# Lorentz Distributed NoncommutativeF(T,TG) Wormhole Solutions

Authors: M. Sharif; Kanwal Nazir
Journal: Advances in High Energy Physics
 (2018)

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## Abstract

The aim of this paper is to study static spherically symmetric noncommutativeF(T,TG) wormhole solutions along with Lorentzian distribution. Here, T and TG are torsion scalar and teleparallel equivalent Gauss-Bonnet term, respectively. We take a particular redshift function and two F(T,TG) 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.


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## Body

## 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,k-essence, Chaplygin gas, and quintessence [1–5].The second way leads to gravitational modification which results in modified theories of gravity. Among these theories, theF(T) 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 F(T) theory is proposed by involving higher order torsion correction terms named as F(T,TG) theory depending upon T and TG [9]. This is a completely different theory which does not correspond to F(T) 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 F(T,TG) 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 f(R) 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 F(T) wormhole geometry by considering a particular F(T) 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 f(G) 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 f(R) theory. Sharif and Rani [26] investigated wormhole solutions with the effects of electrostatic field and for galactic halo regions in F(T) 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 F(T) gravity. We have explored noncommutative geometry in F(T,TG) 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 F(T,TG) gravity along with noncommutative Lorentz distributed geometry. We study wormhole geometry and corresponding energy conditions.The paper is arranged as follows. Section2 briefly recalls the basics of F(T,TG) theory, the wormhole geometry, and energy conditions. In Section 3, we investigate physically acceptable wormhole solutions and energy conditions for two particular F(T,TG) models. In Section 4, we analyze the stability of these wormhole solutions. The last section summarizes the results.


