Chiral condensates for neutron stars in hadron-quark crossover: From a parity doublet nucleon model to a Nambu–Jona-Lasinio quark model

Takuya, Minamikawa,; Kojo, Toru; Harada, Masayasu

doi:10.1103/physrevc.104.065201

Cited by 13 publications

(13 citation statements)

References 129 publications

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“…Based on the constrained properties of dense stellar matter, we extract the corresponding quark condensate in the framework of equivparticle model [38], and find it is decreasing nonlinearly with density. At larger densities with pure quark matter, the quark condensate is still large and does not decrease quickly with density, suggesting that the stellar matter in hybrid stars are highly nonperturbative even when a deconfinement phase transition takes place at ρ ρ TOV , which is consistent with the recent studies in the absence of a strong first-order phase transition [39,40].…”

Section: Discussionsupporting

confidence: 89%

“…We then extract the inmedium quark condensate in these dense stellar matter in the framework of an equivparticle model [38]. It is found that the quark condensate is decreasing with density but rises in certain cases at the end of mixed phases, suggesting that the stellar matter in hybrid stars are highly nonperturbative even when a deconfinement phase transition takes place at ρ ≤ ρ TOV , which is consistent with the recent studies assuming a smooth crossover from nuclear matter to quark matter [39,40].…”

Section: Introductionsupporting

confidence: 83%

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Deconfinement phase transition and quark condensate in compact stars

Hao-Miao¹,

Xia²,

Sun³

et al. 2022

Preprint

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We investigate systematically the possible deconfinement phase transition from nuclear matter to quark matter in compact stars. The properties of nuclear matter are fixed by expanding its binding energy to the order of ρ 3 , while those of quark matter are predicted by an equivparticle model. The Maxwell construction is then applied for the quark-hadron mixed phase. By confronting compact star structures with pulsar observations, we obtain several EOSs that are compatible with the latest observations while supporting quark cores inside the most massive stars. It is found that the quark core is rather small and does not emerge for compact stars with M 2M . The in-medium quark condensate of the stellar matter in those stars are then extracted within the framework of an equivparticle model, which decreases nonlinearly with density. At larger densities with pure quark matter, the quark condensate is still large and does not necessary decrease with density, indicating significant nonperturbative contributions within the density regions covered by compact stars.

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Section: Discussionsupporting

confidence: 89%

Section: Introductionsupporting

confidence: 83%

Deconfinement phase transition and quark condensate in compact stars

Hao-Miao¹,

Xia²,

Sun³

et al. 2022

Preprint

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“…This article is mostly a review of our works, Refs. [66][67][68], and it also presents improvements to the analyses of Refs. [66,68] with the up-to-date version of our PDM.…”

Section: Introductionmentioning

confidence: 99%

“…[66][67][68], and it also presents improvements to the analyses of Refs. [66,68] with the up-to-date version of our PDM. In Ref.…”

Section: Introductionmentioning

confidence: 99%

Chiral Restoration of Nucleons in Neutron Star Matter: Studies Based on a Parity Doublet Model

et al. 2023

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We review the chiral variant and invariant components of nucleon masses and the consequence of their existence on the chiral restoration in extreme conditions, particularly in neutron star matter. We consider a model of linear realization of chiral symmetry with the nucleon parity doublet structure that permits the chiral invariant mass, m0, for positive and negative parity nucleons. The nuclear matter is constructed with the parity doublet nucleon model coupled to scalar fields σ, vector fields (ω,ρ), and mesons with strangeness through the U(1)A anomaly. In models with a large m0, the nucleon mass is insensitive to the medium, and the nuclear saturation properties can be reproduced without demanding strong couplings of the nucleons to the scalar fields σ and vector fields ω. We confront the resulting nuclear equations of state with nuclear constraints and neutron star observations and delineate the chiral invariant mass and effective interactions. To further examine the nuclear equations of state beyond the saturation density, we supplement quark models to set the boundary conditions from the high-density side. The quark models are constrained by the two-solar-mass conditions, and such constraints are transferred to nuclear models through the causality and thermodynamic stability conditions. We also calculate various condensates and the matter composition from nuclear to quark matter in a unified matter by constructing a generating functional that interpolates the nuclear and quark matter with external fields. Two types of chiral restoration are discussed: one due to the positive scalar charges of nucleons and the other triggered by the evolution of the Dirac sea. We found that the U(1)A anomaly softens equations of state from low to high density.

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“…Actually, one can proceed further by extending the interpolation from physical EOS, P (µ B ), to a general generating function, P (µ B ; J), in which external sources J are coupled to various condensates and flavor densities. After constructing a unified functional with various sources, one can differentiate the functional with J to compute various quantities such as chiral and diquark condensates as well as flavor compositions [2]. This updates the 3-window modeling from thermodynamic quantities to more microscopic quantities which are not directly measured but are important to characterize the state of matter in dense QCD.…”

Section: Introduction Imentioning

confidence: 99%

Chiral condensates for neutron stars in hadron-quark crossover; from a parity doublet nucleon model to an NJL quark model

Takuya

Kojo²,

Harada³

2022

Supl. Rev. Mex. Fis.

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In this contribution, we summarize our recent studies on the chiral invariant mass and the chiral condensates in neutron star matter. We construct a unified equations of state assuming the crossover phase transition from hadronic matter described by a parity doublet model to quark matter by an Nambu--Jona-Lasinio type quark model. We first show that the chiral invariant mass is constrained to be $600\,\mbox{MeV}\, \lesssim\, m_0 \,\lesssim \, 900\,\mbox{MeV}$ from recent observations of neutron stars. We then determine the density dependence of the chiral condensate in the crossover description, and show that the chiral condensates are actually smoothly connected from the hadronic matter where the change is driven by the positive chiral scalar charge in a nucleon, to the quark matter where the change is by the modification of the quark Dirac sea, reflecting the hadron-quark crossover.

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Chiral condensates for neutron stars in hadron-quark crossover: From a parity doublet nucleon model to a Nambu–Jona-Lasinio quark model

Cited by 13 publications

References 129 publications

Deconfinement phase transition and quark condensate in compact stars

Deconfinement phase transition and quark condensate in compact stars

Chiral Restoration of Nucleons in Neutron Star Matter: Studies Based on a Parity Doublet Model

Chiral condensates for neutron stars in hadron-quark crossover; from a parity doublet nucleon model to an NJL quark model

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