Phase transition and stiffer core fluid in neutron stars: Effects on stellar configurations, dynamical stability, and tidal deformability

Abstract

In this work, we investigate the influence of the phase transition and a stiffer fluid in neutron stars' cores on the static equilibrium configuration, dynamical stability, and tidal deformability. For this aim, it is taken into account that the fluid in the core and the envelope follow the relativistic polytropic equation of state. We find that the phase transition and a stiffer fluid in the core will reflect in the total mass, radius, speed of sound, core radius, radial stability with a slow and rapid conversion at the interface, and tidal deformability. We also investigate the dimensionless tidal deformability ${\Lambda }_1$ and ${\Lambda }_2$ for a binary neutron stars system with chirp mass equal to GW$170817$. Finally, we contrast our results with observational data to show the role that phase transition and a stiffer core fluid could play in the study of neutron stars.

To appear in EPJC

References in corpus (14)

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• Region of hadron-quark mixed phase in hybrid stars
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Cited by in corpus (4)

• Dark matter effects on hybrid star properties
• Dark energy effects on realistic neutron stars
• Quark confinement in an equiparticle quark model: application to stellar matter
• Exploring Temperature Influences on Gravitational Wave Production in Binary White Dwarfs