Interacting 
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 and 
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 quark matter at finite densities and quark stars

Yuan, Wen-Li; Li, Ang; Miao, Zhiqiang; Zuo, Bing-Jun; Bai, Zhan

doi:10.1103/physrevd.105.123004

Cited by 20 publications

(2 citation statements)

References 104 publications

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“…While the negative vacuum pressure P(μ = 0; M) can be consistently calculated in NJL-type models (Buballa 2005), the results are unsatisfactory, due to the lack of confinement at vanishing density, as discussed in detail in Yuan et al (2022).…”

Section: Eosmentioning

confidence: 99%

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Two-flavor Color Superconducting Quark Stars May Not Exist

Yuan,

2024

ApJ

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Large uncertainties in the determinations of the equation of state of dense stellar matter allow for the intriguing possibility that the bulk quark matter in beta equilibrium might be the true ground state of the matter at zero pressure. Also, quarks will form Cooper pairs very readily since the dominant interaction between quarks is attractive in some channels. As a result, quark matter will generically exhibit color superconductivity, with the favored pairing pattern at intermediately high densities being two-flavor pairing. In the light of several possible candidates for such self-bound quark stars, including the very low-mass central compact object in supernova remnant HESS J1731-347 reported recently, we carry out a one-field theoretic model, the Nambu–Jona–Lasinio model, to investigate the stability of the beta-stable two-flavor color superconducting (2SC) phase of quark matter, but find no physically allowed parameter space for the existence of 2SC quark stars.

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Section: Eosmentioning

confidence: 99%

“…. See also the discussions inHoldom et al (2018),Zhou et al (2018),Ren & Zhang (2020), Zhang (2020),Li et al (2021b),Miao et al (2021), andYuan et al (2022). Correspondingly, the NJL-type model parameters should be chosen to ensure that the energy per baryon (E/A) of 2SC quark matter must be lower than 930 MeV, i.e., the E/A of the most stable iron nuclei.…”

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confidence: 99%

Two-flavor Color Superconducting Quark Stars May Not Exist

Yuan,

2024

ApJ

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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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Symmetry energy of strange quark matter and tidal deformability of strange quark stars

Xia

Lù

et al. 2022

NUCL SCI TECH

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Interacting ud and uds quark matter at finite densities and quark stars

Cited by 20 publications

References 104 publications

Two-flavor Color Superconducting Quark Stars May Not Exist

Two-flavor Color Superconducting Quark Stars May Not Exist

Quark stars in the pure pseudo-Wigner phase

Symmetry energy of strange quark matter and tidal deformability of strange quark stars

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