Narrow Results

In this paper, we construct (2 + 1)-dimensional thin-shell wormholes from rotating Bañados–Teitelboim–Zanelli black hole and discuss their stability with the influence of scalar field at thin-shell. We apply Israel thin-shell formalism to evaluate surface stresses and study the behavior of energy conditions. We also study attractive and repulsive characteristics of the respective wormhole configurations according to the direction of radial acceleration. The linearized stability of rotating thin-shell wormholes is analyzed by assuming three different scalar field models at thin-shell. It is found that the increasing rate of angular momentum appears as an effective ingredient for stable wormholes while electric charge does not provide significant results in this regard. We conclude that less massive scalar field yields more stable 3D wormhole solutions.

This paper explores the stable configuration of thin-shell wormholes constructed from two regular black holes (modified Hayward and four parametric) by using Visser cut and paste approach. The components of stress-energy tensor are evaluated through the Lanczos equations. We analyze the stability of thin-shell by using radial perturbation preserving its symmetries about equilibrium static solution. It is found that modified Hayward wormholes are more stable than the Hayward wormholes. Further, the stable regions of four parametric regular wormholes are larger than the Schwarzschild, Reissner–Nordström and Ayón–Beato–García wormholes. We conclude that stable region decreases for highly charged thin-shell wormholes.

This paper is devoted to studying the structure of gravitationally vacuum condensate stars under the influence of matter and geometry coupled gravity. This alternative to black hole comprises three domains, i.e. interior, exterior and thin-shell. We investigate such regions by considering particular equations of state for a specific model of energy–momentum squared gravity. The nonsingular solutions of field equations are obtained to describe the interior region of gravastar and the Schwarzschild spacetime represents the exterior region. The junction conditions are used to match interior and exterior domains while Lanczos equations provide the surface density and pressure at thin-shell. We investigate various attributes of gravastar such as the equation of state parameter, entropy, proper length as well as energy. The physical features of a gravitationally vacuum star indicate a linear relationship with the thickness of the shell and provide a viable structure similar to general relativity.

This paper examines the structure of a gravitational vacuum star (also known as gravastar) in the background of $f(\Re ,{{𝒯}}^2)$ theory. This hypothetical object can be treated as a substitute of a black hole, with three regions: (i) the internal region, (ii) the intrinsic shell and (iii) the outer region. We examine these geometries using Finch–Skea metric for the radial metric component along with the particular $f(\Re ,{{𝒯}}^2)$ model. We determine singularity-free solutions for both the inner as well as thin-shell domains. The smooth matching of the interior region with external Schwarzschild spacetime is obtained through Israel matching constraints. Finally, we study various characteristics of gravastar domains including the equation-of-state parameter, proper length, entropy, energy as well as surface redshift. It is found that the compact gravastar structure is a viable alternate to the black hole in the perspective of this gravity.

This work is devoted to exploring the stability of thin-shell wormholes developed from two equivalent copies of charged quintessence (charged Kiselev) black holes by using Visser cut and paste approach. The characteristics of the surface matter of the shell are determined by using Israel formalism. We examine the stability of thin-shell by assuming a barotropic equation of state for the surface matter of the wormhole throat. We conclude that wormhole becomes stable in the presence of both charge and Kiselev parameter otherwise, it shows an unstable behavior.

This paper is devoted to the study of the stability of thin-shell wormholes from Kerr black hole. We employ Israel thin-shell formalism to evaluate surface stresses and study the behavior of energy conditions. The linearized stability of rotating thin-shell wormholes is analyzed by taking two different candidates of dark energy as exotic matter at thin-shell. It is found that generalized phantom model ($p=\frac{A}{k^n}\sigma$ which reduces to phantom equation of state as $n\to 0$ and $A<-1$, where $k(\tau )$ is wormhole throat radius and $\tau$ is the proper time) yields more stable wormhole solutions as compared to the barotropic equation of state ($p=\omega \sigma$, $\omega$ is the equation of state parameter and $\sigma$ is the surface density) for particular ranges of equilibrium throat radius and the whole range of $𝜃$.

