Structure of magnetized strange quark star in perturbative QCD

Sedaghat, J.; Zebarjad, S. M.; Bordbar, G. H.; Panah, B. Eslam

doi:10.1016/j.physletb.2022.137032

Cited by 13 publications

(3 citation statements)

References 58 publications

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“…Also, for the analysis that depends on a range of values for the dark fermion mass, magnetic field and the intensity of DM self-interaction, it is convenient to avoid other degrees of freedom in parameters that would be necessary in more realistic descriptions of the EoS, such as those relying on perturbative QCD [20,[37][38][39][40][41][42][43][44][45][46]. Even though results on perturbative magnetic QCD are available for very large magnetic fields [47,48], we postpone this analysis to a future publication.…”

Section: Introductionmentioning

confidence: 99%

Strange magnetars admixed with fermionic dark matter

Ferreira

Fraga

2023

J. Cosmol. Astropart. Phys.

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We discuss strange stars admixed with fermionic dark matter in the presence of a strong magnetic field using the two-fluid Tolman-Oppenheimer-Volkov equations. We describe strange quark matter using the MIT bag model and consider magnetic fields in the range ∼ 1017 - 1018 G. For the fermionic dark matter, we consider the cases of free particles and strongly self-interacting particles, with dark fermion masses m = 5, 100, 500 GeV. We discuss the effects of dark matter and a strong magnetic field on the masses and radii of the stars, as well as on its tidal deformability. Even though strong magnetic fields contribute to decreasing the total mass of the star, they attenuate the rate of decrease in the maximum mass brought about by increasing the dark matter fraction in the admixed system. The most intensely affected observable, however, is the tidal deformability, with variations on the range of 70%-90% for reasonable values of the magnetic field or dark matter central energy density.

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Section: Introductionmentioning

confidence: 99%

Strange magnetars admixed with fermionic dark matter

Ferreira

Fraga

2023

J. Cosmol. Astropart. Phys.

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“…Isolated nonaccreting neutron stars are cold, less than ~0.1 MeV, and after a few hundred years can be nearly isothermal [39]. For larger masses and higher pressures, a transition to a quark star can occur which may have spin or tidal deformation [40], strange quarks [41,42], magnetic field effects [43], or color superconductivity [44]. For the known transition temperature, there is a baryon chemical potential, or, equivalently, a density or pressure, where the phase transition will occur which can be described by the EoS [45] and, when considering the case of an isotropic density and pressure as source terms, can be described by the TOV equations.…”

Section: Introductionmentioning

confidence: 99%

The van der Waals Hexaquark Chemical Potential in Dense Stellar Matter

Andrew

Steinfelds

Andrew³

2023

Particles

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We explore the chemical potential of a QCD-motivated van der Waals (VDW) phase change model for the six-quark color-singlet, strangeness S = −2 particle known as the hexaquark with quark content (uuddss). The hexaquark may have internal structure, indicated by short range correlations that allow for non-color-singlet diquark and triquark configurations whose interactions will change the magnitude of the chemical potential. In the multicomponent VDW Equation of State (EoS), the quark-quark particle interaction terms are sensitive to the QCD color factor, causing the pairing of these terms to give different interaction strengths for their respective contributions to the chemical potential. This results in a critical temperature near 163 MeV for the color-singlet states and tens of MeV below this for various mixed diquark and triquark states. The VDW chemical potential is also sensitive to the number density, leading to chemical potential isotherms that exhibit spinodal extrema, which also depend upon the internal hexaquark configurations. These extrema determine regions of metastability for the mixed states near the critical point. We use this chemical potential with the chemical potential-modified TOV equations to investigate the properties of hexaquark formation in cold compact stellar cores in beta equilibrium. We find thresholds for hexaquark layers and changes in maximum mass values that are consistent with observations from high mass compact stellar objects such as PSR 09043 + 10 and GW 190814. In general, we find that the VDW-TOV model has an upper stability mass and radius bound for a chemical potential of 1340 MeV with a compactness of C~0.2.

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“…In light of the theory of E. Witten, the strange quark matter might be the ground state of strongly interacting matter [1,2], and many studies focused on strange quark stars (pure quark stars or hybrid neutron stars with quark cores) since then [3][4][5][6][7][8][9][10]. However, a recent study [11] proposed that the stable quark matter might not be strange, and nonstrange quark stars with large masses can exist.…”

Section: Introductionmentioning

confidence: 99%

The study of nonstrange quark stars within a modified NJL model

Li¹,

Zuo²,

Zhao³

et al. 2022

Preprint

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In this work, we employ a modified Nambu-Jona-Lasinio (NJL) model with proper-time regularization to study the structure of nonstrange quark stars. Considering the physical meaning of the four-fermion interaction coupling constant G in the conventional NJL model, we modify it by G = G1 + G2 ψψ to highlight the feedback of quark propagator to gluon propagator. To study the dependence of the equation of state (EOS) on this modification as well as the vacuum pressure, we choose nine representative EOSs for comparison. As a result, we find that a smaller G1 corresponds to a stiffer EOS, but at low energy densities, a higher vacuum pressure (i.e., a smaller bag constant) yields a softer one. Furthermore, the heaviest quark star obtained with the modified NJL model satisfies not only recent mass measurement of PSR J0740+6620, but also radius constraints from x-ray timing observations. The corresponding tidal deformability is also in agreement with GW170817.

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Structure of magnetized strange quark star in perturbative QCD

Cited by 13 publications

References 58 publications

Strange magnetars admixed with fermionic dark matter

Strange magnetars admixed with fermionic dark matter

The van der Waals Hexaquark Chemical Potential in Dense Stellar Matter

The study of nonstrange quark stars within a modified NJL model

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