Noncommutative Wormhole Solutions in Einstein Gauss-Bonnet Gravity

Abstract

We explore static spherically symmetric wormhole solutions in the framework of n-dimensional Einstein Gauss-Bonnet gravity. Our objective is to find out wormhole solutions that satisfy energy conditions. For this purpose, we consider two frameworks such as Gaussian distributed and Lorentzian distributed noncommutative geometry. Taking into account constant redshift function, we obtain solutions in the form of shape function. The fifth and sixth dimensional solutions with positive as well as negative Gauss-Bonnet coefficient are discussed. Also, we check the equilibrium condition for the wormhole solutions with the help of generalized Tolman-Oppenheimer-Volkoff equation. It is interesting to mention here that we obtain fifth dimensional stable wormhole solutions in both distributions that satisfy the energy conditions.

Academic Editor:Rong-Gen Cai

Department of Mathematics, COMSATS Institute of Information Technology, Lahore 54000, Pakistan

Received 2 November 2015; Revised 25 January 2016; Accepted 3 February 2016

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 SCOAP³ .

1. Introduction

The study of wormhole solution becomes a prime focus of interest in the modern cosmology as it connects different distant parts of the universe as a shortcut. The wormhole is like a tunnel or bridge with two ends which are open in distant parts of the universe to join. To develop the mathematical structure of wormhole in general relativity [1], the basic ingredient is an energy-momentum tensor which constitutes exotic matter. This is hypothetical form of matter results of the violation of energy conditions. For two-way travel, the traversable condition must be fulfilled; that is, the throat of wormhole must remains open due to violation of the null energy condition. Since normal matter satisfies the energy conditions, the matter violating the energy condition is called exotic. The phantom dark energy violates the energy conditions which may be a reasonable source of wormhole construction [2, 3]. The inclusion of some scalar field models, electromagnetic field, Gaussian and Lorentzian distributions of noncommutative geometry, thin-shell formalism, and so forth demonstrates more interesting and useful results [4-11].

In order to minimize the usage of exotic matter or to find another source of violation while normal matter satisfies the energy conditions, many directions are adopted so far. Modified theories of gravity are the most appealing direction which contribute to using effective energy-momentum tensor. For instance, in [figure omitted; refer to PDF] [12] as well as [figure omitted; refer to PDF] [13] theories, it has been proved that the effective energy-momentum tensor which consists of higher order curvature terms or some torsion terms is responsible for the necessary violation to traverse through the wormhole. Nowadays, higher dimensional wormhole solutions are also under discussion. Many theories point out the existence of extra dimensions in the universe which leads to explore wormhole solutions for higher dimensions.

Rahaman with his collaborators have done a lot of work taking noncommutative geometry in four-dimensional spacetime as well as higher dimensional cases. Rahaman et al. [14] studied the higher dimensional static spherically symmetric wormhole solutions in general relativity with Gaussian distribution. They found these solutions up to four dimensions while they found these solutions in a very restrictive way for fifth dimensional case. Bhar and Rahaman [15] obtained the same result by taking Lorentzian distribution. Rahaman et al. [16] worked for viable physical properties of new wormhole solutions inspired by noncommutative geometry with conformal killing vectors. In [figure omitted; refer to PDF] gravity with Gaussian [17] and Lorentzian distributions [8], wormhole solutions are constructed but with violation of energy conditions. Sharif and Rani [13] explored the noncommutative wormhole solutions in [figure omitted; refer to PDF] gravity and found some physically acceptable solutions.

In a recent paper, Jawad and Rani [18] studied Lorentz distributed wormhole solutions in [figure omitted; refer to PDF] gravity and found some stable wormhole solutions satisfying energy conditions. In the higher dimensional gravity theories, [figure omitted; refer to PDF] -dimensional Einstein Gauss-Bonnet gravity is widely used. The modern string theory established its natural appearance in the low energy effective action. Bhawal and Kar [19] studied Lorentzian wormhole solutions in [figure omitted; refer to PDF] -dimensional Einstein Gauss-Bonnet gravity which depend on the dimensionality of the spacetime and coupling coefficient of Gauss-Bonnet combination. Taking traceless fluid, Mehdizadeh et al. [20] extended this work and found wormhole solutions which satisfy energy conditions.

