Analytical model on mass limits of strange stars

Molla, Sajahan; Murshid, Masum; Kalam, Mehedi

doi:10.1007/s10509-021-04035-0

Astrophys Space Sci

2022

DOI: 10.1007/s10509-021-04035-0

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Analytical model on mass limits of strange stars

Sajahan Molla

Masum Murshid

Mehedi Kalam

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Cited by 2 publications

References 57 publications

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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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Quark stars in the pure pseudo-Wigner phase

Su,

Shi,

Huang

et al. 2024

Astrophys Space Sci

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A regular interior solution of Einstein field equations

Estevez-Delgado

Duran³

et al. 2023

Can. J. Phys.

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Starting from the solution of the Einstein field equations in a static and spherically symmetric spacetime which contains an isotropic fluid, we construct a model to represent the interior of compact objects with compactness rate u=GM/(c2R )<0.23577. The solution is obtained by imposing the isotropy condition for the radial and tangential pressures, this generates an ordinary differential equation of second order for the temporal gtt and radial grr metric potentials, which can be solved for a specific function of gtt. The graphic analysis of the solution shows that it is physically acceptable, that is to say, the density, pressure and speed of sound are positive, regular and monotonically decreasing functions, also, the solution is stable due to meeting the criteria of the adiabatic index. When taking the data of mass M=1.44+0.15-0.14M⊙ and radius R=13.02+1.24-1.06 km which corresponds to the estimations of the star PSR J0030+045 we obtain values of central density ρc=7.5125x1017 kg/m3 for the maximum compactness u=0.19628 and of ρc=2.8411x1017 kg/m3 for the minimum compactness u=0.13460, which are consistent with those expected for this type of stars.

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Analytical model on mass limits of strange stars

Cited by 2 publications

References 57 publications

Quark stars in the pure pseudo-Wigner phase

Quark stars in the pure pseudo-Wigner phase

A regular interior solution of Einstein field equations

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