Neutron star deformability with hyperonization in density-dependent relativistic mean-field models

Shangguan, W. Z.; Huang, Zhenguang; Wei, Si-Na; Jiang, Wei-Zhou

doi:10.1103/physrevd.104.063035

Cited by 6 publications

(4 citation statements)

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“…The SLCd can simultaneously reproduce the properties of finite nuclei [24] and neutron star properties with and without hyperonization [55]. In addition, the neutron star deformability obtained with the SLCd fits the data fairly well [50]. The progress to describe the properties of finite nuclei and neutron stars is also made with the SCL [16,56].…”

Section: Resultsmentioning

confidence: 86%

“…Together with rather soft vector potential, the SCL and FSUGold are not able to meet the 2M constraint of neutron stars. The situation with the NJL350 and SLCd is quite different by owning the stiff EOS's at high densities and fitting the 2M constraint of neutron stars [20,50,55]. The scalar field that dictates the nucleon effective mass changes the kinetic symmetry energy (the kinetic part of the symmetry energy) which in the relativistic formulation is…”

Section: Resultsmentioning

confidence: 99%

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Nuclear Potentials Relevant to the Symmetry Energy in Chiral Models

Wei

Jiang

2022

Symmetry

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We employ the extended Nambu-Jona-Lasinio (NJL), linear-σ models, and the density-dependent model with chiral limits to work out the mean fields and relevant properties of nuclear matter. To have the constraint from the data, we re-examine the Dirac optical potentials and symmetry potential based on the relativistic impulse approximation (RIA). Unlike the extended NJL and the density-dependent models with the chiral limit in terms of the vanishing scalar density, the extended linear-σ model with a sluggish changing scalar field loses the chiral limit at the high-density end. The various scalar fields can characterize the different Schrödinger-equivalent potentials and kinetic symmetry energy in the whole density region and the symmetry potential in the intermediate density region. The drop in the scalar field due to the chiral restoration results in a clear rise of the kinetic symmetry energy. The chiral limit in the models gives rise to the softening of the symmetry potential and thereof the symmetry energy at high densities.

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Section: Resultsmentioning

confidence: 86%

Section: Resultsmentioning

confidence: 99%

Nuclear Potentials Relevant to the Symmetry Energy in Chiral Models

Wei

Jiang

2022

Symmetry

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“…The description of the neutron stars based on microscopic models of the strong interaction still suffers from important uncertainties. The contrast between the recently obtained observational data and the predictions of a high variety of hadronic models [59][60][61][62][63][64][65][66][67][68][69][70][71][72][73][74][75][76][77][78]79] is a source for fixing missing information. Many of these studies have assumed that matter is composed only by protons, neutrons and leptons.…”

Section: Introductionmentioning

confidence: 86%

Influence of hyperon–hyperon interaction on the properties of neutron stars

Aguirre

2024

J. Phys. G: Nucl. Part. Phys.

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The properties of neutron stars are studied in a composite modelof the strong interaction. In the regime of low to medium baryonicdensities a covariant hadronic model is adopted which includes anexclusive channel for the hyperon-hyperon interaction mediated byhidden strangeness mesons, which in turn couple to other mesonsthrough polynomial vertices. The new coupling constants aresubject to phenomenological constraints. The presence of freequarks in the core of the star is considered by using theNambu-Jona Lasinio model supplemented with a vector interaction.The deconfinement process is described by a continuous coexistenceof phases. Several structure parameters of neutron stars, such asmass-radius relation, moment of inertia, tidal deformability, andthe propagation of nonradial f and g-modes within the relativisticCowling approximation are studied. The predictions of the modelare in good agreement with recent observational data, inparticular the maximum inertial mass is greater than theobservational lower limit of two solar masses.

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“…On the other hand, fundamental symmetries and new methods have been proposed to constrain the symmetry energy [20−26]. Though it remains a challenge to resolve the uncertainty of the symmetry energy, one may employ this uncertainty to study its effect on physical ob-servables, such as pulsar glitches [27,28] and star tidal deformability [29,30]. These astrophysical observations may constrain or even reduce the uncertainty.…”

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confidence: 99%

Neutron star core-crust transition and the crustal moment of inertia in the nonlinear relativistic Hartree approximation*

Li 李,

Wei 韦,

Yang 杨

et al. 2024

Chinese Phys. C

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We investigate the effects of the $\sigma$ meson mass ($m_\sigma$), symmetry energy and its slope on the neutron star core-crust transition density and the crustal moment of inertia ($\Delta I/I$) in the nonlinear relativistic Hartree approach (RHA), which includes vacuum polarization. Although the core-crust transition density ($\rho_{t}$), pressure ($P_{t}$), and neutron star radius ($R$) that are all dependent on the symmetry energy all contribute to determining $\Delta I/I$, we find that changing only the slope of symmetry energy within a reasonable range is not sufficient to reach $\Delta I/I\geq7\%$ to achieve the large glitches of the Vela pulsar. However, since all three factors ($\rho_{t}$, $P_{t}$, and $R$) increase with the increase of $m_\sigma$ through scalar vacuum polarization, adjusting $m_\sigma$ can easily achieve $\Delta I/I\geq7\%$.

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Neutron star deformability with hyperonization in density-dependent relativistic mean-field models

Cited by 6 publications

References 50 publications

Nuclear Potentials Relevant to the Symmetry Energy in Chiral Models

Nuclear Potentials Relevant to the Symmetry Energy in Chiral Models

Influence of hyperon–hyperon interaction on the properties of neutron stars

Neutron star core-crust transition and the crustal moment of inertia in the nonlinear relativistic Hartree approximation*

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