## 2.FT,TG Gravity

This section presents some basic review ofF(T,TG) gravity. The idea of such extension is to construct an action involving higher order torsion terms. In curvature theory other than simple modification as f(R) theory, one can propose the higher order curvature correction terms in order to modify the action such as GB combination G or functions f(G). 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 fieldea(xλ). The simplest one is the trivial tetrad which can be expressed as ea=δλa∂λ and eb=δλb∂λ, where the Kronecker delta is denoted by δaλ. 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(1)ha=haλ∂λ,hb=haλdxλ. The nontrivial tetrad satisfies haλhbλ=δba and haλhaμ=δλμ. The tetrad fields can be related to metric tensor through(2)gλμ=ηabhλahμb, where ηab=diag⁡(1,-1,-1,-1) is the Minkowski metric. Here, Greek indices (λ,μ) represent coordinates on manifold and Latin indices (a,b) correspond to the coordinates on tangent space. The other field is described as the connection 1-forms ωab(xλ) which are the source of parallel transportation, also known as Weitzenböck connection. It has the following form:(3)ωλνμ=hμahaλ,ν.The structure coefficientsCabc appear in commutation relation of the tetrad as(4)Cabc=hc-1ha,hb,where(5)Cabc=hμbhλahcλ,μ-hcμ,λ. The torsion as well as curvature tensors has the following expressions:(6)Tbca=-Cbca-ωbca+ωcba,Rbcda=ωbdeωeca+ωbd,ca-Ccdeωbea-ωbceωeda-ωbc,da. The contorsion tensor can be described as(7)Kabc=-Kbac=12-Tabc+Tcab-Tbca. Both the torsion scalars are written as(8)T=14TabcTabc+12TabcTcba-TabaTcbc,TG=Kea2bKa3fcKa1eaKfa4d+2Kea4fKfcdKa1a2aKa3eb+2Kea4c,dKa3eb×Ka1a2a-2Ka3ebKefcKa1a2aKfa4dδa1a2a3a4abcd. This comprehensive theory has been proposed by Kofinas et al. [10] whose action is described as(9)S=∫hFT,TGκ2+Lmd4x, where Lm is the matter Lagrangian, κ2=1, g represents determinant of the metric coefficients, and h=-g=det⁡(hλa). The field equations obtained by varying the action about hλa are given as(10)CbcdHdca+2Hacd+-TGFTGT,TG+FT,TG-TFTT,TGηab+2Hbac-Hkcba+HacbCddc+2-Hcba+Hacb+Hbac,c+4Hdbc×Cdca+TacdHcdb-Hab=κ2Tab, where(11)Habc=ηacKbdd-KbcaFTT,TG+FTGT,TGϵablfKdqrKldp+2KbcpϵadlfKdqr+KilpϵqdlfKjdrKqftϵkprt+ϵabldKfdpϵcprtKlfr,t-12CqtrKlfq+ϵcprtKdfpϵaldfKbkr,t-12CqtrKblq+ϵcprtϵaldf×FTGT,TGKblqKdfrCqpt+KblpFTGT,TGKdfr,t,Hab=FTT,TGϵalceKlfrϵbrteKfct. Here, Tab represents the matter energy-momentum tensor. The functions FT and FTG are the derivatives of F with respect to T and TG, respectively. Notice that, for F(T,TG)=-T, teleparallel equivalent to GR is achieved. Also, for TG=0, we can obtain F(T) 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](12)ds2=e2αrdt2-dr21-βr/r-r2dθ2-r2sin2⁡θdϕ2,where α(r) is the redshift function and β(r) represents the shape function. The gravitational redshift is measured through the function α(r) whereas β(r) controls the wormhole shape. The radial coordinate r, 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, α(r) must be finite throughout. For this purpose, we assumed zero redshift function that implies e2α(r)→1. There are two properties related to the shape function to maintain the wormhole geometry. The first property is positiveness; that is, as r→∞, β(r) must be defined as a positive function. The second is flaring-out condition; that is, β(r)-rβ′(r)/β2(r)>0 and β(r)=rth at r=rth with β′(rth)<1 (rth is the wormhole throat radius). The condition of asymptotic flatness (β(r)/r→0 as r→∞) should be fulfilled by the space-time at large distances.To investigate the wormhole solutions, we assume a diagonal tetrad [31] as(13)hλa=diage-αr,11-βr/r,r,rsin⁡θ.This is the simplest and frequently used tetrad for the Morris and Thorne static spherically symmetric metric. This also provides nonzero TG which is the basic ingredient for this theory. If we take some other tetrad then it may lead to zero TG. Thus these orthonormal bases are most suitable for this theory. The torsion scalars turn out to be(14)T=4r1-βrrα′+2r21-βrr,(15)TG=8βrα′rr4-8βrα′2rr31-βrr+12βrα′rβ′rr4-8β′rα′rr3-12β2rα′rr5-8βrα′′rr31-βrr.In order to satisfy the condition of no horizon for a traversable wormhole, we have to assume α(r)=0. Substituting this assumption in the above torsion scalars, we obtain TG=0 which means that the function F(T,TG) reduces to F(T) representing F(T) theory. Hence, we cannot take α(r) as a constant function; instead we assume α(r) as(16)αr=-ψr,ψ>0,which is finite and nonzero for r>0. 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 as(17)Tmλμ=pt+ρVλVμ-gλμpt+pr-ptημηλ,where ρ, Vλ, ηλ, pr, and pt represent the energy density, four-velocity, radial space-like four-vector orthogonal to Vλ, and radial and tangential components of pressure, respectively. We consider energy-momentum tensor as T(m)λμ=diag⁡(ρ,-pr,-pt,-pt). Using (12)–(16) in (10), we obtain the field equations as(18)ρ=FT,TG+2β′rr2FTT,TG-TGFTGT,TG-TFTT,TG-4FT′r1-βrr+4FTG′T,TGr35βrr-3β2rr2-2-3β′r1-βrr+8FTG′′T,TGr21-2-βrrβrr,(19)pr=-FT,TG+FTT,TGT-4ψr3-2βrr3+4βrψr4+TGFTGT,TG+48r41-βrr2ψFTG′T,TG,(20)pt=-FT,TG+TGFTGT,TG+TFTT,TG+βrr3-2ψr3-β′rr2+βrψr4+2ψ2r4+β′rψr3-2βrψ2r5-4βrψr4+4ψr3FTT,TG+21r-1-βrrψ′+βrψr3FT′T,TG+12ψβrr5-12ψβ2rr6+16βrψ2r6+12ψβ′rr4-8ψ2r5-8β2rψ2r7+12βrψβ′rr5-16ψr4-16β2rψr6-32βrψr5FTG′T,TG+8ψr31-βrr2+βrr×FTG′′T,TG, where prime stands for the derivative with respect to r.


