Thin-shell Wormholes Research Articles

Dynamical and thermodynamical stability of a charged thin-shell wormhole

AbstractA study of the dynamical and thermodynamical stability of a charged thin-shell wormhole built by gluing two Reissner–Nordström geometries is presented. The charge on the shell is linearly related to the matter content. For the dynamical stability, a concise inequality is obtained, valid for any barotropic equation of state that relates the pressure with the energy density at the throat. A thermodynamical description of the system is introduced, which leads to the temperature and the electric potentials. Adopting a linear equation of state for the pressure and a definite form for the entropy function, the set of equilibrium configurations that are both dynamically and thermodynamically stable is found.

Thin-shell wormholes with non-collapsing dark energy throats connecting flat Minkowski spacetimes

This research revisits the thin-shell wormhole connecting two Minkowski spacetimes — originally introduced by Matt Visser. Upon setting a particular timelike hypersurface with a de-sitter-induced line element, the corresponding thin-shell wormhole (TSW) possesses a minimum radius and a uniform surface energy–momentum tensor in the form of dark energy. The bounded from below radius for the throat implies that it does not collapse. The r−τ profile curve of the hypersurface is a Catenary in r−τ plane where r and τ are the radial coordinate and the proper time on the throat, respectively. It is also shown that while the throat is dynamic, the surface energy–momentum tensor of the dark energy is in the form of an effective cosmological constant in the spherically symmetric TSW. The 4-dimensional cylindrically symmetric TSW with a similar throat profile shares the same features as its spherical counterpart, however, its uniform surface energy–momentum tensor does not mimic an effective cosmological constant. The higher-dimensional generalization of the spherically symmetric TSW admits the same properties as in the 4-dimensional one.

Effect of perfect fluid dark matter on Bardeen thin-shell wormholes

Effect of perfect fluid dark matter on Bardeen thin-shell wormholes

Additional observational features of the thin-shell wormhole by considering quantum corrections* *Supported by the National Natural Science Foundation of China (11903025), the Science and Technology Program of Sichuan Province, China (2023ZYD0023), the Youth Science and Technology Innovation Research Team of Sichuan Province, China (21CXTD0038), the Natural Science Foundation of Sichuan Province, China (2022NSFSC1833), and by the Central Guidance on the

By considering an asymmetric thin-shell wormhole (ATSW) surrounded by an optically and geometrically thin disk, we investigate the luminosity distribution of this ATSW with the spacetime on two sides encoded with the renormalization group improved (RGI) parameters (Ω, γ). Although some light rays are absorbed into the throat in the vicinity of the wormhole, they return through the throat with certain conditions, unlike in the case of black holes. The spacetime on one side of the wormhole can capture the additional photons emitted from the thin disk, resulting in several interesting observable features of the wormhole. The results in this paper show that there are two additional orbit numbers n in the ATSW and six transfer functions, rather than three as in the black hole case. In this case, the ATSW indeed has a more complex observable structure, where some additional light rings arise naturally. For instance, there are two additional photon rings for the emitted Model 1. Moreover, we also find a new wide hump between the first and second additional photon rings in Model 2. The effects of Ω and γ on the observed images are clearly addressed throughout this study, and the influence of Ω is found to be larger. Finally, we conclude that the observations of the RGI-ATSW can help further distinguish it from other ATSWs and black holes when a thin accretion disk exists around it.

Impact of cold dark matter and variable equations of state on the stability of thin-shell wormholes

The goal of this research is to better understand how two identical black hole copies, bounded by a cold dark matter halo, produce and stabilize thin-shell wormholes. The occurrence of a cold dark matter halo is discovered to increase the black hole’s horizon radius. Investigating the stable geometry of these wormholes by linearized radial perturbation analysis is the main objective of the work. It is noteworthy that the development of thin-shell wormholes with reduced energy limitations is associated with the presence of a cold dark matter halo. We study how the stability of the wormholes is affected by variable equations of state, including phantom-like, variable Chaplygin, and barotropic equations of state. The question emphasizes how crucial the existence of a cold dark matter halo is to preserving stable thin-shell wormhole configurations. The findings shed light on the interactions between a cold dark matter halo and wormholes, which improved our knowledge of both phenomena and their possible consequences for extraterrestrial travel.

