Advances in High Energy Physics

Volume 2018, Article ID 7517634, 10 pages

https://doi.org/10.1155/2018/7517634

## Lorentz Distributed Noncommutative Wormhole Solutions

Department of Mathematics, University of the Punjab, Quaid-e-Azam Campus, Lahore 54590, Pakistan

Correspondence should be addressed to M. Sharif; kp.ude.up@htam.firahsm

Received 27 October 2017; Revised 21 December 2017; Accepted 25 December 2017; Published 7 February 2018

Academic Editor: Elias C. Vagenas

Copyright © 2018 M. Sharif and Kanwal Nazir. 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}.

#### Abstract

The aim of this paper is to study static spherically symmetric noncommutative wormhole solutions along with Lorentzian distribution. Here, and are torsion scalar and teleparallel equivalent Gauss-Bonnet term, respectively. We take a particular redshift function and two models. We analyze the behavior of shape function and also examine null as well as weak energy conditions graphically. It is concluded that there exist realistic wormhole solutions for both models. We also studied the stability of these wormhole solutions through equilibrium condition and found them stable.

#### 1. Introduction

It is well-known through different cosmological observations that our universe undergoes accelerated expansion that opens up new directions. A plethora of work has been performed to explain this phenomenon. It is believed that, behind this expansion, there is a mysterious force dubbed as dark energy (DE) identified by its negative pressure. Its nature is generally described by the following two well-known approaches. The first approach leads to modifying the matter part of general relativity (GR) action that gives rise to several DE models including cosmological constant, -essence, Chaplygin gas, and quintessence [1–5].

The second way leads to gravitational modification which results in modified theories of gravity. Among these theories, the theory [6] is a viable modification which is achieved by torsional formulation. Various cosmological features of this theory have been investigated like solar system constraints, static wormhole solutions, discussion of Birkhoff’s theorem, instability ranges of collapsing stars, and many more [6–8]. Recently, a well-known modified version of theory is proposed by involving higher order torsion correction terms named as theory depending upon and [9]. This is a completely different theory which does not correspond to as well as any other modified theory. It is a novel modified gravity theory having no curvature terms. The dynamical analysis [10] and cosmological applications [11] of this theory turn out to be very captivating.

Chattopadhyay et al. [12] studied pilgrim DE model and reconstructed models by assuming flat FRW metric. Jawad et al. [13] explored reconstruction scheme in this theory by considering a particular ghost DE model. Jawad and Debnath [14] worked on reconstruction scenario by taking a new pilgrim DE model and evaluated different cosmological parameters. Zubair and Jawad discussed thermodynamics at the apparent horizon [15]. We developed reconstructed models by assuming different eras of DE and their combinations with FRW and Bianchi type I universe models, respectively [16].

The study of wormhole solutions provides fascinating aspects of cosmology especially in modified theories. Agnese and Camera [17] discussed static spherically symmetric and traversable wormhole solutions in Brans-Dicke scalar tensor theory. Anchordoqui et al. [18] showed the existence of analytical wormhole solutions and concluded that there may exist a wormhole sustained by normal matter. Lobo and Oliveira [19] considered theory to examine the traversable wormhole geometries through different equations of state. They analyzed that wormhole solution may exist in this theory and discussed the behavior of energy conditions. Böhmer et al. [20] examined static traversable wormhole geometry by considering a particular model and constructed physically viable wormhole solutions. The dynamical wormhole solutions have also been studied in this theory by assuming anisotropic fluid [21]. Recently, Sharif and Ikram [22] explored static wormhole solutions and investigated energy conditions in gravity. They found that these conditions are satisfied only for barotropic fluid in some particular regions.

General relativity does not explain microscopic physics (completely described through quantum theory). Classically, the smooth texture of space-time damages at short distances. In GR, the space-time geometry is deformed by gravity while it is quantized through quantum gravity. To overcome this problem, noncommutative geometry establishes a remarkable framework that discusses the dynamics of space-time at short distances. This framework introduces a scale of minimum length having a good agreement with Planck length. The consequences of noncommutativity can be examined in GR by taking the standard form of the Einstein tensor and altered form of matter tensor.

