Mass dependence of symmetry energy coefficients in the Skyrme force

Wang, Ning; Liu, M.; Jiang, Hui; Tian, Junlong; Zhao, Y. M.

doi:10.1103/physrevc.91.044308

Cited by 26 publications

(21 citation statements)

References 55 publications

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“…2 (e), (f)) results in the absence of s 1/2 state near the Fermi level and shows no bubble character. The inversion of proton states (3s 1/2 and 1h 11/2 ) similar to 206 Hg [36] results in the unoccupied 3s 1/2 state in all the N = 126 (Z = 48−78) isotones indicating bubble structure in the complete chain (seen in Fig. 2(g)).…”

mentioning

confidence: 76%

Bubble structure in magic nuclei

Saxena

Kumawat

Kaushik³

et al. 2019

Physics Letters B

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The existence of bubble nuclei identified by the central depletion in nucleonic density is studied for the conventional magic N (Z) = 8, 20, 28, 40, 50, 82, 126 isotones (isotopes) and recently speculated magic N = 164, 184, 228 superheavy isotones. Many new bubble nuclei are predicted in all regions. Study of density profiles, form factor, single particle levels and depletion fraction (DF) across the periodic chart reveals that the central depletion is correlated to shell structure and occurs due to unoccupancy in s-orbit (2s, 3s, 4s) and inversion of (2s, 1d) and (3s, 1h) states in nuclei upto Z ≤ 82. Bubble effect in superheavy region is a signature of the interplay between the Coulomb and nn-interaction and depletion fraction (DF) is found to increase with Z (Coulomb repulsion) and decrease with isospin. Our results are consistent with the available data. The occupancy in s-state in 34 Si increases with temperature which appears to quench the bubble effect.

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mentioning

confidence: 76%

Bubble structure in magic nuclei

Saxena

Kumawat

Kaushik³

et al. 2019

Physics Letters B

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“…[24], the kinetic part of E sym,4 (ρ 0 ) is predicted to be 7.18 ± 2.52 MeV by considering the high-momentum tail in the single-nucleon momentum distributions based on an interacting Fermi gas model that could be due to short-range correlations of nucleon-nucleon interactions. Most recently, a significantly large value of E sym,4 (ρ 0 ) = 20.0 ± 4.6 is estimated within an extended semi-empirical nuclear mass formula [25] by analyzing the fourth-order symmetry energy of finite nuclei [26][27][28][29] extracted from nuclear mass data. Given such a large uncertainty, a systematic study on the fourth-order symmetry energy is therefore critically important, and this provides the main motivation of the present work.…”

Section: Introductionmentioning

confidence: 99%

Nuclear matter fourth-order symmetry energy in nonrelativistic mean-field models

Zhang

Chen

2017

Phys. Rev. C

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Background: Nuclear matter fourth-order symmetry energy Esym,4(ρ) may significantly influence the properties of neutron stars such as the core-crust transition density and pressure as well as the proton fraction at high densities. The magnitude of Esym,4(ρ) is, however, largely uncertain. Purpose: Based on systematic analyses of several popular non-relativistic energy density functionals with mean-field approximation, we estimate the value of the Esym,4(ρ) at nuclear normal density ρ0 and its density dependence, and explore the correlation between Esym,4(ρ0) and other macroscopic quantities of nuclear matter properties. Method: We use the empirical values of some nuclear macroscopic quantities to construct model parameter sets by Monte Carlo method for four different energy density functionals with mean-field approximation, namely, the conventional Skyrme-Hartree-Fock (SHF) model, the extended SkyrmeHartree-Fock (eSHF) model, the Gogny-Hartree-Fock (GHF) model, and the momentum-dependent interaction (MDI) model. With the constructed samples of parameter sets, we can estimate the density dependence of Esym,4(ρ) and analyze the correlation of Esym,4(ρ0) with other macroscopic quantities.Results: The value of Esym,4(ρ0) is estimated to be 1.02 ± 0.49 MeV for the SHF model, 1.02 ± 0.50 MeV for the eSHF model, 0.70 ± 0.60 MeV for the GHF model, and 0.74 ± 0.63 MeV for the MDI model. Moreover, our results indicate that the density dependence of Esym,4(ρ) is model dependent, especially at higher densities. Furthermore, we find that the Esym,4(ρ0) has strong positive (negative) correlation with isoscalar (isovector) nucleon effective mass m * s,0 (m * v,0 ) at ρ0. In particular, for the SHF and eSHF models, the Esym,4(ρ) is completely determined by the isoscalar and isovector nucleon effective masses m * s (ρ) and m * v (ρ), and the analytical expression is given. Conclusions: In the mean-field models, the magnitude of Esym,4(ρ0) is generally less than 2 MeV, and its density dependence depends on models, especially at higher densities. Esym,4(ρ0) is strongly correlated with m * s,0 and m * v,0 .

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“…[21,22]. But how to change it depends on the isospin asymmetry I for given mass number A, decreases or increases?…”

Section: Introductionmentioning

confidence: 99%

Effect of Wigner energy on the symmetry energy coefficient in nuclei

et al. 2016

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The nuclear symmetry energy coefficient (including the coefficient a (4) sym of I 4 term) of finite nuclei is extracted by using the differences of available experimental binding energies of isobaric nuclei.It is found that the extracted symmetry energy coefficient a * sym (A, I) decreases with increasing of isospin asymmetry I, which is mainly caused by Wigner correction, since e * sym is the summation of the traditional symmetry energy e sym and the Wigner energy e W . We obtain the optimal values J = 30.25 ± 0.10 MeV, a ss = 56.18 ± 1.25 MeV, a sym term increases rapidly with increasing of isospin asymmetry I. For very neutron-rich nuclei, the contribution of asym term will play an important role.

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Mass dependence of symmetry energy coefficients in the Skyrme force

Cited by 26 publications

References 55 publications

Bubble structure in magic nuclei

Bubble structure in magic nuclei

Nuclear matter fourth-order symmetry energy in nonrelativistic mean-field models

Effect of Wigner energy on the symmetry energy coefficient in nuclei

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