We explore wormhole solutions taking spacetime of [figure omitted; refer to PDF] sphere in the framework of [figure omitted; refer to PDF] -dimensional Einstein Gauss-Bonnet gravity. We consider two frameworks: noncommutative geometry having Gaussian distributed energy density and Lorentzian distributed energy density. For [figure omitted; refer to PDF] and [figure omitted; refer to PDF] -dimensions, we take positive as well as negative Gauss-Bonnet coefficient. Also, we check the stability of wormhole solutions with the help of generalized Tolman-Oppenheimer-Volkoff equation. The paper is organized as follows: in Section 2, we construct the field equation for higher dimensional wormhole solutions in [figure omitted; refer to PDF] -dimensional Gauss-Bonnet gravity. Section 3 is devoted to the construction of wormhole solutions in Gaussian and Lorentzian noncommutative frameworks. In Section 4, we check the equilibrium condition of the wormhole solutions. Section 5 summarizes the discussions and results.

2. Field Equations

In this section, we provide some basic and brief reviews about [figure omitted; refer to PDF] -dimensional Einstein Gauss-Bonnet gravity as well as wormhole geometry and construct field equations in the underlying scenario.

2.1. [figure omitted; refer to PDF] -Dimensional Einstein Gauss-Bonnet Gravity

The action for [figure omitted; refer to PDF] -dimensional Einstein-Gauss-Bonnet gravity is an outcome of string theory in low energy limit. It is given by [figure omitted; refer to PDF] where [figure omitted; refer to PDF] is the [figure omitted; refer to PDF] -dimensional Ricci scalar, [figure omitted; refer to PDF] is the Gauss-Bonnet coefficient, and [figure omitted; refer to PDF] is the Gauss-Bonnet term defined as [figure omitted; refer to PDF] Varying the action with respect to metric tensor, the field equations becomes [figure omitted; refer to PDF] where [figure omitted; refer to PDF] and [figure omitted; refer to PDF] are the Einstein and energy-momentum tensors, respectively, while Gauss-Bonnet tensor is defined as [figure omitted; refer to PDF] It is noted that we assume [figure omitted; refer to PDF] where [figure omitted; refer to PDF] is the [figure omitted; refer to PDF] -dimensional gravitational constant.

2.2. Wormhole Geometry

The wormhole spacetime for [figure omitted; refer to PDF] sphere is given by [14, 15] [figure omitted; refer to PDF] where [figure omitted; refer to PDF] is the redshift function and [figure omitted; refer to PDF] is the shape function. For traversable wormhole scenario, we have to choose [figure omitted; refer to PDF] to be finite to satisfy the no-horizon condition. Usually, it is taken as zero for the sake of simplicity, which gives [figure omitted; refer to PDF] . The reason behind finite redshift function is as follows. The redshift function defines that part of the metric responsible for finding the magnitude of the gravitational redshift. The gravitational redshift is the reduction in the frequency that a photon will experience when it climbs out from gravitational potential well in order to escape to infinity. In doing so, the photon uses energy. Its energy is proportional to its frequency. A reduction in energy then is equivalent to a reduction in frequency, which is also known as redshift function. If the wormhole has an event horizon, it means that a photon emitted outwardly from the horizon cannot escape to infinity. In other words, it would take an infinite amount of energy for the photon to escape. Its frequency would be infinity reduced; that is, its redshift would be negatively infinite. A negatively infinite value of the redshift function at a particular value of the radial coordinate indicates the presence of an event horizon there. Thus to be traversable wormhole solution, the magnitude of its redshift function must be finite.

The shape of the wormhole is such that a spherical hole in space with increasing length of diameter as moving far from throat (the minimum nonzero value of radial coordinate denoted as [figure omitted; refer to PDF] ) and combines two asymptomatically flat regions. In order to have a proper shape of the wormhole, the shape function must attain the ratio to radial coordinate as [figure omitted; refer to PDF] and represents increasing behavior with respect to radial coordinate which is [figure omitted; refer to PDF] . This condition of ratio is known as flare-out condition. In addition, the value of shape function and radial coordinate must be same at throat; that is, [figure omitted; refer to PDF] . There are also some other constraints applied on the derivative of shape functions which must be satisfied. These are [figure omitted; refer to PDF] and [figure omitted; refer to PDF] . Also, the proper distance [figure omitted; refer to PDF] must meet the criteria as decreasing behavior from upper region [figure omitted; refer to PDF] towards throat where [figure omitted; refer to PDF] and then towards lower region where [figure omitted; refer to PDF] .