This work studies the theoretical construction of charged quintessence thin-shell wormholes using Israel thin-shell approach. The stability of these wormhole solutions is investigated by taking linear, logarithmic and Chaplygin gas models as a constituent of exotic matter at thin-shell. The presence of wormhole stability regions particularly relies on the physically justifiable values of charge and quintessence parameter. It is noted that the increasing value of charge seems as an effective component for stable regions while the rise in negativity of the quintessence parameter gives more stable wormhole configurations.

We address the problem of stitching together the vacuum, static, planar-symmetric Taub spacetime and the flat Friedmann–Robertson–Walker (FRW) cosmology using the Israel thin shell formalism. The joining of Taub and FRW spacetimes is reminiscent of the Oppenheimer–Snyder collapse used in modeling the formation of a singularity from a collapsing spherical ball of dust. A possible mechanism for the formation of a planar singularity is provided. It is hoped that tackling such example will improve our intuition on planar-symmetric systems in Einstein’s general relativity (GR).

This paper examines the structure of gravastar (gravitationally vacuum star) in the background of $f(\Re ,{{𝒯}}^2)$ theory. The gravastar can be regarded as a substitute for a black hole comprising of three regions (i) the interior domain, (ii) the intrinsic shell and (iii) the exterior domain. We investigate these domains by employing Karmarkar’s condition by assuming a specific $f(\Re ,{{𝒯}}^2)$ model. The field equations are solved to evaluate nonsingular solutions of both the interior and intermediate regions. Inner as well as outer spacetimes are matched together using Israel formalism to obtain density and pressure at the joining surface. Different attributes of gravastar like the equation of state parameter, proper length, entropy and energy are analyzed through graphical behavior. It is found that the gravastar model is a viable alternative to the black hole in the context of this gravity.

This paper investigates stability of thin-shell developed from the matching of interior traversable wormhole with exterior Ayon–Beato–Garcia–de Sitter regular black hole through cut and paste approach. We employ Israel formalism and Lanczos equations to obtain the components of surface stress-energy tensor at thin-shell. These surface stresses violate null and weak energy conditions that suggest the presence of exotic matter at thin-shell. The surface pressure explains collapse as well as expanding behavior of the developed geometry. We explore stability of the constructed thin-shell through both perturbations along shell radius as well as barotropic equation of state for three appropriate values of the shape function $b(x)=a{x}^{\alpha }+(1-a)$. It is concluded that stability of thin-shell depends on the shape function, charge and cosmological constant.

This paper explores the role of nonlinear electrodynamics on the stable configuration of thin-shell wormholes formulated from two equivalent geometries of Reissner–Nordström black hole with nonlinear electrodynamics. For this purpose, we use cut and paste approach to eliminate the central singularity and event horizons of the black hole geometry. Then, we explore the stability of the developed model by considering different types of matter distribution located at thin-shell, i.e. barotropic model and variable equations of state (phantomlike variable and Chaplygin variable models). We use linearized radial perturbation to explore the stable characteristics of thin-shell wormholes. It is interesting to mention that Schwarzschild and Reissner–Nordström black holes show the unstable configuration for such type of matter distribution while Reissner–Nordström black hole with nonlinear electrodynamics expresses stable regions. It is found that the presence of nonlinear electrodynamics gives the possibility of a stable structure for barotropic as well as variable models. It is concluded that stable region increases for these models by considering higher negative values of coupling constant $\alpha$ and the real constant $n$.

In this paper, we inspect the stable geometry of thin-shell wormholes in the background of static spherically-symmetric AdS black holes solution bounded by dark fluid and Chaplygin-like equation of state $p=-{ℬ}/\rho$, where $p$ and $\rho$ denote the pressure and energy density that are related through positive constant ${ℬ}$. For this purpose, we consider the two equivalent copies of black holes and connected them at the hypersurface through cut and paste approach. Then, we employ the linearized radial perturbation to discuss the stability of the developed wormhole geometry by assuming variable equations of state. We obtain the maximum stable configuration for massive black holes for both barotropic and Chaplygin variable equations of state while for higher values of $n$, stable regions decrease. It is found that for every selection of physical parameters of black hole geometry with low intensity of Chaplygin dark fluid, we get the stable configuration of thin-shell wormholes.

