Shell evolution beyond<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mrow><mml:mi>N</mml:mi><mml:mo>=</mml:mo><mml:mn>40</mml:mn></mml:mrow><mml:mo>:</mml:mo></mml:math><mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"><mml:mmultiscripts><mml:mi mathvariant="normal">Cu</mml:mi><mml:mprescripts /><mml:none /><mml:mrow><mml:mn>69</mml:mn><mml:mo>,</mml:mo><mml:mn>71</mml:mn><mml:mo>,</mml:mo><mml:mn>73</mml:mn></mml:mrow></mml:mmultiscripts></mml:math>

Şahin, E.; Doncel, M.; Sieja, K.; Angelis, G. de; Gadea, A.; Quintana, B.; Görgen, A.; Modamio, V.; Mengoni, D.; Valiente-Dobón, J.J.; John, P. R.; Albers, M.; Bazzacco, D.; Benzoni, G.; Birkenbach, B.; Cederwall, B.; Clément, E.; Curien, D.; Corradi, L.; Désesquelles, P.; Dewald, Α.; Didierjean, F.; Duchêne, G.; Eberth, J.; Erduran, M. N.; Farnea, E.; Fioretto, E.; Fransen, C.; Gernhäuser, R.; Gottardo, A.; Hackstein, M.; Hagen, T. W.; Hernández-Prieto, A.; Hess, H.; Hüyük, T.; Jungclaus, A.; Klupp, S.; Körten, W.; Kuşoğlu, A.; Lenzi, S. M.; Ljungvall, J.; Louchart, C.; Lunardi, S.; Menegazzo, R.; Michelagnoli, C.; Mijatović, T.; Million, B.; Molini, P.; Montagnoli, G.; Montanari, D.; Möller, O.; Napoli, D. R.; Obertelli, A.; Orlandi, R.; Pollarolo, G.; Pullia, A.; Recchia, F.; Reiter, P.; Rosso, D.; Rother, W.; Salsac, M. D.; Scarlassara, F.; Schlarb, M.; Siem, S.; Singh, Pushpendra P.; Söderström, P.-A.; Stefanini, A. M.; Stézowski, O.; Sulignano, B.; Szilner, S.; Theisen, Ch.; Ur, C. A.; Yalçınkaya, M.

doi:10.1103/physrevc.91.034302

Cited by 27 publications

(6 citation statements)

References 59 publications

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“…To see how the observed level and decay scheme compares with theory as well as to shed light on the fate of the shell closure Z = 28, large-scale shell-model calculations were performed in the valence space comprising neutron (f 5/2 p 1/2 g 9/2 d 5/2 ) and proton fp orbitals. The Hamiltonian employed here was the one based on the Lenzi, Nowacki, Poves, and Sieja interaction [36], which was used recently to study the copper isotopes from 69 Cu to 77 Cu [37][38][39]. Due to the large size of the configuration space, the calculations were truncated to 8p-8h excitations across Z = 28 and N = 40 gaps, which assured, however, a good convergence of the calculated spectra for 76 Ni.…”

Section: Resultsmentioning

confidence: 99%

Nuclear structure of Ni76 from the ( p,2p ) reaction

Elekes¹,

Kripkó²,

Sohler³

et al. 2019

Phys. Rev. C

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The nuclear structure of the 76 Ni nucleus was investigated by (p, 2p) reaction using a NaI(Tl) array to detect the deexciting prompt γ rays. A new transition with an energy of 2227 keV was identified by γ γ and γ γ γ coincidences. According to these coincidence spectra the observed transition connects a new state at 4147 keV and the previously known 4 + 1 state at 1920 keV. Two weaker transitions were also obtained at 2441 and 2838 keV, which could be tentatively placed to feed the known 2 + 1 state at 990 keV. Our shell-model calculations using the Lenzi, Nowacki, Poves, and Sieja interaction produced good candidates for the experimental proton hole states in the observed energy region, and the theoretical cross sections showed good agreement with the experimental values. Although we could not assign all the experimental states to the theoretical ones unambiguously, the results are consistent with a reasonably large Z = 28 shell gap for nickel isotopes in accordance with previous studies.

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Section: Resultsmentioning

confidence: 99%

Nuclear structure of Ni76 from the ( p,2p ) reaction

Elekes¹,

Kripkó²,

Sohler³

et al. 2019

Phys. Rev. C

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“…We have thus performed large scale shell-model calculations within the proton f p and neutron f pg 9/2 d 5/2 model space, employing the Hamiltonian from Ref. [11] with minor modifications [72,73]. Additionally, the global monopole term was made more attractive by 30 keV to obtain a better agreement of the S 2n energies in neutron-rich chromium and iron isotopes.…”

Section: A Structural Evolution Of the Neutron-rich Chromium Isotopesmentioning

confidence: 99%

Time-of-flight mass measurements of neutron-rich chromium isotopes up toN=40and implications for the accreted neutron star crust

