Quark star matter in heavy quark stars

Abstract

We study the thermodynamic properties of asymmetric quark matter and large mass quark stars within the confined-isospin-density-dependent-quark-mass model. We find that the quark matter symmetry energy should be very large in order to describe the recent discovered heavy compact stars PSR J0348+0432 ($$\text {2.01}\pm \text {0.04}M_{\odot }$$ 2.01 ± 0.04 M ⊙ ), MSP J0740+6620 ($$\text {2.14}\pm ^\text {0.10}_\text {0.09}M_{\odot }$$ 2.14 ± 0.09 0.10 M ⊙ of 68.3$$\%$$ % credibility interval and $$\text {2.14}\pm ^\text {0.20}_\text {0.18}M_{\odot }$$ 2.14 ± 0.18 0.20 M ⊙ of 95.4$$\%$$ % credibility interval) and PSR J2215+5135 (2.27$$\pm ^\text {0.10}_\text {0.09}M_{\odot }$$ ± 0.09 0.10 M ⊙ ) as QSs. The tidal deformability $$\Lambda _{1.4}$$ Λ 1.4 of the QSs is also investigated in this work, and the result indicates that $$\Lambda _{1.4}$$ Λ 1.4 may depend on the isospin effects and the strength / orientation distribution of the magnetic fields inside the quark stars.

Properties of proto neutron star PSR J0737-3039A*

“…On this basis, they predicted the mass of the NS PSR J0737-3039A as 1.3374 M 1.3440 M in the framework of hybrid -gravity [9]. An NS has a high density, strong magnetic field, and high rotation speed [10][11][12][13][14][15][16]. Several massive NSs, PSR J1614-2230 [17,18], PSR J0348+0432 [19], and PSR J0740+ 6620 [20], have been observed in recent years.…”

Oscillating Magnetized Color Superconducting Quark Stars

“…Furthermore, these profiles are almost flat, and considering a surface value of B ∼ 10 15 Gausscorresponding to the observed MF surface values for magnetars-they do not allow reaching internal MF strength values much beyond this order of magnitude. This feature prevents reaching MFs of ∼ 10 17 -10 18 Gauss in the center of magnetars, values that emerge from magneto-hydrodynamics simulations (Igoshev et al, 2021;Pili et al, 2014;Frieben and Rezzolla, 2012;Naso et al, 2008); in particular, some works even suggest that the central MF in hybrid stars with quark matter in their cores could be as large as 10 19 Gauss (Sotani and Tatsumi, 2015) and in QSs could be as large as 10 20 Gauss (Ferrer et al, 2010;Chu et al, 2018Chu et al, , 2021.…”

Oscillating Magnetized Color Superconducting Quark Stars

“…Furthermore, these profiles are almost flat, and considering a surface value of B ∼ 10 15 Gauss-corresponding to the observed MF surface values for magnetars-they do not allow reaching internal MF strength values much beyond this order of magnitude. This feature prevents reaching MFs of ∼ 10 17 -10 18 Gauss in the center of magnetars, values that emerge from magneto-hydrodynamics simulations [39,41,42,53]; in particular, some works even suggest that the central MF in hybrid stars with quark matter in their cores could be as large as 10 19 Gauss [54] and in QSs could be as large as 10 20 Gauss [55][56][57].…”