Electrically charged strange stars with an interacting quark matter equation of state

Gonçalves, V. P.; Lazzari, Lucas

doi:10.1103/physrevd.102.034031

Cited by 20 publications

(24 citation statements)

References 45 publications

(75 reference statements)

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“…In particular, in Ref. [30], two of the authors have studied the properties of charged strange stars considering an EoS based on perturbative QCD and demonstrated that the presence of an electric charge distribution implies that the maximum mass is larger in comparison to the neutral counterpart, in agreement with the results obtained in Ref. [32] using a simplified approach (see also Refs.…”

Section: Introductionsupporting

confidence: 77%

“…In this section, we will present a brief review of the theoretical framework necessary to investigate electrically charged compact stars (see Refs. [30][31][32]34,35] for extensive details). Initially, we will present the electrically-charged structure equations and the model for the electric charge distribution used in this work.…”

Section: Frameworkmentioning

confidence: 99%

“…In the last years, several authors have discussed the basic structure equations needed to derive the properties of a charged compact star [30][31][32]34,35]. In our analysis, we will assume a static and spherically symmetric charged star.…”

Section: Charged Stellar Structure Equationsmentioning

confidence: 99%

“…Ref. [30], one finds that the Einstein-Maxwell field equations imply that the charged stellar structure is determined by the following system of equations…”

Section: Charged Stellar Structure Equationsmentioning

confidence: 99%

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Electrically charged supermassive twin stars

2022

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By assuming that ultra dense hybrid neutron stars are endowed with a distribution of electric charge, we study the corresponding twin star solutions and their properties resulting from a sharp first order transition from confined hadronic to a deconfined quark phase. Two distinct quark matter equations of state with increasing stiffness are considered and the values for the maximum gravitational masses of the hadronic and hybrid twin configurations are obtained for different values of the total electric charge. Interestingly, our calculations indicate that sharp transitions make charged twin hybrid stars more massive than their neutral counterparts, and that the $${2}\,{\hbox {M}_{\odot }}$$ 2 M ⊙ constraint from PSR J0740+6620 is surpassed for standard values of electric charge and can be considered stable only satisfying $$\partial M/\partial \epsilon _0 > 0$$ ∂ M / ∂ ϵ 0 > 0 . In particular, our charged stellar models reach masses even higher than the unknown compact object measured in the GW190814 event.

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Section: Introductionsupporting

confidence: 77%

Section: Frameworkmentioning

confidence: 99%

Section: Charged Stellar Structure Equationsmentioning

confidence: 99%

“…Ref. [30], one finds that the Einstein-Maxwell field equations imply that the charged stellar structure is determined by the following system of equations…”

Section: Charged Stellar Structure Equationsmentioning

confidence: 99%

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Electrically charged supermassive twin stars

2022

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“…On the other hand, the possibility for GW190814's secondary as a neutron star can be accomplished by: (1) choosing/constructing stiff EOSs having a maximum mass larger than 2.5 M [76,[141][142][143][144][145][146][147][148][149][150]; (2) considering the effects of fast rotations, which can increase the maximum mass by about 20% when a star rotates at the Kepler frequency (the maximum frequency at which the gravitational attraction is still sufficient to keep matter bound to the pulsar surface) [42,43,139,140,145,[151][152][153][154][155][156][157] ; (3) considering other effects/models that can modify the maximum mass of a neutron star, such as the magnetic field [147], twin star [158], two families of compact stars [142], finite temperature [153], antikaon condensation [159], net electric charge [144], etc.…”

Section: Is Gw190814's Secondary a Superfast And Supermassive Neutron Star Or Something Else?mentioning

confidence: 99%

Progress in Constraining Nuclear Symmetry Energy Using Neutron Star Observables Since GW170817

Cai²,

Wang

et al. 2021

Universe

138

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The density dependence of nuclear symmetry energy is among the most uncertain parts of the Equation of State (EOS) of dense neutron-rich nuclear matter. It is currently poorly known especially at suprasaturation densities partially because of our poor knowledge about isovector nuclear interactions at short distances. Because of its broad impacts on many interesting issues, pinning down the density dependence of nuclear symmetry energy has been a longstanding and shared goal of both astrophysics and nuclear physics. New observational data of neutron stars including their masses, radii, and tidal deformations since GW170817 have helped improve our knowledge about nuclear symmetry energy, especially at high densities. Based on various model analyses of these new data by many people in the nuclear astrophysics community, while our brief review might be incomplete and biased unintentionally, we learned in particular the following: (1) The slope parameter L of nuclear symmetry energy at saturation density ρ0 of nuclear matter from 24 new analyses of neutron star observables was about L≈57.7±19 MeV at a 68% confidence level, consistent with its fiducial value from surveys of over 50 earlier analyses of both terrestrial and astrophysical data within error bars. (2) The curvature Ksym of nuclear symmetry energy at ρ0 from 16 new analyses of neutron star observables was about Ksym≈−107±88 MeV at a 68% confidence level, in very good agreement with the systematics of earlier analyses. (3) The magnitude of nuclear symmetry energy at 2ρ0, i.e., Esym(2ρ0)≈51±13 MeV at a 68% confidence level, was extracted from nine new analyses of neutron star observables, consistent with the results from earlier analyses of heavy-ion reactions and the latest predictions of the state-of-the-art nuclear many-body theories. (4) While the available data from canonical neutron stars did not provide tight constraints on nuclear symmetry energy at densities above about 2ρ0, the lower radius boundary R2.01=12.2 km from NICER’s very recent observation of PSR J0740+6620 of mass 2.08±0.07M⊙ and radius R=12.2–16.3 km at a 68% confidence level set a tight lower limit for nuclear symmetry energy at densities above 2ρ0. (5) Bayesian inferences of nuclear symmetry energy using models encapsulating a first-order hadron–quark phase transition from observables of canonical neutron stars indicated that the phase transition shifted appreciably both L and Ksym to higher values, but with larger uncertainties compared to analyses assuming no such phase transition. (6) The high-density behavior of nuclear symmetry energy significantly affected the minimum frequency necessary to rotationally support GW190814’s secondary component of mass (2.50–2.67) M⊙ as the fastest and most massive pulsar discovered so far. Overall, thanks to the hard work of many people in the astrophysics and nuclear physics community, new data of neutron star observations since the discovery of GW170817 have significantly enriched our knowledge about the symmetry energy of dense neutron-rich nuclear matter.

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A stellar model with anisotropic fluid and Chaplygin equation of state

Sunzu

Mathias

2022

Indian J Phys

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Electrically charged strange stars with an interacting quark matter equation of state

Cited by 20 publications

References 45 publications

Electrically charged supermassive twin stars

Electrically charged supermassive twin stars

Progress in Constraining Nuclear Symmetry Energy Using Neutron Star Observables Since GW170817

A stellar model with anisotropic fluid and Chaplygin equation of state

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