Noncommutative geometry is considered as the essential property of space-time geometry which plays an impressive role in several areas. Rahaman et al. [23] explored wormhole solutions along with noncommutative geometry and showed the existence of asymptotically flat solutions for four dimensions. Abreu and Sasaki [24] studied the effects of null energy condition (NEC) and weak energy condition (WEC) with noncommutative wormhole. Jamil et al. [25] discussed the same work in theory. Sharif and Rani [26] investigated wormhole solutions with the effects of electrostatic field and for galactic halo regions in gravity.

Recently, Bhar and Rahaman [27] considered Lorentzian distributed density function and examined the fact that wormhole solutions exist in different dimensional space-time with noncommutative geometry. They found that wormhole solutions can exist only in four and five dimensions but no wormhole solution exists for higher than five dimensions. Jawad and Rani [28] investigated Lorentz distributed noncommutative wormhole solutions in gravity. We have explored noncommutative geometry in gravity and found that effective energy-momentum tensor is responsible for the violation of energy conditions rather than noncommutative geometry [29]. Inspired by all these attempts, we investigate whether physically acceptable wormholes exist in gravity along with noncommutative Lorentz distributed geometry. We study wormhole geometry and corresponding energy conditions.

The paper is arranged as follows. Section 2 briefly recalls the basics of theory, the wormhole geometry, and energy conditions. In Section 3, we investigate physically acceptable wormhole solutions and energy conditions for two particular models. In Section 4, we analyze the stability of these wormhole solutions. The last section summarizes the results.

#### 2. Gravity

This section presents some basic review of gravity. The idea of such extension is to construct an action involving higher order torsion terms. In curvature theory other than simple modification as theory, one can propose the higher order curvature correction terms in order to modify the action such as GB combination or functions . In a similar way, one can start from the teleparallel theory and construct an action by proposing higher torsion correction terms.

The most dominant variable in the underlying gravity is the tetrad field . The simplest one is the trivial tetrad which can be expressed as and , where the Kronecker delta is denoted by . These tetrad fields are of less interest as they result in zero torsion. On the other hand, the nontrivial tetrad fields are more favorable for constructing teleparallel theory because they give nonzero torsion. They can be expressed as The nontrivial tetrad satisfies and . The tetrad fields can be related to metric tensor through where is the Minkowski metric. Here, Greek indices represent coordinates on manifold and Latin indices correspond to the coordinates on tangent space. The other field is described as the connection 1-forms which are the source of parallel transportation, also known as Weitzenböck connection. It has the following form:

The structure coefficients appear in commutation relation of the tetrad aswhere The torsion as well as curvature tensors has the following expressions: The contorsion tensor can be described as Both the torsion scalars are written as This comprehensive theory has been proposed by Kofinas et al. [10] whose action is described as where is the matter Lagrangian, , represents determinant of the metric coefficients, and . The field equations obtained by varying the action about are given as where Here, represents the matter energy-momentum tensor. The functions and are the derivatives of with respect to and , respectively. Notice that, for , teleparallel equivalent to GR is achieved. Also, for , we can obtain theory.

Next, we explain the wormhole geometry as well as energy conditions in this gravity.

##### 2.1. Wormhole Geometry

Wormhole associates two disconnected models of the universe or two distant regions of the same universe (interuniverse or intrauniverse wormhole). It has basically a tube, bridge, or tunnel type appearance. This tunnel provides a shortcut between two distant cosmic regions. The well-known example of such a structure is defined by Misner and Wheeler [30] in the form of solutions of the Einstein field equations named as wormhole solutions. Einstein and Rosen made another attempt and established Einstein-Rosen bridge.

The first attempt to introduce the notion of traversable wormholes is made by Morris and Thorne [31]. The Lorentzian traversable wormholes are more fascinating in a way that one may traverse from one to another end of the wormhole [32]. The traversability is possible in the presence of exotic matter as it produces repulsion which keeps open throat of the wormhole. Being the generalization of Schwarzschild wormhole, these wormholes have no event horizon and allow two-way travel. The space-time for static spherically symmetric as well as traversable wormholes is defined as [31]where is the redshift function and represents the shape function. The gravitational redshift is measured through the function whereas controls the wormhole shape. The radial coordinate , redshift, and shape functions must satisfy few conditions for the traversable wormhole. The redshift function needs to satisfy no horizon condition because it is necessary for traversability. Thus to avoid horizons, must be finite throughout. For this purpose, we assumed zero redshift function that implies . There are two properties related to the shape function to maintain the wormhole geometry. The first property is positiveness; that is, as , must be defined as a positive function. The second is flaring-out condition; that is, and at with ( is the wormhole throat radius). The condition of asymptotic flatness ( as ) should be fulfilled by the space-time at large distances.

