Compact Object with a Local Dark Energy Shell

TL;DR

This paper explores models of compact objects with a cosmological constant, revealing conditions under which dark energy can exist inside neutron star-like objects and analyzing the impact of the cosmological constant on their physical properties.

Contribution

It introduces new models of compact objects with dark energy shells, demonstrating the influence of the cosmological constant on their internal structure and energy conditions.

Findings

Dark energy can exist in the outer layers of certain compact objects.

Models are compatible with various cosmological constant values, including negative, zero, and positive.

Solutions with zero radial pressure are limited to negative cosmological constant.

Abstract

We investigate some models of compact objects in the general relativity theory with cosmological constant $\Lambda$, based on two density profiles, one of them attributed to Stewart and the other one to Durgapal and Bannerji, proposed in the literature to model "neutron stars". For them, a nonlocal equation of state with cosmological constant is obtained as a consequence of the chosen metric. In another direction, we obtain a solution for configurations with null radial pressure. The first model (based on the Stewart's density profile) turned out to be the most interesting, since surprisingly it admits the presence of dark energy in the interior of the star, in the outermost layers, for a certain range of mass-radius ratio $\gamma$. This dark energy is independent of the cosmological constant, since it is a consequence of the tangential pressure of the fluid be sufficiently negative. Still in this case, for other values of $\gamma$, all the energy conditions are satisfied. Another advantage of this model, as well as that based on the density profile of Durgapal and Bannnerji is the existence of intervals of $\gamma$ compatible with physically acceptable models for $\Lambda < 0$, $\Lambda = 0$ and $\Lambda > 0$, which also allowed us to analyze the influence of $\Lambda$ on the behavior of the fluid with respect to the energy conditions. The other configuration studied here, $P_r=0$, only allow solutions for $\Lambda<0$, in order to ensure a positive mass for the object and to satisfy all the energy conditions in a specific range of $\gamma$.