Stability of lower dimensional counter-rotating thin-shell wormholes with scalar hair

The motivation for constructing a thin-shell wormhole from a (2+1)-dimensional rotating black hole arises from the desire to study the effects of a nonminimally coupled scalar field in this particular spacetime. By investigating the behavior of such a field in the presence of rotation, we can gain insights into the interplay between gravity and scalar fields in lower-dimensional systems. Additionally, this construction allows us to explore potential connections between black hole physics and exotic phenomena like traversable wormholes. The radial perturbation around the equilibrium throat radius is considered to explore the stable configuration for specific values of physical parameters. Then, the equations of state, specifically the phantom-like and generalized Chaplygin gas model for exotic matter is used to conduct an extensive investigation into the stability of the counter-rotating thin-shell wormholes. Our results show that the presence of a scalar field enhances the stability of the counter-rotating thin-shell wormholes.

Effects of torsion charge on optical appearance and additional photon rings of an asymmetric thin-shell wormhole

In this paper, we study the optical properties of asymmetric thin-shell wormholes (ATWs) under torsion charge. Utilizing the cut-and-paste method developed by Visser, we construct these wormholes and determine their key physical properties, such as the radius of the photon sphere and critical impact parameters, under different torsion charges. Furthermore, we investigate the effective potential and behavior of photon motion within the wormhole spacetime, identifying a relationship between photon trajectories and impact parameters. The study focuses on scenarios where thin accretion disks act as the primary light source. It reveals that the optical features of ATWs under torsion charge significantly differ from those of black holes (BHs). Notably, an increase in torsion charge leads to a reduction in the sizes of both extra photon rings and lensing bands, which serve as important markers for distinguishing and characterizing ATW spacetimes from those of BHs.

Stability of asymmetric Schwarzschild–Rindler–de Sitter thin shell wormhole

The paper examines the dynamics of asymmetric thin shell wormholes that connect two distinct spacetimes using the cut and paste technique. The focus is on analyzing the linear stability of these wormholes by considering radial perturbations and utilizing the modified generalized Chaplygin gas equation of state. The specific case of an asymmetric wormhole connecting Schwarzschild–Rindler spacetime to Schwarzschild–Rindler–de Sitter space–time is analyzed using this formalism. Our investigation uncovers the existence of both stable and unstable regions, which are contingent upon the appropriate selection of various parameters within the metric spacetime and equation of state. Additionally, we determine that stability regions exist as a consequence of the square speed of sound. By increasing the value of the cosmological constant, the stability region is expanded. Furthermore, the stability regions are augmented by the influence of Rindler parameters, while the stability regions are also affected by adjustments in the equation of state parameters, leading to their enlargement.

Stability of GMGHS charged thin shell wormhole in string theory

Stability of GMGHS charged thin shell wormhole in string theory

Quantum Oppenheimer–Snyder–Swiss Cheese model

The quantum Oppenheimer–Snyder (qOS) model in loop quantum cosmology is combined with the quantum Swiss Cheese (qSC) model. While in the qOS model, the interior Ashtekar–Pawlowski–Singh (APS) semiclassical metric is joined to an exterior static spherically symmetric metric, in the qSC model an exterior APS metric is joined to an interior spherically symmetric metric. The qOS model represents a deformed Schwarzschild black hole containing a collapsing APS ball. On the other hand, the qSC describes a deformed Schwarzschild black hole surrounded by a quantum-modified Friedmann–Robertson–Walker universe i.e., APS metric. In this Letter, we apply the concept of the Thin-Shell Wormhole (TSW) to combine the two individual models in a single model that is called the quantum Oppenheimer–Snyder–Swiss Cheese (qOSSC) model. Unlike qOS and qSC, in which the interior and exterior metrics are glued smoothly without an energy–momentum tensor on the interface hypersurface, in the qOSSC model there exists an exotic surface fluid on the throat which satisfies a dark energy equation of state. The dynamic of the throat is investigated, and the universe may bounce from the minimum radius without forming a black hole.

