Research Article  Open Access
Schwarzschildde Sitter and Antide Sitter ThinShell Wormholes and Their Stability
Abstract
This paper is devoted to construct Schwarzschildde Sitter and antide Sitter thinshell wormholes by employing Visser’s cut and paste technique. The DarmoisIsrael formalism is adopted to formulate the surface stresses of the shell. We analyze null and weak energy conditions as well as attractive and repulsive characteristics of thinshell wormholes. We also explore stable and unstable solutions against linear perturbations by taking two different Chaplygin gas models for exotic matter. It is concluded that the stressenergy tensor components violate the null and weak energy conditions indicating the existence of exotic matter at the wormhole throat. Finally, we find unstable and stable configurations for the constructed thinshell wormholes.
1. Introduction
A wormhole is a hypothetical region of spacetime which acts as a shortcut connecting different regions of the universe through a handle or tunnel. The word “wormhole,” also known as EinsteinRosen bridge, was first investigated by Einstein and Rosen [1]. The occurrence of event horizon prevents the traversable motion across distant regions of the universe through this wormhole. Morris and Thorne [2] suggested traversable wormhole solution which has no event horizon and enables the observers to traverse across both universes.
Traversable wormholes are made up of two asymptotically flat regions which are associated by a throat and satisfy the flareout condition to conserve the wormhole geometry. The violation of null (NEC) and weak energy conditions (WEC) is the fundamental property for traversable wormholes indicating the occurrence of exotic matter which must be fulfilled at the wormhole throat. The physical evidence of wormholes is a debatable issue due to exotic matter at the throat. Null energy condition is the weakest condition whose violation leads to the violation of WEC as well as strong energy condition (SEC). We characterize exotic matter by the stressenergy tensor components formulated by applying the DarmoisIsrael formalism [3, 4]. It was proposed [5] that the violation of NEC can be minimized by applying the cut and paste procedure to construct a spherically symmetric thinshell wormhole (TSW). The exotic matter was restricted at the edges and corners of the wormhole throat so that an observer could easily travel without encountering it.
It has always been fascinating to explore the stability issue of different solutions of the field equations. Different stability phases of the celestial objects give rise to various evolutionary mechanisms in the universe [6, 7]. Traversable wormholes are of remarkable significance if they are stable under linear perturbations preserving the symmetry. The stable/unstable wormhole models can be analyzed either by taking perturbations around a static solution or by using equation of state (EoS) for exotic matter at the wormhole throat. In this context, Poisson and Visser [8] investigated stable TSWs against linear perturbations formed by joining two different manifolds of the Schwarzschild geometry. Lobo and Crawford [9] extended this analysis for spherically symmetric TSWs with cosmological constant () and found that positive increases the stability regions but this region decreases for negative .
Thibeault et al. [10] studied stable 5D wormhole configurations with GaussBonnet term in EinsteinMaxwell theory. Amirabi et al. [11] analyzed the effects of GaussBonnet term on wormhole stability in higher dimensions. Sharif and Yousaf [12] found some stable wormhole solutions due to gravity. Eiroa and Simeone [13] explored only unstable cylindrical TSWs from local cosmic strings. Richarte [14] studied these solutions by invoking Chaplygin as well as antiChaplygin gases with . Recently, we have constructed charged black string wormhole configurations and examined stable TSWs [15].
In order to explore some realistic sources for exotic matter at the wormhole throat, a lot of work has been done by taking various candidates like phantom energy [16, 17], tachyon matter [18], and Chaplygin gas [19, 20]. Eiroa [21] constructed spherical TSWs in the context of generalized Chaplygin gas (GCG). Kuhfittig [22] discussed the stability of spherical TSWs in the presence of and charge by considering phantomlike EoS at the throat. Bandyopadhyay et al. [23] investigated the stability of TSWs supported by modified Chaplygin gas (MCG). Banerjee [24] explored stability formalism for dimensional spherical TSWs by taking phantom energy and Chaplygin gas as an exotic matter. Sharif and Azam have investigated both stable and unstable spherical TSWs by using modified generalized Chaplygin gas (MGCG) [25] and generalized cosmic Chaplygin gas (GCCG) [26].
This paper is devoted to analyze the stability of spherical TSWs in the presence of by taking two different EoSs for exotic matter. The paper is arranged in the following way. In Section 2, we implement Visser’s cut and paste approach to construct Schwarzschildde Sitter and antide Sitter TSWs and discuss different physical aspects of these constructed TSWs. A general linearized formalism for stability is developed in Section 3. This analysis is applied to the constructed TSWs in Section 4. The last section deals with the conclusions of our results.