In order to make the wormhole traversable, the throat must remain open. To prevent shrinking of wormhole throat, there must exist such form of energy-momentum tensor which provides the corresponding matter content. This matter content violates the energy conditions in order to keep throat open and thus is named as exotic matter. This implies that violation of these conditions is the basic key ingredient to construct traversable wormhole solutions. Since the usual energy-momentum tensor satisfies the energy conditions, therefore the search for wormhole solutions for which violation may come from other sources while matter content satisfying energy conditions becomes one of the most challenging problems in astrophysics.

The higher dimensional gravity theories and modified theories may play positive role by providing violation from higher order Lagrangian terms and effective form of energy-momentum tensor. The relationship between Raychaudhuri equation and attractiveness of gravity yields the weak energy condition (WEC) as [figure omitted; refer to PDF] , for any time-like vector [figure omitted; refer to PDF] . In terms of components of the energy-momentum tensor, this inequality yields [figure omitted; refer to PDF] and [figure omitted; refer to PDF] . The null energy condition (NEC) is developed by continuity through WEC; that is, the NEC is [figure omitted; refer to PDF] , for any null vector [figure omitted; refer to PDF] . This inequality gives [figure omitted; refer to PDF] . Also, it is noted that WEC keeps NEC.

The anisotropic energy-momentum is given by [figure omitted; refer to PDF] where [figure omitted; refer to PDF] and [figure omitted; refer to PDF] are the radial and tangential pressure components with [figure omitted; refer to PDF] , [figure omitted; refer to PDF] , and satisfy [figure omitted; refer to PDF] . Using (3), the field equations become [figure omitted; refer to PDF] where prime refers derivative with respect to [figure omitted; refer to PDF] and [figure omitted; refer to PDF] for the sake of notational simplicity.

3. Wormhole Solutions

In order to discuss the wormhole geometry and solutions, there are several frameworks and strategies used to find unknown functions. For instance, we have five unknown functions [figure omitted; refer to PDF] , [figure omitted; refer to PDF] , [figure omitted; refer to PDF] , [figure omitted; refer to PDF] , and [figure omitted; refer to PDF] in the underlying case. One may choose some kind of equation of state representing accelerated expansion of the universe, or different forms of energy density such as energy density of static spherically symmetric object with noncommutative geometry having Gaussian or Lorentzian distributions and galactic halo region and so forth. The traceless energy-momentum tensor is also used which is related to the Casimir effect. In order to construct viable wormhole solutions in [figure omitted; refer to PDF] -dimensional Einstein-Gauss-Bonnet gravity, we assume different forms of energy density of noncommutative geometry in the following.

Nicolini et al. [21] have improved the short distance behavior of point-like structures in a new conceptual approach based on coordinate coherent state formalism to noncommutative gravity. In their method, curvature singularities which appear in general relativity can be eliminated. They have demonstrated that black hole evaporation process should be stopped when a black hole reaches a minimal mass. This minimal mass, named black hole remnant, is a result of the existence of a minimal observable length. This approach, which is the so-called noncommutative geometry inspired model, via a minimal length caused by averaging noncommutative coordinate fluctuations cures the curvature singularity in black holes. In fact, the curvature singularity at the origin of black holes is substituted for a regular de Sitter core. Accordingly, the ultimate phase of the Hawking evaporation as a novel thermodynamically steady state comprising a nonsingular behavior is concluded.

It must be noted that, generally, it is not required to consider the length scale of the coordinate noncommutativity to be the same as the Planck length. Since, the noncommutativity influences appear on a length scale connected to that region, they can behave as an adjustable parameter corresponding to that pertinent scale. The presence of a universal short distance cut-off leads to the effects such as in quantum field theory; it curves UV divergences while it cures curvature singularities in general relativity. In the specific case of the gravity field equations, the only modification occurs at the level of the energy-momentum tensor, while [figure omitted; refer to PDF] is formally left unchanged. In nonommutative space, the usual definition of mass density in the form of Dirac delta function does not hold. So in this space the usual form of the energy density of the static spherically symmetry smeared and particle-like gravitational source requires some other forms of distribution.

In view of the above explanations, we are going to discuss wormhole solutions with the help of two well-known energy distributions such as Gaussian and Lorentzian in noncommutative scenario. As an important remark, the essential aspects of the noncommutativity approach are not specifically sensitive to any of these distributions of the smearing effects [22] rather only distribution parameter is different. The Gaussian source has also been used by Sushkov [23] to model phantom-energy supported wormholes, as well as by Nicolini and Spallucci [24] for the purpose of modeling the physical effects of short distance fluctuations of noncommutative coordinates in the study of black holes. Galactic rotation curves inspired by a noncommutative geometry background are discussed [25]. The stability of a particular class of thin-shell wormholes in noncommutative geometry is analyzed elsewhere [26].

