The stifness of the supranuclear equation of state (once again)

Horvath, J. E.; Souza, Rodrigo Alvares de

doi:10.1088/1742-6596/861/1/012010

Cited by 2 publications

(1 citation statement)

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“…One key ingredient is the composition of the matter in colliding stars. Even within the standard picture, nucleons are hardly the only particle present, since hyperons are expected at certain inner density and explicitly considered for many years [10][11][12][13][14][15][16][17]. Even more exotic components have been considered, notably quark matter, both as a part of the innermost region of the stars or as an absolutely stable state (strange quark matter, SQM) composing essentially all the star up to the upper layers [18][19][20][21].…”

Section: Introductionmentioning

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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