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Bennett, Michael B.; Wrede, C.; Brown, B. A.; Liddick, S. N.; Pérez–Loureiro, D.; Bardayan, D. W.; Chen, A. A.; Chipps, K. A.; Fry, C.; Glassman, Brent; Langer, C.; Larson, N.; McNeice, E.; Meisel, Z.; Ong, Wei Jia; O’Malley, P. D.; Pain, S. D.; Prokop, C. J.; Schatz, H.; Schwartz, Sanford; Suchyta, S.; Thompson, P.; Walters, Matthew; Xu, Xing

doi:10.1103/physrevlett.116.102502

Cited by 36 publications

(32 citation statements)

References 42 publications

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“…So far, only A = 9 [16], A = 35 [20], A = 53 [21], and recently A = 21 [17], of the known T = 3/2 quartets have shown significant nonzero a The parameter uncertainty has been scaled with χ 2 n . b During the review process, E x = 6279.0(6) keV [59] for the IAS in 31 S was published. The new value, which differs 2.6σ from Ref.…”

Section: M(at T Z ) = A(at ) + B(at )T Z + C(at )Tmentioning

confidence: 99%

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Mass of astrophysically relevantCl31and the breakdown of the isobaric multiplet mass equation

et al. 2016

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The mass of 31 Cl has been measured with the JYFLTRAP double Penning trap mass spectrometer at the Ion Guide Isotope Separator On-Line (IGISOL) facility. The determined mass-excess value, −7034.7(34) keV, is 15 times more precise than in the Atomic Mass Evaluation 2012. The quadratic form of the isobaric multiplet mass equation for the T = 3/2 quartet at A = 31 fails (χ 2 n = 11.6) and a non-zero cubic term, d = −3.5(11) keV, is obtained when the new mass value is adopted. 31 Cl has been found to be less proton-bound with a proton separation energy of Sp = 265(4) keV. Energies for the excited states in 31 Cl and the photodisintegration rate on 31 Cl have been determined with significantly improved precision using the new Sp value. The improved photodisintegration rate helps to constrain astrophysical conditions where 30 S can act as a waiting point in the rapid proton capture process in type I x-ray bursts.

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Section: M(at T Z ) = A(at ) + B(at )T Z + C(at )Tmentioning

confidence: 99%

“…the A = 31 quartet because there are candidates for the T = 1/2,3/2 + states [58,59] close to the T = 3/2 IAS. The breakdown of the IMME at A = 31 is a crucial finding since the proton separation energy S p = 282.8(44) keV based on the quadratic IMME prediction from Ref.…”

Section: M(at T Z ) = A(at ) + B(at )T Z + C(at )Tmentioning

confidence: 99%

Mass of astrophysically relevantCl31and the breakdown of the isobaric multiplet mass equation

et al. 2016

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“…It has been suggested that the closely-lying excited T = 1, I π = 1 + and T = 0, I π = 1 + states with the energy separation 188.2±1.2 keV [22] in 32 S greatly enhances the isospin mixing, and also the isospin-breaking correction [22]. In another very recent work [23], a large isospin mixing has been observed in 31 Cl β delayed γ-decay experiment. The investigation indicates a large isospin-mixing between the T = 1/2 and T = 3/2 states with spin-parity I π = 3/2 + .…”

mentioning

confidence: 91%

“…In most experiments and theories, the correction due to ISB is known to be smaller than 2% [18,20,21], and the nucleus-independent F t values are found to be consistent [18]. However, recent data have indicated an anomalously large ISB effect in the superallowed Fermi βdecay of 32 Cl [22] and 31 Cl [23]. An unusually large correction δ C = 5.3(9)% has been reported for the Fermi β -decay from 32 Cl to the T = 1 isobaric analog state (IAS) in 32 S, and a large isospin mixing has been observed for the β -decay from 31 Cl to the T = 3/2 IAS in 31 S. It should be noted that these results may depend on both the INC force and the location of the states that mix.…”

