Strange Star Equations of State Revisited

Menezes, D. P.; Melrose, D. B.

doi:10.1071/as05022

Cited by 10 publications

(24 citation statements)

References 41 publications

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“…In [25] we investigated the properties of strange stars using two different models: the MIT bag model [26], which is widely favored in the literature on strange stars, and the color-favor-locked phase (CFL) model [27], which allows the quarks near the Fermi surface to form Cooper pairs which condense and break the color gauge symmetry [28]. At sufficiently high density the favored phase is called CFL, in which quarks of all three colors and all three flavors are allowed to pair.…”

mentioning

confidence: 99%

Quark stars within relativistic models

Menezes¹,

Providência²,

Melrose³

2006

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

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Lately, it has been suggested that strange (quark) stars can be responsible for glitches and other observational features of pulsars. Some discussions on whether quark stars, if really exist, are bare or crusted are also a source of controversy in the recent literature. In the present work we use the Nambu-Jona-Lasinio model, known to incorporate chiral symmetry, necessarily present in the QCD formalism, in order to describe quark star properties. We compare our results for the stars and the features of the model with the much simpler model normally used in the description of strange stars, namely the MIT bag model. We also investigate the differences in the stellar properties which arise due to the presence of the crust. We show that the NJL model produces results which are somewhat different as compared with the MIT model. PACS number(s): 26.60.+c,24.10.Jv, 21.65.+f,95.30.Tg

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mentioning

confidence: 99%

Quark stars within relativistic models

Menezes¹,

Providência²,

Melrose³

2006

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

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“…The influence of the temperature was also investigated by means of fixed entropy per baryon. The charge effect does not alter previous conclusions related to the mass and radius behavior of protoneutron stars with larger entropy [8,10]. …”

Section: Results and Conclusionmentioning

confidence: 55%

“…4, 5 and 6-7. For quark stars we present two sets of calculations, one for EoS obtained with the MIT bag model and another one for EoS obtained with the Nambu-Jona-Lasinio model because their strangeness compositions are very different, as seen in [10]. Some considerations are now in order: in building EoS that describe stellar matter, β-equilibrium and charge neutrality are always required since compact star properties are not affected by electric fields below 10 20 V /m.…”

Section: A Electrically Charged Compact Starsmentioning

confidence: 99%

“…We have calculated the results for 48 different configuration models of compact stars. The EoS for hadronic and hybrid stars were taken from [8], the EoS for quark stars were taken from [10]. In table I the electric charge Q is given in Coulomb and f varies from zero (no charge) to a small value (0.0006).…”

Section: A Electrically Charged Compact Starsmentioning

confidence: 99%

“…Some of the possibilities are the presence of hyperons [1][2][3], a mixed phase of hyperons and quarks [4][5][6][7][8], a phase of deconfined quarks or pion and kaon condensates [9]. Another possibility would be that pulsars are, in fact, quark stars [10]. In conventional models, hadrons are assumed to be the true ground state of the strong interaction.…”

Section: Introductionmentioning

confidence: 99%

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Electrically charged pulsars

Alloy

Menezes

2007

Braz. J. Phys.

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In the present work we investigate one possible variation on the usual electrically neutral pulsars: the inclusion of electric charge through a naive prescription. We study the effect of electric charge in pulsars assuming that the charge distribution is proportional to the energy density. All calculations were performed for equations of state obtained at zero temperature and also for fixed entropies. We then choose one of the models, the Nambu-JonaLasinio model for zero temperature quark stars without the inclusion of leptons, what makes them electrically charged, and compare the results with the previous one.

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γ-ray bursts and the QCD phase diagram

et al. 2006

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The quantum chromodynamics phase diagram shows the phase transitions that can take place in matter at different temperatures and densities. In this work we discuss the possibility that γ -ray bursts might result from a phase change in the interior of a neutron star and calculate the energy released in the conversion of a metastable star into a stable star. We consider several different initial and several different final configurations. Initial metastable stars are taken as hadronic, hybrid, and quark stars with unpaired quarks; possible stable stars are hybrid and quark stars, taken both with unpaired and paired phases to study the deconfinement phase transition and normal quark matter-superconducting quark matter phase transition within a large number of relativistic models used to describe compact stars. The models used for the hadron matter are the nonlinear Walecka model and the quark-meson coupling model with and without hyperons. For the quark matter we have used the MIT bag model, the bag model with paired quarks to which we refer as the color-flavor-locked phase model, and the Nambu-Jona-Lasinio model. Within this mechanism we obtain energies of the order of 10 50 −10 53 erg, accounting for both long and short γ -ray bursts.

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Strange Star Equations of State Revisited

Cited by 10 publications

References 41 publications

Quark stars within relativistic models

Quark stars within relativistic models

Electrically charged pulsars

γ-ray bursts and the QCD phase diagram

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