Density dependence of the symmetry energy in the post–PREX-CREX era

Reed, Brendan T.; Fattoyev, F. J.; Horowitz, C. J.; Piekarewicz, J.

doi:10.1103/physrevc.109.035803

Cited by 14 publications

(1 citation statement)

References 81 publications

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“…So it puts serious tension to fit CREX and PREX-II data simultaneously without compromising the properties of finite nuclei, bulk nuclear, and dense matter. Recently as reported in [64], while the DINO models provide a plausible solution to the PREX-2-CREX dilemma, they fail to reproduce astrophysical observations like radius and tidal deformability of canonical mass neutron star as obtained from the observations of LIGO-Virgo, NICER and GW170817 event data unless a phase transition or other strong density dependence develops at intermediate densities. Although the DINO models are consistent with the properties of finite nuclei, their large values for K sym induce large stiffening of the EoS at the high densities relevant to neutron stars.…”

Section: Resultsmentioning

confidence: 97%

Relativistic description of dense matter equation of state and neutron star observables constrained by recent astrophysical observations

Kumar,

Kumar

et al. 2024

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

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In the present work, we investigate the bulk properties of nuclear matterand neutron stars with the newly proposed relativistic interaction NL-RS whichprovides an opportunity to readjust the coupling constants keeping in view theproperties of finite nuclei, nuclear matter, PREX-II results for neutron skin thickness in208Pb and astrophysical observations. The NL-RS model interaction has been proposedby fitting the ground state properties (binding energies and charge radii) of finitenuclei, bulk nuclear matter properties, and PREX-II results for neutron skin thicknessof 208 Pb. The relativistic interaction has been generated by including non-linear self-interactions of σ and ωµ -mesons and mixed interactions of ωµ , and ρµ -meson up tothe quartic order. The proposed interaction harmonizes with the finite nuclei, bulknuclear matter, and neutron star properties. A covariance analysis is performed toassess the statistical uncertainties on the model parameters and nuclear observables ofinterest along with correlations amongst them. The equation of state (EoS) composedof nucleons and leptons in β - β-equilibrium is computed with the proposed parameterset and used to study the neutron star structure. The maximum mass of the neutronstar by employing the EoS computed with the NL-RS parameter set is 2.04±0.03M⊙ and the radius of a canonical mass neutron star (R1.4 ) comes out to be equal to13.06±0.16 Km. The value of dimensionless tidal deformability, for canonical mass, is602.23±33.13 which satisfies the

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Section: Resultsmentioning

confidence: 97%

Relativistic description of dense matter equation of state and neutron star observables constrained by recent astrophysical observations

Kumar,

Kumar

et al. 2024

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

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Heaven and Earth: Nuclear Astrophysics after GW170817

Piekarewicz

2024

EPJ Web Conf.

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The historical detection of gravitational waves from the binary neutron star merger GW170817 is providing fundamental new insights into the astrophysical site for the creation of the heaviest elements in the cosmos and the equation of state of neutron-rich matter. Shortly after this historical detection, electromagnetic observations of neutron stars together with measurements of the properties of neutron-rich nuclei at terrestrial facilities have placed additional constraints on the dynamics of neutron-rich matter. It is this unique synergy between heaven and earth that is the focus of this article.

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Hybrid stars and the stiffness of the nuclear equation of state in light of the HESS J1731-347 remnant

Laskos-Patkos,

Koliogiannis,

Moustakidis

2024

EPJ Web Conf.

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The recent observation of the extremely compact neutron star in the HESS J1731-347 remnant has challenged our understanding concerning the nature of dense nuclear matter. In particular, the low radius of the aforementioned compact object favors soft nuclear equations of state. However, the neutron skin thickness of 208Pb extracted from the long-awaited PREX-II experiment favors stiff equations of state which may be associated with larger radii for low mass stellar configurations. In this contribution we present our recent work on the possible reconciliation of the HESS J1731-347 observation in the framework of hybrid stars, under the assumption of a stiff low-density phase which may be favored by the PREX-II results. In addition, we examine the compatibility of the resulting hybrid models with recent constraints based on the observation of PSR J0030+0451, PSR J0952-0607 and GW190814.

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Density dependence of the symmetry energy in the post–PREX-CREX era

Cited by 14 publications

References 81 publications

Relativistic description of dense matter equation of state and neutron star observables constrained by recent astrophysical observations

Relativistic description of dense matter equation of state and neutron star observables constrained by recent astrophysical observations

Heaven and Earth: Nuclear Astrophysics after GW170817

Hybrid stars and the stiffness of the nuclear equation of state in light of the HESS J1731-347 remnant

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