Study of acoustic thin-shell wormholes with different types of matter distributions

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 [Formula: see text] gets closer to zero, it does not show any stable or unstable configurations at the event horizon position. For higher values of [Formula: see text] and [Formula: see text], 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 [Formula: see text] is increased. Additionally, the constructed structure exhibits stable behavior for [Formula: see text] 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 [Formula: see text] at higher values of [Formula: see text]. The stability of acoustic thin-shell WHs is higher than that of Schwarzschild thin-shell WHs for smaller values of [Formula: see text], indicating that the acoustic black hole parameter greatly influences the stable configurations of thin-shell WHs.

Observational appearance and additional photon rings of the asymmetric thin-shell wormhole in Horndeski theory

Observational appearance and additional photon rings of the asymmetric thin-shell wormhole in Horndeski theory

Generic spherically symmetric thin-shell wormholes with equilibrium throat at the innermost photonsphere are unstable

In this research, we prove analytically that a generic spherically symmetric thin-shell wormhole (TSW) with its throat located at the innermost photonsphere of the bulk asymptotically flat black hole and supported by a generic surface barotropic perfect fluid is unstable against a radial linear perturbation. This is the generalization of the instability of the Schwarzschild TSW (STSW) with the throat’s radius located at a0=3M\\documentclass[12pt]{minimal} \\usepackage{amsmath} \\usepackage{wasysym} \\usepackage{amsfonts} \\usepackage{amssymb} \\usepackage{amsbsy} \\usepackage{mathrsfs} \\usepackage{upgreek} \\setlength{\\oddsidemargin}{-69pt} \\begin{document}$$a_{0}=3M$$\\end{document} that was revealed by Poisson and Visser in their seminal work (Poisson and Visser in Phys Rev D 52, 7318, 1995). where they studied the mechanical stability of STSW. Our proof provides a link between the instability of the null circular geodesics on the innermost photonsphere of a generic static spherically symmetric asymptotically black hole and the TSW constructed in the same bulk with a0=rc\\documentclass[12pt]{minimal} \\usepackage{amsmath} \\usepackage{wasysym} \\usepackage{amsfonts} \\usepackage{amssymb} \\usepackage{amsbsy} \\usepackage{mathrsfs} \\usepackage{upgreek} \\setlength{\\oddsidemargin}{-69pt} \\begin{document}$$a_{0}=r_{c}$$\\end{document} where a0\\documentclass[12pt]{minimal} \\usepackage{amsmath} \\usepackage{wasysym} \\usepackage{amsfonts} \\usepackage{amssymb} \\usepackage{amsbsy} \\usepackage{mathrsfs} \\usepackage{upgreek} \\setlength{\\oddsidemargin}{-69pt} \\begin{document}$$ a_{0} $$\\end{document} and rc\\documentclass[12pt]{minimal} \\usepackage{amsmath} \\usepackage{wasysym} \\usepackage{amsfonts} \\usepackage{amssymb} \\usepackage{amsbsy} \\usepackage{mathrsfs} \\usepackage{upgreek} \\setlength{\\oddsidemargin}{-69pt} \\begin{document}$$r_{c}$$\\end{document} are the radius of the TSW and the innermost photonsphere, respectively. For asymptotically flat spherically symmetric black holes possessing more than one photonspheres, the number of the photonspheres is odd and at least one photonsphere is stable which implies the corresponding TSW with its throat identical with the stable photonsphere is also stable.

Observational appearance and extra photon rings of an asymmetric thin-shell wormhole with a Bardeen profile* *Supported by the National Natural Science Foundation of China (11903025), the Science and Technology Program of Sichuan Province, China(2023ZYD0023), and the starting fund of China West Normal University (18Q062)

In this work, the optical appearance of an asymmetric thin-shell wormhole with a Bardeen profile is studied. To initiate the process, we need to construct an asymmetric thin-shell wormhole utilizing the cut-and-paste technique proposed by Visser and subsequently ascertain its pertinent physical quantities such as the radius of the photon sphere and critical impact parameters for different values of magnetic charge g. Then, the effective potential and motion behavior of photons are also investigated within the framework of asymmetric thin-shell wormholes with a Bardeen profile. It can be found that the effective potential, ray trajectory, and azimuthal angle of the thin-shell wormhole exhibit a strong correlation with the mass ratio of black holes. By considering the accretion disk as the sole background light source, we observe additional photon rings and lensing bands in the optical appearance of the asymmetric thin-shell wormhole with a Bardeen profile compared to those exhibited by the Bardeen black hole. One can find that there is an increase in the size of the specific additional light bands with increasing magnetic charge g, which is different from the black hole case. These exceptionally luminous rings can serve as a robust criterion for the identification and characterization of the thin-shell wormhole spacetime.