2. General Formalism
In this section, we provide a basic formalism to construct spherical TSWs. The static spherically symmetric spacetime with nonvanishing is given by where ) and . For , this gives Schwarzschildde Sitter, leads to Schwarzschildantide Sitter, and yields Schwarzschild metric. Since for , so we must have , which leads to two roots, the event horizon and the cosmological horizon for the Schwarzschildde Sitter geometry as follows: where with and the domain and .
The wormhole construction is not possible for , because both horizons merge at . This implies that the wormhole throat radius must have the range and for the static solution. The event horizon for the Schwarzschildantide Sitter geometry is given by Notice that, for the existence of static wormhole configuration, we must have and .
The cut and paste procedure is a successful way for mathematical construction of TSWs. In this context, the interior region of the given spacetime is cut with , yielding two 4D copies with . A new manifold is obtained by joining them at the hypersurface: The geometric condition required for the wormhole construction is the fulfillment of flareout condition by the throat radius; that is, the embedding function in (1) satisfies the relation . The proper radial distance can be defined on the constructed wormhole as , which depicts the throat position for . If this construction fulfills the radial flareout condition, then the new manifold is called geodesically complete and describes a TSW obtained by connecting two regions with radius , which corresponds to the minimal area hypersurface. We define the coordinates at , the proper time on the shell. The induced 3D metric at is defined as We employ the standard DarmoisIsrael formalism [3] to discuss the dynamics of TSWs. The surface stresses at are evaluated by the Einstein equations at , that is, by the Lanczos equations: where and . The surface stressenergy tensor provides the surface energy density and surface tensions . The extrinsic curvatures joining the two sides of the shell are defined as The unit fourvector normals to are defined by satisfying the relation . Using (1) and (7), the components of extrinsic curvature are where dot and prime correspond to and , respectively. Using (6) and (9), the surface stresses to yield
We require the following energy conditions, that is, WEC: , , NEC: , and SEC: , . We see from (10) and (11) that and , which shows the violation of NEC and WEC for different values of and , leading to the occurrence of exotic matter at the shell . The violation of the energy conditions corresponding to both spherical TSWs is shown in Figure 1.
(a)
(b)
Now, we investigate the attractive and repulsive nature of the constructed TSWs. For this purpose, we have to calculate the observer’s fouracceleration: where is the observer’s fourvelocity. The nonzero component of fouracceleration for (1) is given by for which the geodesic equation of motion has the form It is worth mentioning here that a wormhole has attractive nature if ; that is, an observer must move with an outwarddirected radial acceleration in order to avoid being dragged by the wormhole. The wormhole is repulsive for ; that is, an observer must have the radial acceleration directed towards inside in order to keep away from being pushed by the wormhole [22, 24]. The attractive and repulsive characteristics of the spherical TSWs are shown in Figure 2.
(a)
(b)
For large values of , , and , a surface tension is needed to support or hold the wormhole from expanding, so that a traveler can easily traverse through it. For low values of , , and , the surface pressure prevents the wormhole from expanding. The corresponding results are shown in Figure 3.
(a)
(b)
3. Standard Approach for Stability Analysis
This section deals with the wormhole stability through linear perturbations. The corresponding surface stresses, that is, and , for the static wormhole solutions using (10) and (11) turn out to be The dynamics of throat is described by thinshell equation of motion which can be obtained by rearranging (10) as , where is the potential function given by We observe that and satisfy the conservation equation: where is the wormhole throat area. This equation can be written as where we have used . To investigate the wormhole stability, we expand by Taylor’s series up to second order around , yielding Differentiating (16) and using (18), we have It is remarked that stability of wormhole static solution depends upon and .
4. Schwarzschildde Sitter and Antide Sitter Wormholes
Here we construct Schwarzschildde Sitter as well as antide Sitter TSWs. From (15), the surface stresses for static configuration become The matter violating the null and weak energy conditions is known as exotic matter. In order to explore some realistic sources for exotic matter at the WH throat, a lot of work has been done by taking various candidates of dark energy like family of Chaplygin gas, phantom energy, and quintessence. To support the exotic matter at the wormhole throat, we model wormholes by taking GCCG and modified cosmic Chaplygin gas (MCCG) EoSs in the following subsections.