Meisel¹,

George²,

Ahn³

et al. 2016

Phys. Rev. C

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Time-of-flight mass measurements of neutron-rich chromium isotopes up to N=40 and implications for the accreted neutron star crust We present the mass excesses of 59−64 Cr, obtained from recent time-of-flight nuclear mass measurements at the National Superconducting Cyclotron Laboratory at Michigan State University. The mass of 64 Cr was determined for the first time with an atomic mass excess of −33.48(44) MeV. We find a significantly different two-neutron separation energy S2n trend for neutron-rich isotopes of chromium, removing the previously observed enhancement in binding at N = 38. Additionally, we extend the S2n trend for chromium to N = 40, revealing behavior consistent with the previously identified island of inversion in this region. We compare our results to state-of-the-art shell-model calculations performed with a modified Lenzi-Nowacki-Poves-Sieja interaction in the f p-shell, including the g 9/2 and d 5/2 orbits for the neutron valence space. We employ our result for the mass of 64 Cr in accreted neutron star crust network calculations and find a reduction in the strength and depth of electron capture heating from the A = 64 isobaric chain, resulting in a cooler than expected accreted neutron star crust. This reduced heating is found to be due to the over 1 MeV reduction in binding for 64 Cr with respect to values from commonly used global mass models. I. INTRODUCTION 22The evolution of nuclear structure away from the val- production of more neutron-rich nuclides of interest were 106 used alternately, keeping Bρ of the A1900 and S800 fixed. 107Fragments were transmitted through the A1900 fragment spectively. 124The relationship between TOF and nuclear rest mass 125 m rest is obtained from the equation of motion for a 126 charged massive particle through a magnetic system. 127Equating the two counteracting forces, the Lorentz force 128 F L and the centripetal force F c , results in the followingwhere the Lorentz factor γ is a function of velocity v, the Bρ-corrected data were fit with a Gaussian distribu-158 tion in order to determine a mean TOF for each nuclide. 159The relationship between mass over charge m rest /q and 160TOF was fit to the data of reference nuclides in order to

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“…Earlier β-decay, Coulomb excitation, and multinucleon transfer reaction studies showed rather complicated level sequences in the neutron-rich 69-73 Cu isotopes, caused by different excitation modes [13][14][15][16][17][18]. The low-lying 5=2 − and 7=2…”

mentioning

confidence: 95%

Shell Evolution towards Ni78 : Low-Lying States in Cu77
Şahin¹,
Garrote²,
Tsunoda³
et al. 2017
Phys. Rev. Lett.
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The level structure of the neutron-rich 77 Cu nucleus is investigated through β-delayed γ-ray spectroscopy at the Radioactive Isotope Beam Factory of the RIKEN Nishina Center. Ions of 77 Ni are produced by inflight fission, separated and identified in the BigRIPS fragment separator, and implanted in the WAS3ABi silicon detector array, surrounded by Ge cluster detectors of the EURICA array. A large number of excited states in 77 Cu are identified for the first time by correlating γ rays with the β decay of 77 Ni, and a level scheme is constructed by utilizing their coincidence relationships. The good agreement between large-scale Monte Carlo shell model calculations and experimental results allows for the evaluation of the singleparticle structure near 78 Ni and suggests a single-particle nature for both the 5=2 − 1 and 3=2 The evolution of the shell structure is one of the key motivations to study atomic nuclei with large neutron excess. The goal is to understand effects due to this excess of neutrons that are responsible for deviations from the conventional harmonic oscillator description with a strong attractive spin-orbit coupling, which characterizes the shell structure and properties of nuclei near the line of β stability. Such deviations are related to the monopole components of the effective nucleon-nucleon interaction and their strong effects on the single-particle energies (SPEs). The spindependent central component influences the energies of all single-particle orbitals, while the tensor interaction alters the spin-orbit splitting when specific orbits are filled by neutrons or protons [1][2][3][4][5][6][7][8].For the chain of Ni (Z ¼ 28) isotopes between N ¼ 40 and N ¼ 50, theoretical models predict significant changes in the proton SPEs as the ν1g 9=2 shell is filled by neutrons [3,4,[9][10][11][12]. Here, the tensor force responsible for SPE shifts

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Shell evolution beyondN=40:Cu69,71,73

Cited by 27 publications

References 59 publications

Nuclear structure of Ni76 from the ( p,2p ) reaction

Nuclear structure of Ni76 from the ( p,2p ) reaction

Time-of-flight mass measurements of neutron-rich chromium isotopes up toN=40and implications for the accreted neutron star crust

Shell Evolution towards Ni78 : Low-Lying States in Cu77
Şahin¹,
Garrote²,
Tsunoda³
et al. 2017
Phys. Rev. Lett.
Self Cite
33
7
22
0
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Shell evolution beyondN=40:Cu69,71,73

Cited by 27 publications

References 59 publications

Nuclear structure of Ni76 from the ( p,2p ) reaction

Nuclear structure of Ni76 from the ( p,2p ) reaction

Time-of-flight mass measurements of neutron-rich chromium isotopes up toN=40and implications for the accreted neutron star crust

Shell Evolution towards Ni78 : Low-Lying States in Cu77Şahin1, Garrote2, Tsunoda3 et al. 2017Phys. Rev. Lett.Self Cite337220View full textAdd to dashboardCite

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Shell Evolution towards Ni78 : Low-Lying States in Cu77
Şahin¹,
Garrote²,
Tsunoda³
et al. 2017
Phys. Rev. Lett.
Self Cite
33
7
22
0
View full text Add to dashboard Cite