Exploring thin-shell dynamics in regular charged black hole through T-duality

We present a thin-shell in the background of a regular charged static black hole solution in the presence of T-duality effects for the Einstein–Maxwell system. The thin-shell are developed by matching the inner and outer manifolds through the well-known Visser’s cut-and-paste approach. We produce three types of thin-shells with an outer regular charged black hole from T-duality and different choices of inner manifolds named: 1. Thin-shell (inner flat spacetime), 2. Thin-shell Garvastars (inner de Sitter spacetime), and 3. Thin-shell wormholes (inner regular charged black hole from T-duality) We evaluate the surface stresses of a thin layer of matter contents at a thin-shell through Lanczos equations and also develop equations of motion of these constructed configurations. We also explore thin-shell stability through linearized radial perturbations at equilibrium shell radius with barotropic and generalized Chaplygin equations of state. We show that the stability of respective configurations enhances in the presence of exterior charged BH from T-duality. We conclude that thin-shell Garvastars are more stable than thin-shell and thin-shell wormholes.

Thin-Shell Wormholes Admitting Conformal Motions in Spacetimes of Embedding Class One

Thin-Shell Wormholes Admitting Conformal Motions in Spacetimes of Embedding Class One

Black string thin-shell wormhole models supported with generalized Chaplygin gas

Black string thin-shell wormhole models supported with generalized Chaplygin gas

Impact of quintessence and cloud of strings on self-consistent d-dimensional charged thin-shell wormholes

This article evaluates the stability constraints of higher-dimensional geometry of thin-shell wormholes developed from the two equivalent copies of inner and outer d-dimensional charged anti-de Sitter black holes bounded by a cloud of strings and quintessence. Such geometrical structures are built using a cut-and-paste method that joins two identical forms of black hole solutions at the hypersurface. We develop the equation of motion for the constructed wormholes and then use the linear radial perturbation approach to examine the stable configuration. The stability constraints depend on the dimensions of the black holes, cloud, and quintessence parameters. It is worth mentioning that the possibility of a stable structure is greatest for the choice of d-dimensional charged anti-de Sitter black holes with quintessence and a cloud of strings.

Thin-shell wormholes and modified Chaplygin gas with relativistic corrections

In this paper, we analyze thin-shell wormholes from two identical copies of charged static cylindrically symmetric spacetimes using Visser’s ‘cut and paste’ approach under the influence of f(R, T) gravity Harko, Lobo, Nojiri, and Odintsov (2011, Phys. Rev. D 84, 024020). In this scenario, the modified Chaplygin gas supports the exotic matter in the shell which allows, one to examine the dynamics of constructed wormholes. We utilize the junction condition to connect the interior and exterior geometries across the hypersurface and calculate different components of the Lanczos equation recently computed by Roza in Rosa (2021, Phy. Rev. D 103, 104069). We analyze the stability of the thin-shell wormhole models under linear perturbations while keeping the cylindrical symmetry and also examine the influence of charge on their stability. The positive quantity of the second derivative of potential at the throat radius might be interpreted as the stability criterion. We find both unstable and stable wormhole solutions for different parameters included in the equation of state and specific forms of considered gravity and illustrate them theoretically as well as graphically. We examine the impact of electric charge on the stability region of a constructed wormhole, which suggests that a wormhole model with a charge may exhibit more stable behavior compared to an uncharged system.

Thin-shell wormholes with AdS black holes surrounded by Chaplygin dark fluid

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 [Formula: see text], where [Formula: see text] and [Formula: see text] denote the pressure and energy density that are related through positive constant [Formula: see text]. 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 [Formula: see text], 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.