Narrow Results

In this paper, we model a canonical acoustic thin-shell wormhole (CATSW) in the framework of analogue gravity systems. In this model, we apply cut and paste technique to join together two spherically symmetric, analogue canonical acoustic solutions, and compute the analogue surface density/surface pressure of the fluid using the Darmois–Israel formalism. We study the stability analyses by using a linear barotropic fluid (LBF), Chaplygin fluid (CF), logarithmic fluid (LogF), polytropic fluid (PF) and finally Van der Waals Quintessence (VDWQ). We show that a kind of analog acoustic fluid with negative energy is required at the throat to keep the wormhole stable. It is argued that CATSW can be a stabile thin-shell wormhole if we choose a suitable parameter values.

We present an infinite class of one-parameter scalar field extensions to the Bañados, Teitelboim and Zanelli (BTZ) black hole in 2 + 1 dimensions. By virtue of the scalar charge, the thin-shell wormhole supported by a linear fluid at the throat becomes stable against linear perturbations. More interestingly, we provide an example of thin-shell wormhole which is strictly stable in the sense that it is confined in between two classically intransmissible potential barriers.

In this paper, we constructed an acoustic thin-shell wormhole (ATW) under neo-Newtonian theory using the Darmois–Israel junction conditions. To determine the stability of the ATW by applying the cut-and-paste method, we found the surface density and surface pressure of the ATW under neo-Newtonian hydrodynamics just after obtaining an analog acoustic neo-Newtonian solution. We focused on the effects of the neo-Newtonian parameters by performing stability analyses using different types of fluids, such as a linear barotropic fluid (LBF), a Chaplygin fluid (CF), a logarithmic fluid (LogF) and a polytropic fluid (PF). We showed that a fluid with negative energy is required at the throat to keep the wormhole stable. The ATW can be stable if suitable values of the neo-Newtonian parameters $\varsigma$, A and B are chosen.

At the Planck scale of length $\sim 10^{-35}$ m where the energy is comparable with the Planck energy, the quantum gravity corrections to the classical background spacetime results in gravity’s rainbow or rainbow gravity. In this modified theory of gravity, geometry depends on the energy of the test particle used to probe the spacetime, such that in the low energy limit, it yields the standard general relativity. In this work, we study the thin-shell wormholes in the spherically symmetric rainbow gravity. We find the corresponding properties in terms of the rainbow functions which are essential in the rainbow gravity and the stability of such thin-shell wormholes are investigated. Particularly, it will be shown that there are exact solutions in which high energy particles crossing the throat will encounter less amount of total exotic matter. This may be used as an advantage over general relativity to reduce the amount of exotic matter.

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 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 $𝜃$.

We construct a thin-shell wormhole using the cut and paste technique from regular charged black holes with a nonlinear electrodynamics source (proposed by Balart and Vagenas). Using Darmois–Israel formalism we determine the surface stresses, which are localized at the wormhole throat. We also determine the amount of exotic matter present in the shell. To analyze the stability of the constructed wormhole we consider an equation of state as a linear perturbation. The stability region is shown in the graph by varying the values of the parameter.

A thin shell wormhole is constructed utilizing the cut and paste technique from ABGB–de Sitter black hole derived by Matyjasek et al. The surface stress localized at the wormhole throat is determined using Darmois–Israel formalism. We examine the attractive and repulsive nature of the thin shell wormhole on which cosmological constant $(\mathrm{\Lambda })$ has a significant effect. For the fixed values of charge $(q)$ and mass $(M)$, the attractiveness of the wormhole decreases with increasing $\mathrm{\Lambda }$. We calculate the total amount of exotic matter in the shell, which is not much affected by $\mathrm{\Lambda }$. For the construction of the wormhole in de Sitter universe, the regular black holes have to be heavily charged with a light mass to minimize the amount of required exotic matter. The stability of the wormhole solution is explored by considering a general equation of state in the form of linear perturbation. The stability regions are shown in the figures.

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.

In this paper, we construct thin-shell wormholes in (2 + 1)-dimensions from noncommutative BTZ black hole by applying the cut-and-paste procedure implemented by Visser. We calculate the surface stresses localized at the wormhole throat by using the Darmois–Israel formalism and we find that the wormholes are supported by matter violating the energy conditions. In order to explore the dynamical analysis of the wormhole throat, we consider that the matter at the shell is supported by dark energy equation of state (EoS) p = ωρ with ω < 0. The stability analysis is carried out of these wormholes to linearized spherically symmetric perturbations around static solutions. Preserving the symmetry we also consider the linearized radial perturbation around static solution to investigate the stability of wormholes which was explored by the parameter β (speed of sound).

We show that the cold near horizon of the extremal Reissner–Nordström can be considered as the throat of a thin-shell wormhole with arbitrarily small exotic matter and positive angular pressure. Such a wormhole is physical and stable against radial perturbations provided an appropriate perfect fluid exists at the throat.

The thermodynamic stability of a thin-shell wormhole in a Schwarzschild bulk is considered. From the first law, entropy function is found which satisfies the local intrinsic stability conditions. Heat capacity emerges as a well-defined regular function justifying the stability of a Schwarzschild thin-shell wormhole. Our method applies only to static thin-shell wormholes and in this sense it may be considered as supplementary to the classical method of stability. The scope of applications of the method is not limited by the Schwarzschild wormhole.

We have investigated the linearized stability analysis of thin-shell wormhole for scalar hairy black hole solution in Horndeski theory by surgically grafting together two identical copies of this hairy black hole spacetime. The surface stresses at the throat of the wormhole are calculated, and the attractive and repulsive characteristics of this wormhole throat are examined via radial acceleration. We also worked out the total amount of exotic matter in the shell of the wormhole.

In this paper, the charged thin-shell wormholes have been constructed by using cut-and-paste approach in the framework of $f(R)$ theory of gravity. The stability analysis is performed in $f(R)=R+\alpha R^n$ gravity formalism, where $\alpha$ and $n$ are nonzero constants, with a linear equation of state. The stable and unstable regions have been examined for different values of the parameters involved in the model. The effect of charge and mass on the throat radius is analyzed and stability of thin shell is obtained.

In this paper, the construction of thin-shell wormholes is crafted from two Bardeen anti-de Sitter black holes by using the cut and paste approach in the f(R) theory of gravity. The $f(R)=R+\alpha R^n+\beta R^{-m}$ gravity model is considered to obtain the wormhole solutions. The stability is checked for linear perturbation around some static solution. The concavity nature of the potential function is examined by variation of charge, cosmological constant and other parameters involved in the model.