The development and stability of acoustic thin-shell wormholes (WHs) within the context of acoustic black holes are examined in this paper. Utilizing linearized radial perturbations, the stability of these WHs is examined. In this study, a variety of equations of state are taken into account, including barotropic, variable Chaplygin, and phantom-like equations of state. According to the findings, the acoustic black hole structure has an unstable configuration for barotropic fluid. However, as the parameter ${ℰ}$ gets closer to zero, it does not show any stable or unstable configurations at the event horizon position. For higher values of $n$ and $\xi$, the resulting structure for the phantom-like variable equation of state (EoS) displays stable behavior away from the horizon while presenting unstable configurations close to the event horizon. The possibility of a stable structure rises as $n$ is increased. Additionally, the constructed structure exhibits stable behavior for $n=1$ under extreme acoustic black holes, whereas thin-shell topologies demonstrate unstable behavior outside the event horizon for the generalized Chaplygin variable EoS. However, the structure stabilizes for $n=1$ at higher values of $\xi$. The stability of acoustic thin-shell WHs is higher than that of Schwarzschild thin-shell WHs for smaller values of $n$, indicating that the acoustic black hole parameter greatly influences the stable configurations of thin-shell WHs.

This paper focuses on the examination of stable and unstable geometrical structures of thin-shell wormholes constructed from Henneaux–Martinez–Troncoso–Zanelli black holes through the Visser cut-and-paste approach. We use the Israel thin-shell formalism for evaluating the stress–energy tensor components of the matter distribution near the wormhole throat. Equations of state, specifically the phantom-like and generalized Chaplygin gas model for exotic matter, are used to conduct an extensive investigation into the stability of the thin-shell. The radial perturbation around the equilibrium throat radius is also considered to explore the stable configuration for specific values of physical parameters. Our results show that the stable zones of these thin-shell wormholes increase as the scalar field parameter ${ℰ}$ approaches −1. This study gives light on the behavior and dynamics of these wormholes throw light on their potential stability and lead the way for additional theoretical physics research.

With a Kiselev spacetime around Schwarzschild black holes that have undergone quantum correction, the goal of this work is to examine the geometric structure of a thin-shell. In order to do so, we take into consideration black hole solutions and match the inner Minkowski spacetime using a cut and paste method. Our findings indicate that the use of a phantom-like equation of state, such as quintessence, dark energy, and phantom energy, in the linearized radial perturbation technique shows stable thin-shell configurations that lie beyond the outer manifold’s predicted position of the event horizon. Moreover, we discover that the characteristics of the black hole solutions have a significant impact on the thin-shell stability. We examine the behavior of a thin-shell configuration with massless and massive scalar fields by using Klein–Gordon’s equation of motion. According to our findings, the thin-shell system dynamics are significantly influenced by the scalar field, resulting in interesting phenomena including expansion and collapse. These results provide fresh light on the behavior of black hole solutions by providing important insights into the interaction between quantum correction factors related to scalar fields and thin-shell dynamics. In particular, our research suggests that the quantum correction parameter decreases the stable configuration of a Schwarzschild black hole encircled by a quintessence field.

This paper is devoted to discuss stability of regular Hayward thin-shell wormholes. We apply Israel formalism to calculate surface stresses of the shell which violate the null and weak energy conditions leading to the presence of exotic matter. We study the attractive and repulsive characteristics of wormholes corresponding to a^r > 0 and a^r < 0, respectively. It is found that both stable and unstable solutions exist against linear perturbations by assuming Van der Waals quintessence model for exotic matter. We conclude that the Hayward and Van der Waals quintessence parameters increase the stability of thin-shell wormholes.