Dark energy effects on realistic neutron stars

TL;DR

This paper investigates how a dark energy core modeled by Chaplygin Dark Fluid affects neutron star properties, including mass, radius, and stability, using realistic equations of state and observational data.

Contribution

It introduces a detailed analysis of dark energy effects on neutron stars with realistic matter equations of state, including stability and gravitational wave implications.

Findings

Increased energy density jump enhances neutron star stability.

Results align with NICER and GW170817 observational constraints.

Dark energy core influences mass-radius and tidal deformability relations.

Abstract

By considering realistic equations of state (EoSs) to describe the ordinary matter of the stellar crust, in this study, we explore the effect of a dark energy core, made of Chaplygin Dark Fluid (CDF), on neutron stars (NSs). To accomplish this purpose, we solve the stellar structure equations and investigate the impact of the CDF parameters on the several macroscopic properties of NSs such as mass-radius ($M-R$) relation, and tidal deformabilities of a single star and of a binary system, the latter being of great importance when analyzing gravitational-wave signals coming from the merger of such compact objects. We also present an analysis of the radial oscillation modes for the rapid phase transition, with the aim of distinguishing regions consisting of dynamically stable stars from those of unstable ones. Specifically, our outcomes reveal that an increase in the energy density jump (controlled by a parameter $\alpha$) leads to an increase in the radial stability of the NS with a CDF core. Furthermore, our theoretical results are consistent with the observational $M-R$ measurements of millisecond pulsars from NICER data and tidal deformability constraints from the GW170817 event.