3.1. Gaussian Distributed Noncommutative Framework

An intrinsic characteristic of spacetime is the noncommutativity which plays an effective role in several areas. It is an interesting consequence of string theory where the coordinates of spacetime become noncommutative operators on [figure omitted; refer to PDF] -brane [27]. The noncommutativity of spacetime can be converted in the commutator, [figure omitted; refer to PDF] , where [figure omitted; refer to PDF] is an antisymmetric matrix describing discretization of spacetime and has dimension [figure omitted; refer to PDF] . This discretization process is similar to the discretization of phase space by Planck constant. Replacing the point-like structures with smeared objects, the energy density of the particle-like static spherically symmetric gravitational source having mass [figure omitted; refer to PDF] takes the following form [21]: [figure omitted; refer to PDF] where [figure omitted; refer to PDF] is the noncommutative parameter in Gaussian distribution. The mass [figure omitted; refer to PDF] could be a diffused centralized object such as a wormhole [28]. It is mentioned here that the smearing effect is achieved by replacing the Gaussian distribution of minimal length [figure omitted; refer to PDF] with the Dirac delta function. In order to construct [figure omitted; refer to PDF] -dimensional Einstein Gauss-Bonnet wormhole geometry, we equate the energy density given in (7) and [figure omitted; refer to PDF] in (10) yields the following differential equation: [figure omitted; refer to PDF] The solution of this equation is [figure omitted; refer to PDF] where [figure omitted; refer to PDF] is an integration constant. This solution has two roots with plus and minus signs and we assign these roots as [figure omitted; refer to PDF] and [figure omitted; refer to PDF] solutions. In order to plot the quantities [figure omitted; refer to PDF] , [figure omitted; refer to PDF] , [figure omitted; refer to PDF] , and [figure omitted; refer to PDF] to obtain wormhole solutions for both of these solutions, we restrict ourselves to five- and six-dimensional cases with constant redshift function [figure omitted; refer to PDF] . The expressions of NEC takes the form [figure omitted; refer to PDF]

In this regard, we assume values of some constants as [figure omitted; refer to PDF] , [figure omitted; refer to PDF] while [figure omitted; refer to PDF] result in [figure omitted; refer to PDF] for five-dimensional and [figure omitted; refer to PDF] for six-dimensional case. Figure 1(a) represents the plot of [figure omitted; refer to PDF] versus [figure omitted; refer to PDF] for five and six-dimensional wormhole solutions. The graph represents positively increasing behavior for positive [figure omitted; refer to PDF] for both curves. For negative [figure omitted; refer to PDF] , we examine that graph initially represents positive behavior for both dimensions in the range [figure omitted; refer to PDF] and [figure omitted; refer to PDF] for [figure omitted; refer to PDF] and [figure omitted; refer to PDF] , respectively, and then decreases towards negative values. In Figure 1(b), the graph of [figure omitted; refer to PDF] versus [figure omitted; refer to PDF] shows the same behavior for all curves as in Figure 1(a), with positive behavior of dashed curves in the range [figure omitted; refer to PDF] and [figure omitted; refer to PDF] for [figure omitted; refer to PDF] ad [figure omitted; refer to PDF] . However, we have less possibility of wormhole scenario with respect to [figure omitted; refer to PDF] for positive root solution as compared to negative root solution of shape function.

Figure 1: Plots of (a) [figure omitted; refer to PDF] and (b) [figure omitted; refer to PDF] versus [figure omitted; refer to PDF] in Gaussian distribution for [figure omitted; refer to PDF] , [figure omitted; refer to PDF] (red), [figure omitted; refer to PDF] , [figure omitted; refer to PDF] (red dashed), [figure omitted; refer to PDF] , [figure omitted; refer to PDF] (purple), and [figure omitted; refer to PDF] , [figure omitted; refer to PDF] (purple dashed).

