New algorithm to study the pseudo-Wigner solution of the quark gap equation in the framework of the (
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)-flavor NJL model

Li, Chengming; Yin, Peng; Zong, Hong-Shi

doi:10.1103/physrevd.99.076006

Cited by 10 publications

(2 citation statements)

References 52 publications

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“…In this paper, the two-flavor Nambu-Jona-Lasinio(NJL) model [19][20][21][22][23][24][25][26][27][28][29] is used to describe the quark matter in neutron stars, and it is established to manifest the dynamical spontaneously breaking of chiral symmetry, where the effective quark mass is acquired at low densities. As the chemical potential increases, the chiral phase transition occurs and the chiral symmetry begins to restore, which is associated with the fact that the hadronic matter transits to the quark matter, corresponding to the Nambu phase and the pseudo-Wigner phase respectively [30,31]. Consequently, the bag constant B is defined as the difference of pressure between the trivial vacuum pressure of the pseudo-Wigner phase and the non-trivial vacuum pressure of the Nambu phase [30][31][32], as originated from the MIT bag model.…”

Section: Introductionmentioning

confidence: 99%

“…As the chemical potential increases, the chiral phase transition occurs and the chiral symmetry begins to restore, which is associated with the fact that the hadronic matter transits to the quark matter, corresponding to the Nambu phase and the pseudo-Wigner phase respectively [30,31]. Consequently, the bag constant B is defined as the difference of pressure between the trivial vacuum pressure of the pseudo-Wigner phase and the non-trivial vacuum pressure of the Nambu phase [30][31][32], as originated from the MIT bag model. To obtain the EOS of quark stars, the model-independent pressure [33,34] for quark matter is contributed from the particles and the vacuum,…”

Section: Introductionmentioning

confidence: 99%

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The chiral restored quark stars can exist in the universe

Su,

Yan,

et al. 2021

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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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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

The chiral restored quark stars can exist in the universe

Su,

Yan,

et al. 2021

Preprint

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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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Do current astronomical observations exclude the existence of nonstrange quark stars?

et al. 2019

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As is pointed out in a recent work (Phys. Rev. Lett. 120, 222001), quark matter may not be strange. Inspired by this argument, we use a new self-consistent mean field approximation method to study the equation of state of cold dense matter within the framework of the two-flavor NJL model. Then the mass-radius relationship of twoflavor pure quark stars is studied. In the new self-consistent mean field approximation method we introduced, there is a free parameter α, which reflects the weight of different interaction channels. In principle, α should be determined by experiments rather than the self-consistent mean field approximation itself. In this paper, thus, the influence of the variation of α on the critical chemical potential of chiral phase transition and the stiffness of the EOS are thoroughly explored. The stiffness of the EOS can be increased greatly to support a two-solar-mass pure quark star when α is greater than 0.9, because the contribution from the vector term is retained by the Fierz transformation. Our result is also within the constraints on the radius from the recent data analysis of the tidal deformability. This means that the current theoretical calculations and astronomical observations cannot rule out the possibility of a two-flavor pure quark star.

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New algorithm to study the pseudo-Wigner solution of the quark gap equation in the framework of the ( 2+1 )-flavor NJL model

Cited by 10 publications

References 52 publications

The chiral restored quark stars can exist in the universe

The chiral restored quark stars can exist in the universe

Quark stars in the pure pseudo-Wigner phase

Do current astronomical observations exclude the existence of nonstrange quark stars?

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