To investigate the wormhole solutions, we assume a diagonal tetrad [31] asThis is the simplest and frequently used tetrad for the Morris and Thorne static spherically symmetric metric. This also provides nonzero which is the basic ingredient for this theory. If we take some other tetrad then it may lead to zero . Thus these orthonormal bases are most suitable for this theory. The torsion scalars turn out to beIn order to satisfy the condition of no horizon for a traversable wormhole, we have to assume . Substituting this assumption in the above torsion scalars, we obtain which means that the function reduces to representing theory. Hence, we cannot take as a constant function; instead we assume aswhich is finite and nonzero for . Also, it satisfies asymptotic flatness as well as no horizon condition. We assume that anisotropic matter threads the wormhole for which the energy-momentum tensor is defined aswhere , , , , and represent the energy density, four-velocity, radial space-like four-vector orthogonal to , and radial and tangential components of pressure, respectively. We consider energy-momentum tensor as . Using (12)–(16) in (10), we obtain the field equations as where prime stands for the derivative with respect to .

##### 2.2. Energy Conditions

These conditions are mostly considered in GR and also in modified theories of gravity. As these conditions are violated in GR and this guarantees the presence of realistic wormhole, the origin of these conditions is the Raychaudhuri equations along with the requirement of attractive gravity [33]. Consider time-like and null vector field congruence as and , respectively; the Raychaudhuri equations are formulated as follows: where the expansion scalar is used to explain expansion of the volume and shear tensor provides the information about the volume distortion. The vorticity tensor explains the rotating curves. The positive parameters and are used to interpret the congruence in manifold. In the above equations, we may neglect quadratic terms as we consider small volume distortion (without rotation). Thus these equations reduce to . The expression ensures the attractiveness of gravity which leads to and . In modified theories, the Ricci tensor is replaced by the effective energy-momentum tensor, that is, and which introduce effective pressure and effective energy density in these conditions.

It is well-known that the violation of NEC is the basic ingredient to develop a traversable wormhole (due to the existence of exotic matter). It is noted that, in GR, this type of matter leads to the nonrealistic wormhole; otherwise normal matter fulfills NEC. In modified theories, we involve effective energy density as well as pressure by including effective energy-momentum tensor in the corresponding energy conditions. This effective energy-momentum tensor is given as where are dark source terms related to the underlying theory. The condition (violation of NEC) related to confirms the presence of traversable wormhole by holding its throat open. Thus, there may be a chance for normal matter to fulfill these conditions. Hence, there can be realistic wormhole solutions in this modified scenario.

The four conditions (NEC, WEC, dominant (DEC), and strong energy condition (SEC)) are described as follows:(i)NEC: , where (ii)WEC: .(iii)DEC: .(iv)SEC: .

Solving (18) and (19) for effective energy density and pressure, we evaluate the radial effective NEC as So, represents the violation of effective NEC asIf this condition holds then it shows that the traversable wormhole exists in this gravity.

#### 3. Wormhole Solutions

Noncommutative geometry is the fundamental discretization of the space-time and it performs effectively in different areas. It plays an important role in eliminating the divergence that originates in GR. In noncommutativity, smeared substances take the place of pointlike structures. Considering the Lorentzian distribution, the energy density of particle-like static spherically symmetric object with mass has the following form [34]:where is the noncommutative parameter. Comparing (18) and (25), that is, , we obtainThe above equation contains two unknown functions and . In order to solve this equation, we have to assume one of them and evaluate the other one. Next, we consider some specific and viable models from theory and investigate the wormhole solutions under Lorentzian distributed noncommutative geometry. We also discuss the corresponding energy conditions.

##### 3.1. First Model

The first model is considered as [15]where , , , and are arbitrary constants. Here, we take and as dimensionless ones whereas and have dimensions of lengths. This model involves second-order terms and fourth-order contribution from torsion term . Using (14), (15), and (27) in (26), we achieve a complicated differential equation in terms of that cannot be handled analytically. So, we solve it numerically by choosing the corresponding parameters as , , , and . The values of the remaining parameters , , and are taken from [28]. To plot the graph of , we take the initial values as , , and . Figure 1(a) represents the increasing behavior of shape function . We discuss the wormhole throat by plotting in Figure 1(b).