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Figure 2 shows the behavior of energy density versus [figure omitted; refer to PDF] as positively decreasing behavior for both dimensions corresponding to [figure omitted; refer to PDF] and [figure omitted; refer to PDF] dimensions. For [figure omitted; refer to PDF] and positive [figure omitted; refer to PDF] , the plot of [figure omitted; refer to PDF] represents positive behavior in decreasing manner for [figure omitted; refer to PDF] and [figure omitted; refer to PDF] while representing negative behavior for negative [figure omitted; refer to PDF] as shown in Figure 3(a). In Figure 3(b), we examine same behavior for negative root solution. Figure 4(a) depicts the opposite behavior to Figure 3(a), that is, for [figure omitted; refer to PDF] dimensions and positive [figure omitted; refer to PDF] , [figure omitted; refer to PDF] demonstrates negative behavior. Thus, these plots express the violation of WEC incorporating the case of [figure omitted; refer to PDF] . For [figure omitted; refer to PDF] , we obtain the same behavior as in Figure 3(b) which indicates positive behavior for positive [figure omitted; refer to PDF] and [figure omitted; refer to PDF] and negative behavior for negative [figure omitted; refer to PDF] and [figure omitted; refer to PDF] . This implies that WEC is satisfied for negative root solution with positive Gauss-Bonnet coefficient. Thus, we obtain physically acceptable wormhole solutions satisfying WEC for both dimensions.

Figure 2: Plots of (a) [figure omitted; refer to PDF] and (b) [figure omitted; refer to PDF] versus [figure omitted; refer to PDF] in Gaussian distribution for [figure omitted; refer to PDF] , [figure omitted; refer to PDF] (red), [figure omitted; refer to PDF] , [figure omitted; refer to PDF] (red dashed), [figure omitted; refer to PDF] , [figure omitted; refer to PDF] (purple), and [figure omitted; refer to PDF] , [figure omitted; refer to PDF] (purple dashed).

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Figure 3: Plots of (a) [figure omitted; refer to PDF] for [figure omitted; refer to PDF] and (b) [figure omitted; refer to PDF] for [figure omitted; refer to PDF] versus [figure omitted; refer to PDF] in Gaussian distribution for [figure omitted; refer to PDF] , [figure omitted; refer to PDF] (red), [figure omitted; refer to PDF] , [figure omitted; refer to PDF] (red dashed), [figure omitted; refer to PDF] , [figure omitted; refer to PDF] (purple), and [figure omitted; refer to PDF] , [figure omitted; refer to PDF] (purple dashed).

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Figure 4: Plots of (a) [figure omitted; refer to PDF] for [figure omitted; refer to PDF] and (b) [figure omitted; refer to PDF] for [figure omitted; refer to PDF] versus [figure omitted; refer to PDF] for in Gaussian distribution [figure omitted; refer to PDF] , [figure omitted; refer to PDF] (red), [figure omitted; refer to PDF] , [figure omitted; refer to PDF] (red dashed), [figure omitted; refer to PDF] , [figure omitted; refer to PDF] (purple), and [figure omitted; refer to PDF] , [figure omitted; refer to PDF] (purple dashed).

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3.2. Lorentzian Distributed Non-Commutative Framework

Now we consider the case of noncommutative geometry with Lorentzian distribution. The energy density of point-like source under this distribution becomes [8, 15] [figure omitted; refer to PDF] where [figure omitted; refer to PDF] is the noncommutative parameter in Lorentzian distribution. Inserting [figure omitted; refer to PDF] in (7), the differential equation takes the following form: [figure omitted; refer to PDF] The solution of this equation is given by [figure omitted; refer to PDF] where [figure omitted; refer to PDF] is an integration constant. We again assign both solutions as [figure omitted; refer to PDF] and [figure omitted; refer to PDF] and explore the wormhole solutions. In this case, we choose constants as [figure omitted; refer to PDF] , [figure omitted; refer to PDF] , and [figure omitted; refer to PDF] for same dimensions and Gauss-Bonnet coefficient as for noncommutative background.

In Figure 5(a), we plot [figure omitted; refer to PDF] versus [figure omitted; refer to PDF] which represents that the condition for wormhole geometry, that is, [figure omitted; refer to PDF] , holds for [figure omitted; refer to PDF] and [figure omitted; refer to PDF] dimensions with negative [figure omitted; refer to PDF] . For positive [figure omitted; refer to PDF] , the positivity of this expression depends on some ranges so that it remains positive for [figure omitted; refer to PDF] for [figure omitted; refer to PDF] while [figure omitted; refer to PDF] observes the range [figure omitted; refer to PDF] . Figure 5(b) corresponds to the plot of [figure omitted; refer to PDF] with respect to [figure omitted; refer to PDF] showing positive behavior for positive [figure omitted; refer to PDF] . For [figure omitted; refer to PDF] , it expresses a very short range, [figure omitted; refer to PDF] , for positivity whereas it remains negative for [figure omitted; refer to PDF] -dimensional solution. That is, we have no wormhole solution for [figure omitted; refer to PDF] , [figure omitted; refer to PDF] taking negative root solution. So, we skip this case in further discussion. The behavior of [figure omitted; refer to PDF] and [figure omitted; refer to PDF] remains positive for all cases except [figure omitted; refer to PDF] , [figure omitted; refer to PDF] for which it describes negative behavior, as shown in Figures 6(a) and 6(b). This implies that we have no wormhole solutions for [figure omitted; refer to PDF] -dimensional case with negative Gauss-Bonnet coefficient for both solutions.

