keV and a nearby state at 6390.2(7) keV was observed. The second T = 3/2 state in 31 S was observed at Ex = 7050.0(8) keV. Calculations using both USDB and USDE predict a triplet of isospin-mixed states, including the lowest T = 3/2 state in 31 P, mirroring the observed mixing in 31 S, and two isospin-mixed triplets including the second-lowest T = 3/2 states in both 31 S and 31 P.Conclusions: Isospin mixing in 31 S does not by itself explain the IMME breakdown in the lowest quartet, but it likely points to similar isospin mixing in the mirror nucleus 31 P, which would result in a perturbation of the 31 P IAS energy. USDB and USDE calculations both predict candidate 31 P states responsible for the mixing in the energy region slightly above Ex = 6400 keV. The second quartet has been completed thanks to the identification of the second 31 S T = 3/2 state, and the IMME is validated in this quartet.

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“…The two most recent measurements [4,9] produced values that differed from each other systematically in the region of astrophysical interest by about 4 keV. The earlier measurement [3,9,10] carried a combined statistical and systematic uncertainty of ≈ 0.5 keV.…”

Section: CL Excitation Energiesmentioning

confidence: 99%

“…[4] are systematically low and that the systematic effect increases in magnitude with increasing excitation energy (this increase may saturate). Such an increase could result from the fact that the lowest excitation energies were strongly influenced by internal 32 Cl calibration points and that the calibration gradually became more dependent on external calibration points towards higher energies [4], introducing substantial systematic uncertainties from the dependence on the assumed target properties [3,9,10] (primarily) and reaction Q values [9] (secondarily).…”

Section: CL Excitation Energiesmentioning

confidence: 99%

γ-ray constraints on the properties of unbound32Cl levels

et al. 2012

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Systematic differences between measurements of excitation energies and branching ratios of unbound 32 Cl levels near the proton threshold have recently emerged. We investigate these 32 Cl properties using independent information by analyzing existing 32 Ar(βγ) 32 Cl data and using published values from measurements of the 32 S( 3 He,tγ) 32 Cl reaction. Significant evidence emerges in support of particular values. The results increase the thermonuclear rate of the 31 S(p, γ) 32 Cl reaction by up to a factor of two over the temperature range of 0.4 to 2 GK that is reached during type I x-ray bursts on hydrogen-accreting neutron stars.

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Toward preciseQECvalues for the superallowed0+→0+

Cited by 41 publications

References 49 publications

Nuclear structure of30S and its implications for nucleosynthesis in classical novae

Nuclear structure of30S and its implications for nucleosynthesis in classical novae

Isobaric multiplet mass equation in theA=31,T=3/2quartets

γ-ray constraints on the properties of unbound32Cl levels

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