Bag versus NJL models for colour–flavour-locked strange quark matter

Paulucci, L.; Ferrer, Efrain J.; Horvath, J. E.; Incera, Vivian de la

doi:10.1088/0954-3899/40/12/125202

Cited by 15 publications

(14 citation statements)

References 33 publications

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“…When considering CFL matter through a Nambu-Jona-Lasinio (NJL) model with four-fermion interactions at finite density, other interactions, besides the diquark channel [37], can also be considered. Among these additional channels of interactions, vector interactions [38,39] are the most relevant as they can significantly affect the stiffness of the EOS, and hence they will be considered in our analysis.…”

Section: Modelling Of Self-bound Compact Starsmentioning

confidence: 99%

Tidal deformability of strange stars and the GW170817 event

Lourenço,

Lenzi,

Dutra

et al. 2021

Preprint

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In this work we consider strange stars formed by quark matter in the color-flavor-locked (CFL) phase of color superconductivity. The CFL phase is described by a Nambu-Jona-Lasinio model with four-fermion vector and diquark interaction channels. The effect of the color superconducting medium on the gluons are incorporated into the model by including the gluon self-energy in the thermodynamic potential. We construct parametrizations of the model by varying the vector coupling GV and comparing the results to the data on tidal deformability from the GW170817 event, the observational data on maximum masses from massive pulsars such as the MSP J0740+6620, and the mass/radius fits to NICER data for PSR J003+0451. Our results points out to windows for the GV parameter space of the model, with and without gluon effects included, that are compatible with all these astrophysical constraints, namely, 0.21 < GV /GS < 0.4, and 0.02 < GV /GS < 0.1, respectively. We also observe a strong correlation between the tidal deformabilites of the GW170817 event and GV . Our results indicate that strange stars cannot be ruled out in collisions of compact binaries from the structural point of view.

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Section: Modelling Of Self-bound Compact Starsmentioning

confidence: 99%

Tidal deformability of strange stars and the GW170817 event

Lourenço,

Lenzi,

Dutra

et al. 2021

Preprint

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“…8 in [15]). However, when other interactions, also present in a dense medium of quarks [42], such as the diquark channel [43] and/or the vector channel, were taken into account, the EOS stiffened enough to meet the 2M challenge. Because of these findings, quark matter was back in the competition as a possible core phase of massive stars (see for instance [44][45][46]).…”

Section: Inhomogeneous Quark Matter In the Core Of Compact Starsmentioning

confidence: 99%

Crystalline chiral condensates as a component of compact stars

et al. 2015

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We investigate the influence of spatially inhomogeneous chiral symmetry-breaking condensates in a magnetic field background on the equation of state for compact stellar objects. After building a hybrid star composed of nuclear and quark matter using the Maxwell construction, we find, by solving the Tolman-Oppenheimer-Volkoff equations for stellar equilibrium, that our equation of state supports stars with masses around 2 M for values of the magnetic field that are in accordance with those inferred from magnetar data. The inclusion of a weak vector interaction term in the quark part allows one to reach 2 solar masses for relatively small central magnetic fields, making this composition a viable possibility for describing the internal degrees of freedom of this class of astrophysical objects.arXiv:1505.05094v2 [nucl-th]

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“…It can be observed that the splitting between the EoS for different ∆'s is more significant for the values introduced in the MIT model than in those obtained in the NJL model, although they are really significant only for high gap values. As it was found in [18], in the MIT case, the higher the gap, the stiffer the EoS. Hence, as the mass supported by a given star configuration is related to the stiffness of the EoS, a higher value of the gap renders higher maximum masses for stable strange stars [8].…”

Section: Bag Vs Njl Model In the Cfl Phasementioning

confidence: 64%

Equations of State of different phases of dense quark matter

Ferrer

2017

J. Phys.: Conf. Ser.

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Compact stars with significant high densities in their interiors can give rise to quark deconfined phases that can open a window for the study of strongly interacting dense nuclear matter. Recent observations on the mass of two pulsars, PSR J1614-2230 and PSR J0348+0432, have posed a great restriction on their composition, since their equations of state must be hard enough to support masses of about at least two solar masses. The onset of quarks tends to soften the equation of state, but due to their strong interactions, different phases can be realized with new parameters that affect the corresponding equations of state and ultimately the mass-radius relationships. In this paper I will review how the equation of state of dense quark matter is affected by the physical characteristics of the phases that can take place at different baryonic densities with and without the presence of a magnetic field, as well as their connection with the corresponding mass-radius relationship, which can be derived by using different models.

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Bag versus NJL models for colour–flavour-locked strange quark matter

Cited by 15 publications

References 33 publications

Tidal deformability of strange stars and the GW170817 event

Tidal deformability of strange stars and the GW170817 event

Crystalline chiral condensates as a component of compact stars

Equations of State of different phases of dense quark matter

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