4.1. Generalized Cosmic Chaplygin Gas
We model the exotic matter with GCCG [27] at the shell to investigate the wormhole dynamics. The EoS for GCCG is defined as where , , and . Here is taken as a positive constant other than unity. This EoS corresponds to GCG in the limit and the usual Chaplygin gas is recovered for , . Using (15) in (22), we formulate the following equation for static configuration: By taking the first derivative of (22), we have which leads to By differentiating (20) and using (25), can be written as Inserting the values of and from (15), we see that both and become zero at , while (26) takes the form
We are interested to study the stability of Schwarzschildde Sitter and antide Sitter TSWs. In this context, the corresponding dynamical equation for static solution by substituting (21) in (22) takes the form where its solutions represent static spherical TSWs. Equation (27) yields We evaluate the numerical value of from (28) for and check the behavior of solutions by inserting in (29). We analyze the wormhole stability for static Schwarzschildde Sitter and antide Sitter solutions. The wormhole throat radius must have the range for the existence of Schwarzschildde Sitter solution. Static stable and unstable solutions exist if , and , respectively. For , there is no static solution which leads to the nonphysical region (grey zone).
The unstable and stable wormhole solutions correspond to dotted and solid curves, respectively. The results in Figures 4–6 can be summarized as follows.(i)Figure 4 for indicates unstable and stable solutions for both Schwarzschildde Sitter and antideSitter TSWs corresponding to . These solutions tend to decrease and meet the horizon radius with increasing value of . The horizon radius continues to step down by decreasing the value of .(ii)For , we have two types of solutions (stable and unstable) for , while there exist different solutions for ; two of them are stable and one is unstable with as shown in Figures 5 and 6. Here also, the horizon radius continues to decrease as in the previous cases.
4.2. Modified Cosmic Chaplygin Gas
Now we consider MCCG as exotic matter at the wormhole throat. The EoS for MCCG is given by Sadeghi and Farahani [28] used MCCG as varying MCCG by assuming as a function of scale factor . Here, we assume as a constant as in the above model. Inserting (15) in (30), we formulate the corresponding dynamical equation (for static configuration) as Differentiating (30), we have The second derivative of by using (20) and (32) becomes Inserting the values of and , we find that at , while (33) turns out to be
For the Schwarzschildde Sitter and antide Sitter wormhole static solutions, (31) takes the form By substituting and in (34), (satisfied by the throat radius) turns out to be To discuss the behavior of spherical TSWs with MCCG, we evaluate the numerical value of from (35) for and then substitute it in (36). The results in Figures 7–10 corresponding to show stable and unstable wormhole solutions for . In Figures 7 and 8, we find both stable and unstable configurations corresponding to . These solutions tend to decrease and meet the horizon radius with increasing value of . Similarly, we examine both types of solutions for (Figures 910). The throat radius appears as an increasing function of for and . Moreover, the radius of horizon for the given manifold decreases with small values of .
5. Conclusions
This paper is devoted to construct spherical TSWs with nonvanishing cosmological constant by employing Visser’s cut and paste scheme. We have found that the stressenergy tensor components violate the NEC and WEC showing the existence of exotic matter at the throat. We have also examined the attractive and repulsive characteristics of TSWs. A wormhole has attractive nature if which exhibits that an observer should move with an outgoing radial acceleration to avoid being dragged by the wormhole, while it is repulsive for ; that is, an observer must have the radial acceleration directed towards the inside to keep away from being pushed by the wormhole.
The standard stability approach has been applied by considering two different models of Chaplygin gas as dark energy candidates at the wormhole throat. We have formulated the solutions numerically by solving the dynamical equations for . The results corresponding to GCCG and MCCG for the stability of Schwarzschildde Sitter and antide Sitter configurations are summarized as follows.(i)Firstly, we have investigated solutions for GCCG corresponding to . We have found one stable and one unstable static wormhole solution for the given values of and . For , there exist three types of static solutions (one unstable and two stable) with . For , the wormhole throat is a decreasing function of and touches the horizon radius which decreases gradually.(ii)Secondly, for MCCG, we have both stable and unstable solutions corresponding to both spherical TSW geometries for all values of . Table 1 shows the comparison of solutions for GCCG and MCCG with GCG and MGCG for different values of . This indicates that the stability of static solutions depends upon the choice of EoS. Here “1S” and “1US” stand for one stable and one unstable solution, respectively. There exist unstable spherical TSW solutions for corresponding to GCG [21]. We find that some stable solutions also exist for GCCG and MCCG with as compared to GCG. It is worthwhile to mention here that our results for both EoS reduce to [21, 25] in the limit .

Conflict of Interests
The authors declare that there is no conflict of interests regarding the publication of this paper.
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Copyright
Copyright © 2014 M. Sharif and Saadia Mumtaz. This is an open access article distributed under the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. The publication of this article was funded by SCOAP^{3}.