mentioning

confidence: 99%

“…To demonstrate that the present shell-model calculations with the chosen effective INC interactions work also for the excited multiplet states in this mass region, we list in Table 1 the CDE's and TDE's for the ground and excited multiplet states in A = 22, 23, 29 − 32. These mass numbers are chosen because they involve the isotopes of our present interest ( 31 Cl, 32 Cl, and 23 Al), for which transition strengths in superallowed Fermi β -decay were observed [22,23,25], and these will be the main focus Table 1: Comparison between experimental and calculated CDE and TDE values (in keV) for the ground and excited multiplet states for A = 22,23,29 − 32. All the CDE's are calculated for states with T = 1/2,T z> = 1/2, p = 1 (see Eq.…”

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confidence: 99%

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Isospin-symmetry breaking in superallowed Fermi β -decay due to isospin-nonconserving forces

et al. 2017

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We investigate isospin-symmetry breaking effects in the sd-shell region with large-scale shell-model calculations, aiming to understand the recent anomalies observed in superallowed Fermi β -decay. We begin with calculations of Coulomb displacement energies (CDE's) and triplet displacement energies (TDE's) by adding the T = 1, J = 0 isospin nonconserving (INC) interaction into the usual isospin-invariant Hamiltonian. It is found that CDE's and TDE's can be systematically described with high accuracy. A total number of 122 one-and two-proton separation energies are predicted accordingly, and locations of the proton drip-line and candidates for proton-emitters are thereby suggested. However, attempt to explain the anomalies in the superallowed Fermi β -decay fails because these well-fitted T = 1, J = 0 INC interactions are found no effects on the nuclear matrix elements. It is demonstrated that the observed large isospin-breaking correction in the 32 Cl β -decay, the large isospin-mixing in the 31 Cl β -decay, and the small isospin-mixing in the 23 Al β -decay can be consistently understood by introducing additional T = 1, J = 2 INC interactions related to the s 1/2 orbit.The degeneracies of energy levels in nuclei with interchanging number of protons and neutrons indicate the existence of isospin symmetry [1,2]. The concept of this approximate symmetry is successful in describing various observables, there are conditions where it does not hold. Isospin symmetry is broken in QCD due to the mass difference between the up and down quarks and their electromagnetic interaction [3]. In nuclei, the Coulomb interaction and the charge-dependent nucleonnucleon interaction break this symmetry, giving rise to observable effects. Especially for nuclei near the N = Z line, both the ground states and excited spectra are affected by isospin-symmetry breaking (ISB). Therefore, investigation of protonrich nuclei far from the line of stability provides important testing ground for ISB effects. It has been known that ISB in nuclear many-body systems in terms of the isospin nonconserving (INC) interactions [4] leads to non-zero Coulomb displacement energy (CDE) [5,6] and triplet displacement energy (TDE) (see definitions in Eq. (1) below). While the microscopic origin of possible INC sources is yet to be understood, study of these quantities must involve the knowledge of the many-body effects in nuclear structure [7]. This suggests that the detailed shell-model calculations with an inclusion of INC forces are es-

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Experimental Study of the $${^{30}}{\text {P}({\text {p}}}{,}{\upgamma })^{31}\text {S}$$ Reaction in Classical Novae

Meyer¹,

Séréville²,

Hammache³

et al. 2019

Springer Proceedings in Physics

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Isospin Mixing RevealsP30(p,γ)S<

Cited by 36 publications

References 42 publications

Mass of astrophysically relevantCl31and the breakdown of the isobaric multiplet mass equation

Mass of astrophysically relevantCl31and the breakdown of the isobaric multiplet mass equation

Isospin-symmetry breaking in superallowed Fermi β -decay due to isospin-nonconserving forces

Experimental Study of the $${^{30}}{\text {P}({\text {p}}}{,}{\upgamma })^{31}\text {S}$$ Reaction in Classical Novae

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