Strange quark stars within proper time regularized (
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)-flavor NJL model

Li, Cheng-Ming; Zuo, Shu-Yu; Yan, Yan; Zhao, Ya-Peng; Wang, Fei; Huang, Yun‐Feng; Zong, Hong-Shi

doi:10.1103/physrevd.101.063023

Cited by 28 publications

(19 citation statements)

References 68 publications

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“…2. This requires a correc- tion to be added to the calculation of y R to account for the energy discontinuity between the star's surface and its outside, reading [69][70][71][72] y…”

Section: Numerical Results and The Gw170817 Eventmentioning

confidence: 99%

Tidal deformability of strange stars and the GW170817 event

Lourenço,

Lenzi,

Dutra

et al. 2021

Preprint

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In this work we consider strange stars formed by quark matter in the color-flavor-locked (CFL) phase of color superconductivity. The CFL phase is described by a Nambu-Jona-Lasinio model with four-fermion vector and diquark interaction channels. The effect of the color superconducting medium on the gluons are incorporated into the model by including the gluon self-energy in the thermodynamic potential. We construct parametrizations of the model by varying the vector coupling GV and comparing the results to the data on tidal deformability from the GW170817 event, the observational data on maximum masses from massive pulsars such as the MSP J0740+6620, and the mass/radius fits to NICER data for PSR J003+0451. Our results points out to windows for the GV parameter space of the model, with and without gluon effects included, that are compatible with all these astrophysical constraints, namely, 0.21 < GV /GS < 0.4, and 0.02 < GV /GS < 0.1, respectively. We also observe a strong correlation between the tidal deformabilites of the GW170817 event and GV . Our results indicate that strange stars cannot be ruled out in collisions of compact binaries from the structural point of view.

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“…2. This requires a correc- tion to be added to the calculation of y R to account for the energy discontinuity between the star's surface and its outside, reading [69][70][71][72] y…”

Section: Numerical Results and The Gw170817 Eventmentioning

confidence: 99%

Tidal deformability of strange stars and the GW170817 event

Lourenço,

Lenzi,

Dutra

et al. 2021

Preprint

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“…where B is the bag constant of MIT bag model [59,81,85]. Plugging the solutions we obtained into Equation (52), we can get the EOSs of quark stars.…”

Section: The Effects Of Chiral Chemical Potential On Quark Starsmentioning

confidence: 99%

“…Our previous works have investigated the effects of α on the EOS and the properties of quark stars [59,81,85]. The larger α leads to stiffer EOS and larger maximum mass of quark star.…”

Section: The Effects Of Chiral Chemical Potential On Quark Starsmentioning

confidence: 99%

A Brief Review of Chiral Chemical Potential and Its Physical Effects

et al. 2020

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Nontrivial topological gluon configuration is one of the remarkable features of the Quantum Chromodynamics (QCD). Due to chiral anomaly, the chiral imbalance between right- and left-hand quarks can be induced by the transition of the nontrivial gluon configurations between different vacuums. In this review, we will introduce the origin of the chiral chemical potential and its physical effects. These include: (1) the chiral imbalance in the presence of strong magnetic and related physical phenomena; (2) the influence of chiral chemical potential on the QCD phase structure; and (3) the effects of chiral chemical potential on quark stars. Moreover, we propose for the first time that quark stars are likely to be a natural laboratory for testing the destruction of strong interaction CP.

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“…In Refs. [13,14,35], the vacuum pressure P(µ = 0) is set as −B to confine quark matter at zero chemical potential. However, the boundary condition of the Tolman-Oppenheimer-Volkoff (TOV) equation with zero pressure on the surface of quark stars leads to the possibility that hadronic matter may exist on the surface.…”

Section: Introductionmentioning

confidence: 99%

“…Note that the previous work of Refs. [13,14,35] mainly studied hybrid stars. The EOS there is not for two-flavor quark stars but for hybrid stars, which attempts to describe hybrid stars from the equivalent quark model.…”

Section: Introductionmentioning

confidence: 99%

The chiral restored quark stars can exist in the universe

Su,

Yan,

et al. 2021

Preprint

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In this paper, the equation of state (EOS) of deconfined quark stars is studied in the framework of the twoflavor NJL model, and the self-consistent mean field approximation is employed by introducing a parameter α combining the original Lagrangian and the Fierz-transformed Lagrangian, L R = (1 − α)L + αL F , to measure the weights of different interaction channels. It is believed that the deconfinement of phase transition happens along with the chiral phase transition. Thus, due to the lack of description of confinement in the NJL model, the vacuum pressure is set to confine quarks at low densities, which is the pressure corresponding to the critical point of chiral phase transition. We find that deconfined quark stars can reach over two-solar-mass, and the bag constant therefore shifts from (130 MeV) 4 to (150 MeV) 4 as α grows. In addition, the tidal deformability Λ is yielded ranging from 253 to 482 along with the decrease of α, which satisfies the astronomical constraint of Λ < 800 for 1.4-solar-mass neutron stars.

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Strange quark stars within proper time regularized ( 2+1 )-flavor NJL model

Cited by 28 publications

References 68 publications

Tidal deformability of strange stars and the GW170817 event

Tidal deformability of strange stars and the GW170817 event

A Brief Review of Chiral Chemical Potential and Its Physical Effects

The chiral restored quark stars can exist in the universe

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