Figure 5: Plots of (a) [figure omitted; refer to PDF] and (b) [figure omitted; refer to PDF] versus [figure omitted; refer to PDF] in Lorentzian distribution for [figure omitted; refer to PDF] , [figure omitted; refer to PDF] (red), [figure omitted; refer to PDF] , [figure omitted; refer to PDF] (red dashed), and [figure omitted; refer to PDF] , [figure omitted; refer to PDF] (purple).

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Figure 6: Plots of (a) [figure omitted; refer to PDF] and (b) [figure omitted; refer to PDF] versus [figure omitted; refer to PDF] in Lorentzian distribution for [figure omitted; refer to PDF] , [figure omitted; refer to PDF] (red), [figure omitted; refer to PDF] , [figure omitted; refer to PDF] (red dashed), and [figure omitted; refer to PDF] , [figure omitted; refer to PDF] (purple). For (a) [figure omitted; refer to PDF] , [figure omitted; refer to PDF] , and [figure omitted; refer to PDF] (purple dashed).

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Figure 7(a) expresses the behavior of [figure omitted; refer to PDF] for positive root solution versus [figure omitted; refer to PDF] which remains positive for the range [figure omitted; refer to PDF] for [figure omitted; refer to PDF] and [figure omitted; refer to PDF] with positive [figure omitted; refer to PDF] and then turns towards negative behavior. It demonstrates negative behavior for [figure omitted; refer to PDF] and then moves to positive region. Incorporating [figure omitted; refer to PDF] solution, [figure omitted; refer to PDF] shows positive behavior only for the case [figure omitted; refer to PDF] , [figure omitted; refer to PDF] and negative behavior for the remaining two cases as shown in Figure 7(b). In Figures 8(a) and 8(b), we draw [figure omitted; refer to PDF] for both solutions versus [figure omitted; refer to PDF] . This expression represents the negative behavior for ( [figure omitted; refer to PDF] , [figure omitted; refer to PDF] ), ( [figure omitted; refer to PDF] , [figure omitted; refer to PDF] ) with [figure omitted; refer to PDF] and ( [figure omitted; refer to PDF] , [figure omitted; refer to PDF] ) with [figure omitted; refer to PDF] and preserves positivity for ( [figure omitted; refer to PDF] , [figure omitted; refer to PDF] ) with [figure omitted; refer to PDF] , ( [figure omitted; refer to PDF] , [figure omitted; refer to PDF] ), ( [figure omitted; refer to PDF] , [figure omitted; refer to PDF] ) with [figure omitted; refer to PDF] solution.

Figure 7: Plots of (a) [figure omitted; refer to PDF] for [figure omitted; refer to PDF] and (b) [figure omitted; refer to PDF] for [figure omitted; refer to PDF] versus [figure omitted; refer to PDF] in Lorentzian distribution for [figure omitted; refer to PDF] , [figure omitted; refer to PDF] (red), [figure omitted; refer to PDF] , [figure omitted; refer to PDF] (red dashed), and [figure omitted; refer to PDF] , [figure omitted; refer to PDF] (purple).

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Figure 8: Plots of (a) [figure omitted; refer to PDF] for [figure omitted; refer to PDF] and (b) [figure omitted; refer to PDF] for [figure omitted; refer to PDF] versus [figure omitted; refer to PDF] in Lorentzian distribution for [figure omitted; refer to PDF] , [figure omitted; refer to PDF] (red), [figure omitted; refer to PDF] , [figure omitted; refer to PDF] (red dashed), and [figure omitted; refer to PDF] , [figure omitted; refer to PDF] (purple).

