Can the PREX-2 and CREX results be understood by relativistic mean-field models with the astrophysical constraints?

Miyatsu, Tsuyoshi; Cheoun, Myung-Ki; Kim, Kyungsik; Saito, Koichi

doi:10.1016/j.physletb.2023.138013

Cited by 18 publications

(6 citation statements)

References 67 publications

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“…This implies that when we include only recently measured Δr np ( 208 Pb = 0.283± 0.071 fm) from PREX-II results [25] in our fitting data to constrain the linear density dependence of symmetry energy, a larger value of neutron skin thickness Δr np = 0.196 fm for 48 Ca is obtained for NL-RS model and is significantly overestimated the CREX results [25]. The reason might be that the PREX-II data suggests relatively stiff values of L whereas CREX data suggest very softness of linear density dependence of symmetry energy as also discussed in [34,[60][61][62][63]. The Δr np for 48 Ca predicted by the NL-RS model overestimates the recently reported value by CREX results and the serious tension between CREX and PREX-II measurements continues as also discussed in [60][61][62][63].…”

Section: Discussionmentioning

confidence: 79%

“…Also as reported in [34,[58][59][60][61][62] that it is difficult to produce CREX and PREX-II results simultaneously and the CREX results push the value of L towards a lower value, while PREX-II shifts it towards a higher value. It is also reported in [34,62,63] that it is very difficult to understand the PREX-II and CREX results simultaneously within relativistic mean field models. 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.…”

Section: Resultsmentioning

confidence: 95%

“…The CREX has recently given a model-independent extraction of neutron skin thickness of 48 Ca as Δr np = 0.121 ± 0.026 fm [24]. Also as reported in [34,[58][59][60][61][62] that it is difficult to produce CREX and PREX-II results simultaneously and the CREX results push the value of L towards a lower value, while PREX-II shifts it towards a higher value. It is also reported in [34,62,63] that it is very difficult to understand the PREX-II and CREX results simultaneously within relativistic mean field models.…”

Section: Resultsmentioning

confidence: 99%

See 2 more Smart Citations

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: Discussionmentioning

confidence: 79%

Section: Resultsmentioning

confidence: 95%

Section: Resultsmentioning

confidence: 99%

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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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“…[19], but without spin-orbit cor- rections. As shown, the charge radius of Ca is larger than that of experiments [31]. If the neutron skin thickness of Pb is forced to be thick, the charge radius of Pb becomes smaller.…”

mentioning

confidence: 78%

“…The experiments of neutron skin thickness are taken from PREX-II[2] and CREX[16]. The experimental charge radii are taken from[31].…”

mentioning

confidence: 99%

Implications of neutron skin measurements on Skyrme equations of state*

Guan 管,

Pei 裴,

Jiang 蒋

2024

Chinese Phys. C

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The recent measurements on neutron skins via parity violation in electron scattering have extracted an abnormal thick neutron skin for $^{208}$Pb, which has significant consequences in nuclear equation of state (EoS) and neutron star observations. This work performs optimizations of extended Skyrme forces in a consistent manner by including neutron skin thicknesses from PREX-II and CREX experimentsand investigates nuclear EoS and neutron stars in the GW170817 event. By varying the fitting weights of neutron skins, several new Skyrme parameterizations are obtained. Our results show the competition in the fitting procedure to simultaneously describe neutron skins, other properties of finite nuclei and neutron star observations. The prospects in resolving the neutron skin issues are also discussed.

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New quantification of symmetry energy from neutron skin thicknesses of 48Ca and 208Pb

An,

Sun,

Cao

et al. 2024

NUCL SCI TECH

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Can the PREX-2 and CREX results be understood by relativistic mean-field models with the astrophysical constraints?

Cited by 18 publications

References 67 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

Implications of neutron skin measurements on Skyrme equations of state*

New quantification of symmetry energy from neutron skin thicknesses of 48Ca and 208Pb

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