Rotating hybrid stars with the Dyson-Schwinger quark model

Wei, Jin-Biao; Chen, H.; Burgio, G. F.; Schulze, H.-J.

doi:10.1103/physrevd.96.043008

Cited by 15 publications

(11 citation statements)

References 99 publications

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“…We describe the quark phase in the DSM with an interaction parameter α = 1, 2, 3, 4 that models the quenching of the free quark-gluon vertex inside QM, see Refs. [44][45][46][47][48][49] for details. Increasing α leads to more stable QM in the DSM.…”

Section: Equations Of Statementioning

confidence: 99%

Neutron star universal relations with microscopic equations of state

Wei

Figura

Burgio

et al. 2019

J. Phys. G: Nucl. Part. Phys.

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We calculate neutron star's moment of inertia and deformabilities using various microscopic equations of state for nuclear and hybrid star configurations. We confirm several universal relations between the various observables in these cases. We focus in particular on the constraints for the neutron star radii imposed by a determination of the average tidal deformability of the binary neutron star system GW170817. We find compatible radii between 12 and 13 kilometers and identify the suitable equations of state.

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Section: Equations Of Statementioning

confidence: 99%

Neutron star universal relations with microscopic equations of state

Wei

Figura

Burgio

et al. 2019

J. Phys. G: Nucl. Part. Phys.

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“…In Refs. [27][28][29][30][31][32] and Refs. [33][34][35][36][37][38][39], the structure of the hybrid star is investigated with the DSEs and NJL model, respectively.…”

Section: Introductionmentioning

confidence: 99%

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

Zuo

Yan

et al. 2020

Phys. Rev. D

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In this work we use the equation of state (EOS) of (2+1)-flavor Nambu-Jona-Lasinio (NJL) model to study the structure of the strange quark star. With a new free parameter α, the Lagrangian is constructed by two parts, the original NJL Lagrangian and the Fierz transformation of it, asTo determine the range of α, we compare the binding energies in the 2-flavor and (2+1)-flavor cases. We also consider the constraints of chemical equilibrium and electric charge neutrality in the strange quark star and choose six representative EOSs with different α and B (bag constant) to study their influence on the structure of the strange quark star. As a result, we find that a smaller α or B corresponds to a heavier star with a stiffer EOS. Furthermore, the heaviest strange quark star is in agreement with both the recent mass observation of PSR J0740+6620 and the constraint on tidal deformability of GW170817.

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“…The total density and pressure of the QM are given by summing contributions from all flavors, and the pressure of QM at zero density is taken as a phenomenological bag constant [72],…”

Section: B Quark Mattermentioning

confidence: 99%

The equation of state and radial oscillations of neutron stars

Sun,

Zheng,

Chen

et al. 2021

Preprint

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We investigate radial oscillations of pure neutron stars and hybrid stars, employing equations of state of nuclear matter from Brueckner-Hartree-Fock theory, and of quark matter from the Dyson-Schwinger quark model, performing a Gibbs construction for the mixed phase in hybrid stars. We calculate the eigenfrequencies and corresponding oscillation functions. Our results for the zero points of the first-order radial oscillation frequencies give the maximum mass of stable neutron stars, consistent with the common criterion dM/dρ c = 0. Possible observations of the radial oscillation frequencies could help to learn more about the equation of state, predict the maximum mass of neutron stars more precisely, and indicate the presence of quark matter.

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Rotating hybrid stars with the Dyson-Schwinger quark model

Cited by 15 publications

References 99 publications

Neutron star universal relations with microscopic equations of state

Neutron star universal relations with microscopic equations of state

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

The equation of state and radial oscillations of neutron stars

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