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4. Equilibrium Condition

In order to find the equilibrium configuration of the wormhole solutions in Gaussian as well as Lorentzian distributed noncommutative backgrounds, we use the generalized Tolman-Oppenheimer-Volkoff equation. This equation is derived by solving the Einstein equations for a general time-invariant, spherically symmetric metric having metric tensor [figure omitted; refer to PDF] , where [figure omitted; refer to PDF] represents only diagonal entries and [figure omitted; refer to PDF] are general metric functions dependent on [figure omitted; refer to PDF] . The generalized Tolman-Oppenheimer-Volkoff equation is [figure omitted; refer to PDF] Keeping in mind the above equation, de Leon [28] proposed an equation for anisotropic mass distribution which naturally gives the equilibrium for the wormhole subject. It is given by [figure omitted; refer to PDF] where effective gravitational mass [figure omitted; refer to PDF] is measured from throat to some arbitrary radius [figure omitted; refer to PDF] . Accordingly, the gravitational, hydrostatic, and anisotropic force due to anisotropic matter distribution are defied as follows: [figure omitted; refer to PDF] It is required that [figure omitted; refer to PDF] must hold for the wormhole solutions to be in equilibrium. In the underlying cases, we proceed with constant redshift function [figure omitted; refer to PDF] which vanishes the gravitational contribution [figure omitted; refer to PDF] in the equilibrium equation; that is, [figure omitted; refer to PDF] leads to [figure omitted; refer to PDF] for constant [figure omitted; refer to PDF] . Thus, we are left with hydrostatic and anisotropic forces with corresponding equilibrium condition as [figure omitted; refer to PDF] Using (8) and (9), we obtain the following expressions for the hydrostatic and anisotropic forces: [figure omitted; refer to PDF] Figure 9 represents the plots of anisotropic as well as hydrostatic forces for the wormhole solutions in Gaussian distributed framework. Figures 9(a) and 9(c) describe the equilibrium for positive root solution for [figure omitted; refer to PDF] , [figure omitted; refer to PDF] and [figure omitted; refer to PDF] through opposite behavior and hence they cancel each other in order to satisfy (20). For negative root solution, [figure omitted; refer to PDF] , Figures 9(b) and 9(d) show the stable configuration of wormhole solutions for fifth dimensional case only. The behaviors of both forces (which are not in opposite manner) do not cancel each other so there is no equilibrium configuration examined for sixth dimensional wormhole solutions. In the case of Lorentzian noncommutative background, Figure 10 expresses that all wormhole solutions are in equilibrium by satisfying the equilibrium condition for both dimensions.

Figure 9: Plots of (a) [figure omitted; refer to PDF] for [figure omitted; refer to PDF] , (b) [figure omitted; refer to PDF] for [figure omitted; refer to PDF] , (c) [figure omitted; refer to PDF] for [figure omitted; refer to PDF] , (d) [figure omitted; refer to PDF] for [figure omitted; refer to PDF] versus [figure omitted; refer to PDF] with Gaussian distribution for [figure omitted; refer to PDF] , [figure omitted; refer to PDF] (red), [figure omitted; refer to PDF] , [figure omitted; refer to PDF] (red dashed), and [figure omitted; refer to PDF] , [figure omitted; refer to PDF] (purple).

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Figure 10: Plots of (a) [figure omitted; refer to PDF] for [figure omitted; refer to PDF] , (b) [figure omitted; refer to PDF] for [figure omitted; refer to PDF] , (c) [figure omitted; refer to PDF] for [figure omitted; refer to PDF] , (d) [figure omitted; refer to PDF] for [figure omitted; refer to PDF] versus [figure omitted; refer to PDF] with Lorentzian distribution for [figure omitted; refer to PDF] , [figure omitted; refer to PDF] (red), [figure omitted; refer to PDF] , [figure omitted; refer to PDF] (red dashed), and [figure omitted; refer to PDF] , [figure omitted; refer to PDF] (purple).

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5. Conclusion

It is a well-known fact that the existence of wormhole solutions is based on violation of NEC. Since the normal matter satisfies the energy conditions this violation is associated with an energy-momentum tensor which provides exotic matter, a hypothetical form of matter. To explore realistic model or physically acceptable wormhole solutions, it is necessary to find such a source which gives the violation of NEC while normal matter meets the energy conditions. Here in this paper, we have explored wormhole solutions in [figure omitted; refer to PDF] -dimensional Einstein Gauss-Bonnet gravity with Gaussian and Lorentzian noncommutative backgrounds. We have restricted ourselves to fifth and sixth dimensional cases with positive as well as negative Gauss-Bonnet coefficient. Also, we have checked the condition of equilibrium for the wormhole solutions.

The results are summarized in Tables 1 and 2. It is noted that the [figure omitted; refer to PDF] (Tables 1 and 3) and [figure omitted; refer to PDF] (Tables 2 and 4) represent the two roots of the solutions in both backgrounds and EC denotes the equilibrium condition.

