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.
Highlights
Gravastars are of purely theoretical interest and can be described in three different regions with the specific equation of state (EoS)
This paper presents the formalism of charged Kiselev thinshell gravastars to explore stable configuration with different EoS
These values of physical parameters have frequently been used in literature that examine the stable as well as dynamical behavior of thin-shell constructed from different singular and non-singular black holes (BHs) [24,25,26,27,28,29,30,31,32,33,34,35,36,37,38,39,40]
Summary
Gravastars are of purely theoretical interest and can be described in three different regions with the specific equation of state (EoS). The exterior region has zero pressure ( p = 0 = σ ) and can be supported by the vacuum solution of the field equations It contains a stable thermodynamic solution and maximum entropy for small fluctuations. For the description of Mazur–Mottola scenario, Visser and Wiltshire [4] introduced the simplest model from the matching of exterior and interior geometries through the cut and paste approach. They analyzed stable configuration of the developed structure for suitable choice of EoS for the transition layers. Carter [5] extended this concept by the joining of interior DS spacetime and exterior Reissner–Nordström (RN) BH They examined the effects of EoS on the modeling of thin-shell gravastars. Rahaman et al [7,8] studied physical features like proper length, entropy
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