Stability of charged thin-shell gravastars with quintessence

Abstract

This paper develops a new solution of gravitational vacuum star in the background of charged Kiselev black holes as an exterior manifold. We explore physical features and stability of thin-shell gravastars with radial perturbation. The matter thin layer located at thin-shell greatly affects stable configuration of the developed structure. We assume three different choices of matter distribution such as barotropic, generalized Chaplygin gas and generalized phantomlike equation of state. The last two models depend on the shell radius, also known as variable equation of state. For barotropic model, the structure of thin-shell gravastar is mostly unstable while it shows stable configuration for such type of matter distribution with extraordinary quintessence parameter. The resulting gravastar structure indicates stable behavior for generalized Chaplygin gas but unstable for generalized phantomlike model. It is also found that proper length, entropy and energy within the shell show linear relation with thickness of the shell.

Twin Peak Quasi‐Periodic Oscillations and Stability via Thin‐Shell Formalism of Traversable Wormholes in Symmetric Teleparallel Gravity

“…There are many researchers that extended the range of $$B_0(D)$$ to discuss the stability of developed structure. [ 104, 105, 106 ]…”

“…The proper length can be evaluated as [105, 106] $$\begin{equation} l=\int _{D}^{D+\epsilon } \frac{dD}{\sqrt {\frac{2 n^2 (D-a_0-a_1-a_2)+(\ln (D)-\ln (r_0)) (-a_0 \ln (D)+2 n (a_0+a_1)+a_0 \ln (r_0))}{2 D n^2}}}. \end{equation}$$where ε represents the thickness of the shell and $$\epsilon \ll 1$$.…”

“…Entropy of the shell can be obtained as [105, 106] $$\begin{equation} S=4\pi \int _{D}^{D+\epsilon }r^2 h(r) \sqrt {e^{\eta (r)}}dr, \end{equation}$$the entropy density is denoted by $$h(r)$$ at local temperature and calculated as $$\begin{equation} h(r)=\frac{\varpi K_B}{\hbar }\sqrt {\frac{\mathbb {P}(r)}{2\pi }}, \end{equation}$$where ϖ and Planck units $$(K_B = 1 = \hbar )$$ are dimensionless parameters. So, entropy of the shell yields [ 105,106 ] $$\begin{equation} S=\epsilon \varpi D^2\sqrt {8\pi e^{\eta (D)} \mathbb {P}(D)}. \end{equation}$$ Figure represents the linear relationship among entropy and thickness of the shell.…”

“…There are many researchers that extended the range of B 0 (D) to discuss the stability of developed structure. [104,105,106] We consider both choices of shape function to discuss the stability of thin-shell for different values of coupling constant 𝛼, Schwarzschild BH mass and 𝜇 with a 0 = 0.2, a 1 = 0.3, a 2 = 0.4, c 2 = 0.1, c 3 = 0.1, c 6 = 0.1, c 7 = 0.1. Figures 12-14 indicate the stability of thin-shell with shaded region and vertical lines show the presence of event horizon due to the exterior BH geometry for 𝛽 1 (D).…”

Stability of $d$-dimensional Gravastars with Variable Equation of State

“…They concluded that the developed structure shows stable behavior near the formation of the event horizon for suitable values of the physical parameters. Recently, we have constructed thin-shell gravastar from exterior regular as well as charged Kiselve BHs and explored the stability of the developed geometry through radial perturbation by considering variable EoS [18].…”