Dark Energy Star in Gravity's Rainbow

TL;DR

This paper explores how gravity's rainbow modifies the structure and stability of dark energy stars, providing insights into non-singular compact objects and their behavior near phase transitions.

Contribution

It derives a modified TOV equation in gravity's rainbow and analyzes the physical and stability properties of dark energy stars within this framework.

Findings

Gravity's rainbow significantly affects the star's physical properties.

The model remains stable under certain conditions.

Energy conditions are satisfied in the modified framework.

Abstract

The concept of dark energy can be a candidate for preventing the gravitational collapse of compact objects to singularities. According to the usefulness of gravity's rainbow in UV completion of general relativity (by providing a new description of spacetime), it can be an excellent option to study the behavior of compact objects near phase transition regions. In this work, we obtain a modified Tolman-Openheimer-Volkof (TOV) equation for anisotropic dark energy as a fluid by solving the field equations in gravity's rainbow. Next, to compare the results with general relativity, we use a generalized Tolman-Matese-Whitman mass function to determine the physical quantities such as energy density, radial pressure, transverse pressure, gravity profile, and anisotropy factor of the dark energy star. We evaluate the junction condition and investigate the dynamical stability of dark energy star thin shell in gravity's rainbow. We also study the energy conditions for the interior region of this star. We show that the coefficients of gravity's rainbow can significantly affect this non-singular compact object and modify the model near the phase transition region.