Revisiting the equation of state of hybrid stars in the Dyson-Schwinger equation approach to QCD

Bai, Zhan; Chen, Huan; Liu, Yuxin

doi:10.1103/physrevd.97.023018

Cited by 23 publications

(20 citation statements)

References 137 publications

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“…In this work, the possible appearance of hyperons in the dense star matter is not considered, because it prevents from the happening of the hadron-quark phase transition. This problem can be fixed by implementing the 3-window construction method instead of the Gibbs and Maxwell constructions, as has been done in our previous work [127].…”

Section: Discussionmentioning

confidence: 99%

“…The DS equations include in fact an infinite number of coupled integral equations, and in order to solve them, one must take truncation [102][103][104][105][106][107][108][109] and model the dressed gluon propagator [110][111][112][113]. The DS equation approach has been taken to study the phase transition and the CEP [15][16][17][18][19][20][21][22]25,26,[114][115][116][117][118][119][120], and also been used to study the cold dense matter [121][122][123][124][125][126][127].…”

Section: (): V-volmentioning

confidence: 99%

“…We consider two types of the modification function. The first one is a monotonically decreasing function, which has already been used in previous works [122][123][124]126,127]. However, in the earlier works, the modification function includes a free parameter which controls the speed of quark matter approaching the asymptotic freedom.…”

Section: (): V-volmentioning

confidence: 99%

“…Previously, in the study of compact star matter, an exponentially damping function was proposed [122][123][124]126,127] as:…”

Section: Modification For the Gluon Modelmentioning

confidence: 99%

“…In general, a larger coupling constant D corresponds to a larger quark mass function M( p), and a larger critical chemical potential. Meanwhile, it reduces the value μ B,c for the phase transition to happen [127]. However, for some vertex and gluon propagator, the μ B,c might be less than 923 MeV (see, e.g.…”

Section: Modification For the Gluon Modelmentioning

confidence: 99%

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QCD phase transition and equation of state of stellar strong interaction matter via Dyson–Schwinger equation approach

Bai

Liu

2021

Eur. Phys. J. C

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We study the phase structure and phase transition of cold dense QCD matter via the Dyson–Schwinger equation approach. We take the rainbow approximation and the Gaussian-type gluon model. In order to guarantee that the quark number density begins to appear at the nuclear liquid-gas phase transition chemical potential, we propose a chemical potential dependent modification factor for the gluon model. We find that for the iso-symmetric quark matter, the modification reduces the chemical potential of the phase coexistence region of the first-order phase transition. We also implement the relativistic mean field theory to describe the hadron matter, and make use of the Maxwell and Gibbs construction method to study the phase transition of $$\beta $$ β -equilibrium and charge neutral matter in compact stars. The results show that the phase transition will not happen in case of the Gaussian-type gluon model without any modification. The results also indicate that the upper boundary of the coexistence region should be larger than the current Nambu solution existing region. We also calculate the mass-radius relation of the compact stars, and find that the hadron-quark phase transition happens at too high chemical potential so that the maximum mass of the compact star is hardly affected by the hadron-quark phase transition.

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Section: Discussionmentioning

confidence: 99%

Section: (): V-volmentioning

confidence: 99%

Section: (): V-volmentioning

confidence: 99%

“…Previously, in the study of compact star matter, an exponentially damping function was proposed [122][123][124]126,127] as:…”

Section: Modification For the Gluon Modelmentioning

confidence: 99%

Section: Modification For the Gluon Modelmentioning

confidence: 99%

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QCD phase transition and equation of state of stellar strong interaction matter via Dyson–Schwinger equation approach

Bai

Liu

2021

Eur. Phys. J. C

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Note on neutron star equation of state in the light of GW170817

Zhu

2019

AIP Conference Proceedings

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From the very first multimessenger event of GW170817, clean robust constraints can be obtained for the tidal deformabilities of the two stars involved in the merger, which provides us unique opportunity to study the equation of states (EOSs) of dense stellar matter. In this contribution, we employ a model from the quark level, describing consistently a nucleon and manybody nucleonic system from a quark potential. We check that our sets of EOSs are consistent with available experimental and observational constraints at both sub-nuclear saturation densities and higher densities. The agreements with ab-initio calculations are also good. Especially, we tune the density dependence of the symmetry energy (characterized by its slope at nuclear saturation L) and study its influence on the tidal deformability. The so-called QMF18 EOS is named after the case of L = 40 MeV, and it gives M TOV = 2.08 M and R = 11.77 km, Λ = 331 for a 1.4 M star. The tidal signals are demonstrated to be insensitive to the uncertainty on the crust-core matching, despite the good correlation between the symmetry energy slope and the radius of the star.

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Delineating the properties of matter in cold, dense QCD

Kojo

2019

AIP Conference Proceedings

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The properties of dense QCD matter are delineated through the construction of equations of state which should be consistent with the low and high density limits of QCD, nuclear laboratory experiments, and the neutron star observations. These constraints, together with the causality condition of the sound velocity, are used to develop the picture of hadron-quark continuity in which hadronic matter continuously transforms into quark matter (modulo small 1st order phase transitions). The resultant unified equation of state at zero temperature and β -equilibrium, which we call Quark-Hadron-Crossover (QHC19), is consistent with the measured properties of neutron stars as well as the microphysics known for the hadron phenomenology. In particular to ∼ 10n 0 (n 0 : saturation density) the gluons remain as non-perturbative as in vacuum and the strangeness can be as abundant as up-and down-quarks at the core of two-solar mass neutron stars. Within our modeling the maximum mass is found less than 2.35 times solar mass and the baryon density at the core ranges in ∼ 5-8n 0 .

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Revisiting the equation of state of hybrid stars in the Dyson-Schwinger equation approach to QCD

Cited by 23 publications

References 137 publications

QCD phase transition and equation of state of stellar strong interaction matter via Dyson–Schwinger equation approach

QCD phase transition and equation of state of stellar strong interaction matter via Dyson–Schwinger equation approach

Note on neutron star equation of state in the light of GW170817

Delineating the properties of matter in cold, dense QCD

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