Chiral symmetry restoration by parity doubling and the structure of neutron stars

Marczenko, Michał; Blaschke, D.; Redlich, K.; Sasaki, Chihiro

doi:10.1103/physrevd.98.103021

Cited by 62 publications

(64 citation statements)

References 65 publications

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“…Out result shows that the chiral invariant masses are larger than about 600 MeV, which is consistent with the constraint obtained in Ref. [36]. We also showed predictions of the mass-radius relation of neutron stars, as well as the symmetry energy and the slope parameter at high density.…”

Section: A Summary and Discussionsupporting

confidence: 91%

“…The properties of hot and/or dense matter including neutron star matter based on the parity doublet structure are widely studied in Refs. [11,[18][19][20][21][22][23][24][25][26][27][28][29][30][31][32][33][34][35][36]. In [11, 18-22, 24, 26, 28], the authors studied the relation between the chiral invariant mass and the incompressibility K of nuclear matter and their results show that the empirical value K ∼ 240 MeV only when the chiral invariant mass is close to nucleon's mass, m 0 ∼ 900 MeV.…”

Section: Introductionmentioning

confidence: 99%

“…In Ref. [36], the constraint to the chiral invariant mass from the properties of neutron stars including the tidal deformability observed from GW170817 [37][38][39] was obtained as 780-810 MeV. Recently, the parity doublet model is used to study the nuclei with finite size in Ref.…”

Section: Introductionmentioning

confidence: 99%

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Constraint to chiral invariant masses of nucleons from GW170817 in an extended parity doublet model

Yamazaki

Harada

2019

Phys. Rev. C

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We construct nuclear matter based on an extended parity doublet model including four light nucleons N (939), N (1440), N (1535), and N (1650). We exclude some values of the chiral invariant masses by requiring the saturation properties of normal nuclear matter; saturation density, binding energy, incompressibility, and symmetry energy. We find further constraint to the chiral invariant masses from the tidal deformability determined by the observation of the gravitational waves from neutron star merger GW170817. Our result shows that the chiral invariant masses are larger than about 600 MeV. We also give some predictions on the symmetry energy and the slope parameters in the high density region, which will be measured in future experiments.

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Section: A Summary and Discussionsupporting

confidence: 91%

Section: Introductionmentioning

confidence: 99%

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Constraint to chiral invariant masses of nucleons from GW170817 in an extended parity doublet model

Yamazaki

Harada

2019

Phys. Rev. C

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“…In this section, we introduce the hybrid QMN model for the QCD phase transitions at finite temperature and density, following Ref. [10]. In this contribution we consider an isospinasymmetric system of two flavors, N f = 2, in the mean-field approximation.…”

Section: Hybrid Quark-meson-nucleon Modelmentioning

confidence: 99%

“…In this contribution, we explore the implications of dynamical sequential phase transitions at high baryon density on the structure of neutron stars. To this end, we employ the hybrid quarkmeson-nucleon (QMN) model [10]. We demonstrate how high-mass star configurations can be achieved with different neutron-star interior.…”

Section: Introductionmentioning

confidence: 99%

Chiral symmetry restoration by parity doubling and the structure of neutron stars

Marczenko¹,

Blaschke²,

Redlich³

et al. 2019

Proceedings of XIII Quark Confinement and the Hadron Spectrum — PoS(Confinement2018)

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Recent lattice QCD studies at vanishing density exhibit the parity-doubling structure for the lowlying baryons around the chiral crossover temperature. This finding is likely an imprint of the chiral symmetry restoration in the baryonic sector of QCD, and is expected to occur also in cold dense matter, which makes it of major relevance for compact stars. By contrast, typical effective models for compact star matter embody chiral physics solely in the deconfined sector, with quarks as degrees of freedom. In this contribution, we present a description of QCD matter based on the effective hybrid quark-meson-nucleon model. Its characteristic feature is that, under neutron-star conditions, the chiral symmetry is restored in a first-order phase transition deep in the hadronic phase, before the deconfinement of quarks takes place. We discuss the implications of the parity doubling of baryons on the mass-radius relation for compact stars obtained in accordance with the modern constraints on the mass from PSR J0348+0432, the compactness from GW170817, as well as the direct URCA process threshold. We show that the existence of high-mass stars might not necessarily signal the deconfinement of quarks.

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Interpreting binary neutron star mergers: describing the binary neutron star dynamics, modelling gravitational waveforms, and analyzing detections

2021

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Gravitational waves emitted from the coalescence of neutron star binaries open a new window to probe matter and fundamental physics in unexplored, extreme regimes. To extract information about the supranuclear matter inside neutron stars and the properties of the compact binary systems, robust theoretical prescriptions are required. We give an overview about general features of the dynamics and the gravitational wave signal during the binary neutron star coalescence. We briefly describe existing analytical and numerical approaches to investigate the highly dynamical, strong-field region during the merger. We review existing waveform approximants and discuss properties and possible advantages and shortcomings of individual waveform models, and their application for real gravitational-wave data analysis.

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Chiral symmetry restoration by parity doubling and the structure of neutron stars

Cited by 62 publications

References 65 publications

Constraint to chiral invariant masses of nucleons from GW170817 in an extended parity doublet model

Constraint to chiral invariant masses of nucleons from GW170817 in an extended parity doublet model

Chiral symmetry restoration by parity doubling and the structure of neutron stars

Interpreting binary neutron star mergers: describing the binary neutron star dynamics, modelling gravitational waveforms, and analyzing detections

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