Table 1: Wormhole solutions with Gaussian distributed noncommutative framework for [figure omitted; refer to PDF] .

Expressions	[figure omitted; refer to PDF]	[figure omitted; refer to PDF]	[figure omitted; refer to PDF]	[figure omitted; refer to PDF]
[figure omitted; refer to PDF]	Positive	Positive for [figure omitted; refer to PDF]	Positive	Positive for [figure omitted; refer to PDF]
[figure omitted; refer to PDF]	Positive	Positive	Positive	Positive
[figure omitted; refer to PDF]	Positive	Negative	Positive	Negative
[figure omitted; refer to PDF]	Negative	Positive	Negative	Positive
WEC	Violates	Violates	Violates	Violates
E.C	Holds	Holds	Holds	Holds

Table 2: Wormhole solutions with Gaussian distributed noncommutative framework for [figure omitted; refer to PDF] .

Expressions	[figure omitted; refer to PDF]	[figure omitted; refer to PDF]	[figure omitted; refer to PDF]	[figure omitted; refer to PDF]
[figure omitted; refer to PDF]	Positive	Positive for [figure omitted; refer to PDF]	Positive	Positive for [figure omitted; refer to PDF]
[figure omitted; refer to PDF]	Positive	Positive	Positive	Positive
[figure omitted; refer to PDF]	Positive	Negative	Positive	Negative
[figure omitted; refer to PDF]	Positive	Negative	Positive	Negative
WEC	Holds	Violates	Holds	Violates
E.C	Holds	Holds	Does not hold	Does not hold

Table 3: Wormhole solutions with Lorentzian noncommutative background for [figure omitted; refer to PDF] .

Expressions	[figure omitted; refer to PDF]	[figure omitted; refer to PDF]	[figure omitted; refer to PDF]
[figure omitted; refer to PDF]	Positive for [figure omitted; refer to PDF]	Positive	Positive for [figure omitted; refer to PDF]
[figure omitted; refer to PDF]	Positive	Positive	Positive
[figure omitted; refer to PDF]	Positive for [figure omitted; refer to PDF]	Positive for [figure omitted; refer to PDF]	Positive for [figure omitted; refer to PDF]
[figure omitted; refer to PDF]	Negative	Negative	Positive
WEC	Does not hold	Does not hold	Holds for [figure omitted; refer to PDF]
EC	Holds	Holds	Holds

Table 4: Wormhole solutions with Lorentzian noncommutative background for [figure omitted; refer to PDF] .

Expressions	[figure omitted; refer to PDF]	[figure omitted; refer to PDF]	[figure omitted; refer to PDF]
[figure omitted; refer to PDF]	Positive	Positive for [figure omitted; refer to PDF]	Positive
[figure omitted; refer to PDF]	Positive	Positive	Positive
[figure omitted; refer to PDF]	Positive	Negative	Negative
[figure omitted; refer to PDF]	Positive	Negative	Positive
WEC	Holds	Does not hold	Does not hold
E.C	Holds	Holds	Holds

In the Lorentzan distributed noncommutative framework, we have found negative energy density for [figure omitted; refer to PDF] while violation of [figure omitted; refer to PDF] incorporating [figure omitted; refer to PDF] for the case [figure omitted; refer to PDF] , [figure omitted; refer to PDF] so we skipped this case. The remaining results are summarized in Tables 3 and 4.

In the paper [20], higher dimensional asymptotically flat wormhole solutions have been explored in the framework of Gauss-Bonnet gravity by considering a specific choice for a radial dependent redshift function and by imposing a particular equation of state. The WEC is satisfied at the throat by considering a negative Gauss-Bonnet coupling constant. Furthermore, they have considered a constant redshift function and shown specifically that, for negative Gauss-Bonnet coupling constant, one may have normal matter in a determined radial region and that the increase of coupling constant enlarges the normal matter region. In the present paper, we have taken energy density under noncommutative geometry distributions instead of particular equation of state. We have obtained results for positive Gauss-Bonnet coefficient satisfying energy conditions. It contains fifth dimensional wormhole solutions in both backgrounds satisfying equilibrium condition and sixth dimensional with disequilibrium in noncommutative background with [figure omitted; refer to PDF] solution. Also, there is possibility for the existence of wormhole in equilibrium satisfying WEC for [figure omitted; refer to PDF] , [figure omitted; refer to PDF] taking into account [figure omitted; refer to PDF] solution for the range [figure omitted; refer to PDF] .

Conflict of Interests

The authors declare that there is no conflict of interests regarding the publication of this paper.

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