Nonstrange quark stars from an NJL model with proper-time regularization

Wang, Qingwu; Shi, Chao; Zong, Hong-Shi

doi:10.1103/physrevd.100.123003

Cited by 35 publications

(26 citation statements)

References 54 publications

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“…However, recent studies demonstrated that up-down quark matter could be more stable than the strange quark matter and the ordinary nuclear matter [62,80]. Accordingly, it has been proposed that the compact stars involved in the binary merger events GW170817 and GW190814 may be the up-down quark stars (nonstrange quark stars) [59,[81][82][83][84]. Since theoretical predictions and astronomical observations cannot rule out the existence of non-strange quark stars, we will discuss the influence of chiral chemical potential on quark stars in the two flavor case.…”

Section: The Effects Of Chiral Chemical Potential On Quark Starsmentioning

confidence: 99%

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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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Section: The Effects Of Chiral Chemical Potential On Quark Starsmentioning

confidence: 99%

“…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%

A Brief Review of Chiral Chemical Potential and Its Physical Effects

et al. 2020

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“…Since the compactness increases with the mass, the tidal deformability becomes small for heavy stars with strong gravitational interactions, and it reaches the minimum value Λ min ≈ 23 at the maximum mass. The possibility that gravitational wave observations of coalescing neutron stars involve udQSs has been discussed in [19,22] for GW170817 from LIGO/Virgo [33]. In this paper, we extend the discussion to a newer event GW190425 [23], and constrain B eff together with other observations considering the transition rate estimation of neutron stars.…”

Section: Properties Of Udqm and Udqsmentioning

confidence: 80%

“…As a side remark, for the case that a crossing of nðpÞ curves occurs, the chemical potential difference μ H − μ Q starts to decrease above the crossing point with n H > n Q , referring to Eq. (22). At some higher pressure, μ H may become smaller than μ Q , indicating that the hadronic matter becomes more stable again.…”

Section: Conversion Of Neutron Stars and Astrophysical Observationsmentioning

confidence: 97%

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Quantum nucleation of up-down quark matter and astrophysical implications

Ren

Zhang

2020

Phys. Rev. D

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Quark matter with only u and d quarks (udQM) might be the ground state of baryonic matter at large baryon number A > A min. With A min ≳ 300, this has no direct conflict with the stability of ordinary nuclei. An intriguing test of this scenario is to look for quantum nucleation of udQM inside neutron stars due to their large baryon densities. In this paper, we study the transition rate of cold neutron stars to ud quark stars (udQSs) and the astrophysical implications, considering the relevant theoretical uncertainties and observational constraints. It turns out that a large portion of parameter space predicts an instantaneous transition, and so the observed neutron stars are mostly udQSs. We find this possibility still viable under the recent gravitational wave and pulsar observations, although there are debates on its compatibility with some observations that involve some complex structures of quark matter. The tension could be partially relieved in the two-families scenario, where the high-mass stars (M ≳ 2 M ⊙) are all udQSs and the low-mass ones (M ∼ 1.4 M ⊙) are mostly hadronic stars. In this case, the slow transition of the low-mass hadronic stars points to a very specific class of hadronic models with moderately stiff EOSs, and udQM properties are also strongly constrained.

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Quark stars in the pure pseudo-Wigner phase

Su,

Shi,

Huang

et al. 2024

Astrophys Space Sci

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In this paper, we take a different scenario of a pure quark star which is completely composed of quarks in the pseudo-Wigner phase. The equation of state (EOS) of deconfined quark stars is studied in the framework of the two-flavor 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, LR = (1 − α)L + αLF , to measure the weights of different interaction channels. We assume deconfinement 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 found to range 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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Nonstrange quark stars from an NJL model with proper-time regularization

Cited by 35 publications

References 54 publications

A Brief Review of Chiral Chemical Potential and Its Physical Effects

A Brief Review of Chiral Chemical Potential and Its Physical Effects

Quantum nucleation of up-down quark matter and astrophysical implications

Quark stars in the pure pseudo-Wigner phase

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