Asymmetric Nuclear Matter in Relativistic Mean-field Models with Isoscalar- and Isovector-meson Mixing

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

doi:10.3847/1538-4357/ac5f40

Cited by 22 publications

(14 citation statements)

References 76 publications

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“…Also in Zabari et al (2019a), the ω meson self-interactions and the crossing term ρ-ω are not considered. A similar study has been performed very recently in Miyatsu et al (2022).…”

Section: Introductionsupporting

confidence: 56%

Effects of Isoscalar- and Isovector-scalar Meson Mixing on Neutron Star Structure

Cai²,

Zhou³

et al. 2022

ApJ

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Based on the accurately calibrated interaction FSUGold, we show that including isovector-scalar δ meson and its coupling to isoscalar-scalar σ meson in the relativistic mean-field (RMF) model can soften the symmetry energy E sym(n) at intermediate densities while stiffening the E sym(n) at high densities. We find this new RMF model can be simultaneously compatible with (1) the constraints on the equation of state of symmetric nuclear matter at suprasaturation densities from flow data in heavy-ion collisions; (2) the neutron skin thickness of 208Pb from the PREX-II experiment; (3) the largest mass of a neutron star (NS) reported so far from PSR J0740+6620; (4) the limit of Λ1.4 ≤ 580 for the dimensionless tidal deformability of the canonical 1.4 M ⊙ NS from the gravitational-wave signal GW170817; (5) the mass–radius relation of PSR J0030+0451 and PSR J0740+6620 measured by NICER. The new model thus removes the tension between PREX-II and GW170817 observed in the conventional RMF model.

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“…Also in Zabari et al (2019a), the ω meson self-interactions and the crossing term ρ-ω are not considered. A similar study has been performed very recently in Miyatsu et al (2022).…”

Section: Introductionsupporting

confidence: 56%

Effects of Isoscalar- and Isovector-scalar Meson Mixing on Neutron Star Structure

Cai²,

Zhou³

et al. 2022

ApJ

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“…As mentioned in the introduction, we consider various types of RMF effective interactions: LHS (Reinhard 1989), RMF201 (Dadi 2010), NL3 (Lalazissis et al 1997), Hybrid (Piekarewicz & Centelles 2009), TM2 (Sugahara & Toki 1994), NLSV1 (Sharma et al 2000), PK1 (Long et al 2004), NL3ωρ (Horowitz & Piekarewicz 2001), S271v6 (Horowitz & Piekarewicz 2002), HC (Bunta & Gmuca 2003), DD-LZ1 (Wei et al 2020), DD-ME2 (Lalazissis et al 2005), DD2 (Typel et al 2010), PKDD (Long et al 2004), OMEG (Miyatsu et al 2022), and the zero-range point coupling ones without exchanging mesons: DD-PC1 (Nikšić et al 2008), FKVW (Finelli et al 2006), PC-PK1 (Zhao et al 2010). They also cover all variants of the RMF models reviewed in Dutra et al (2014).…”

Section: The Rmf Modelmentioning

confidence: 99%

Astrophysical Implications on Hyperon Couplings and Hyperon Star Properties with Relativistic Equations of States

Sun

Miao

Sun

et al. 2023

ApJ

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Hyperons are essential constituents in the neutron star interior. The poorly known hyperonic interaction is a source of uncertainty for studying laboratory hypernuclei and neutron star observations. In this work, we perform Bayesian inference of phenomenological hyperon–nucleon interactions using the tidal deformability measurement of the GW170817 binary neutron star merger as detected by LIGO/Virgo and the mass–radius measurements of PSR J0030+0541 and PSR J0740+6620 as detected by NICER. The analysis is based on a set of stiff relativistic neutron star matter equation of states with hyperons from the relativistic mean-field theory, naturally fulfilling the causality requirement and empirical nuclear matter properties. We specifically utilize the strong correlation recently deduced between the scalar and vector meson–hyperon couplings, imposed by the measured Λ separation energy in single-Λ hypernuclei, and perform four different tests with or without the strong correlation. We find that the laboratory hypernuclear constraint ensures a large enough Λ–scalar–meson coupling to match the large vector coupling in hyperon star matter. When adopting the current most probable intervals of hyperon couplings from the joint analysis of laboratory and astrophysical data, we find the maximum mass of hyperon stars is at most 2.176 − 0.202 + 0.085 M ⊙ (68% credible interval) from the chosen set of stiff equation of states. The reduction of the stellar radius due to hyperons is quantified based on our analysis and various hyperon star properties are provided.

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“…With the above considerations, we include the isoscalar scalar meson σ and vector mesons ρ and ω in GnEFT. Note that, it is recently found that the iso-vector scalar mesons δ (denoted as a 0 (980) in particle physics) also affects the EoS through the symmetry energy in a sizable way [49,50]. However, since we do not have any idea on how to construct an EFT for them and their structures are still under debate, we will not consider them in the present work.…”

Section: Hidden Symmetries and Hadron Resonancesmentioning

confidence: 99%

Topology and emergent symmetries in dense compact star matter

Ma¹,

Yang²

2023

Preprint

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It has been found that the topology effect and the possible emergent scale and hidden local flavor symmetries at high density reveal a novel structure of the compact star matter. The N f ≥ 2 baryons can be described by the skyrmion in the large Nc limit and there is a robust topology change in the skyrmion matter approach to dense nuclear matter. The hidden scale and local flavor symmetries which are sources introducing the lightest scalar meson-dilaton-and lowest lying vector mesons into to nonlinear chiral effective theory are seen to play important roles in understanding the nuclear force. We review in this paper the generalized nuclear effective theory (GnEFT), which applicable to nuclear matter from low density to the compact star density, constructed with the robust conclusion from the topology approach to dense matter and emergent scale and hidden local flavor symmetries. The topology change at density larger than two times saturation density n0 encoded in the parameters of the effective field theory is interpreted as the hadron-quark continuity in the sense of Cheshire Cat Principle. A novel feature predicted in this theory that has not been found before is the precocious appearance of the conformal sound velocity in the cores of massive stars, although the trace of the energy-momentum tensor of the system is not zero. That is, in contrast to the usual picture, the cores of massive stars are composed of quasiparticles of fractional baryon charges, neither baryons nor deconfined quarks. Hidden scale and local flavor symmetries emerge and give rise a resolution of the longstanding gA quench problem in nuclei transition. To illustrate the rationality of the GnEFT, we finally confront the generalized effective field theory to the global properties of neutron star and the data from gravitational wave detections.

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Asymmetric Nuclear Matter in Relativistic Mean-field Models with Isoscalar- and Isovector-meson Mixing

Abstract: Using the relativistic mean-field model with nonlinear couplings between the isoscalar and isovector mesons, we study the properties of isospin-asymmetric nuclear matter. Not only the vector mixing, ω μ ω μ ρ ν ρ … Show more

Cited by 22 publications

References 76 publications

Effects of Isoscalar- and Isovector-scalar Meson Mixing on Neutron Star Structure

Effects of Isoscalar- and Isovector-scalar Meson Mixing on Neutron Star Structure

Astrophysical Implications on Hyperon Couplings and Hyperon Star Properties with Relativistic Equations of States

Topology and emergent symmetries in dense compact star matter

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