### 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 uλ and kλ, respectively; the Raychaudhuri equations are formulated as follows:(21)dΘdτ-ωλμωλμ+Rλμuλuμ+13Θ2+σλμσλμ=0,dΘdχ-ωλμωλμ+Rλμkλkμ+12Θ2+σλμσλμ=0, where the expansion scalar Θ is used to explain expansion of the volume and shear tensor σλμ provides the information about the volume distortion. The vorticity tensor ωλμ explains the rotating curves. The positive parameters χ and τ 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 Θ=-τRλμuλuμ=-χRλμkλkμ. The expression Θ<0 ensures the attractiveness of gravity which leads to Rλμuλuμ≥0 and Rλμkλkμ≥0. In modified theories, the Ricci tensor is replaced by the effective energy-momentum tensor, that is, Tλμ(eff)uλuμ≥0 and Tλμ(eff)kλkμ≥0 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 tensorTλμeff in the corresponding energy conditions. This effective energy-momentum tensor is given as(22)Tλμeff=TλμH+Tλμm, where Tλμ(H) are dark source terms related to the underlying F(T,TG) theory. The condition (violation of NEC) related to Tλμ(eff) 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:pn(eff)+ρ(eff)≥0,  where n=1,2,3.(ii)
WEC:pn(eff)+ρ(eff)≥0,ρ(eff)≥0.(iii)
DEC:pn(eff)±ρ(eff)≥0,ρ(eff)≥0.(iv)
SEC:pn(eff)+ρ(eff)≥0,ρ(eff)+3p(eff)≥0.Solving (18) and (19) for effective energy density and pressure, we evaluate the radial effective NEC as(23)preff+ρeff=1FTT,TG-βrr3+β′rr2+2r1-βrrα′. So, pr(eff)+ρ(eff)<0 represents the violation of effective NEC as(24)-βrr3+β′rr2+2r1-βrrα′<0.If this condition holds then it shows that the traversable wormhole exists 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](12)ds2=e2αrdt2-dr21-βr/r-r2dθ2-r2sin2⁡θdϕ2,where α(r) is the redshift function and β(r) represents the shape function. The gravitational redshift is measured through the function α(r) whereas β(r) controls the wormhole shape. The radial coordinate r, 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, α(r) must be finite throughout. For this purpose, we assumed zero redshift function that implies e2α(r)→1. There are two properties related to the shape function to maintain the wormhole geometry. The first property is positiveness; that is, as r→∞, β(r) must be defined as a positive function. The second is flaring-out condition; that is, β(r)-rβ′(r)/β2(r)>0 and β(r)=rth at r=rth with β′(rth)<1 (rth is the wormhole throat radius). The condition of asymptotic flatness (β(r)/r→0 as r→∞) should be fulfilled by the space-time at large distances.To investigate the wormhole solutions, we assume a diagonal tetrad [31] as(13)hλa=diage-αr,11-βr/r,r,rsin⁡θ.This is the simplest and frequently used tetrad for the Morris and Thorne static spherically symmetric metric. This also provides nonzero TG which is the basic ingredient for this theory. If we take some other tetrad then it may lead to zero TG. Thus these orthonormal bases are most suitable for this theory. The torsion scalars turn out to be(14)T=4r1-βrrα′+2r21-βrr,(15)TG=8βrα′rr4-8βrα′2rr31-βrr+12βrα′rβ′rr4-8β′rα′rr3-12β2rα′rr5-8βrα′′rr31-βrr.In order to satisfy the condition of no horizon for a traversable wormhole, we have to assume α(r)=0. Substituting this assumption in the above torsion scalars, we obtain TG=0 which means that the function F(T,TG) reduces to F(T) representing F(T) theory. Hence, we cannot take α(r) as a constant function; instead we assume α(r) as(16)αr=-ψr,ψ>0,which is finite and nonzero for r>0. 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 as(17)Tmλμ=pt+ρVλVμ-gλμpt+pr-ptημηλ,where ρ, Vλ, ηλ, pr, and pt represent the energy density, four-velocity, radial space-like four-vector orthogonal to Vλ, and radial and tangential components of pressure, respectively. We consider energy-momentum tensor as T(m)λμ=diag⁡(ρ,-pr,-pt,-pt). Using (12)–(16) in (10), we obtain the field equations as(18)ρ=FT,TG+2β′rr2FTT,TG-TGFTGT,TG-TFTT,TG-4FT′r1-βrr+4FTG′T,TGr35βrr-3β2rr2-2-3β′r1-βrr+8FTG′′T,TGr21-2-βrrβrr,(19)pr=-FT,TG+FTT,TGT-4ψr3-2βrr3+4βrψr4+TGFTGT,TG+48r41-βrr2ψFTG′T,TG,(20)pt=-FT,TG+TGFTGT,TG+TFTT,TG+βrr3-2ψr3-β′rr2+βrψr4+2ψ2r4+β′rψr3-2βrψ2r5-4βrψr4+4ψr3FTT,TG+21r-1-βrrψ′+βrψr3FT′T,TG+12ψβrr5-12ψβ2rr6+16βrψ2r6+12ψβ′rr4-8ψ2r5-8β2rψ2r7+12βrψβ′rr5-16ψr4-16β2rψr6-32βrψr5FTG′T,TG+8ψr31-βrr2+βrr×FTG′′T,TG, where prime stands for the derivative with respect to r.


## 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 uλ and kλ, respectively; the Raychaudhuri equations are formulated as follows:(21)dΘdτ-ωλμωλμ+Rλμuλuμ+13Θ2+σλμσλμ=0,dΘdχ-ωλμωλμ+Rλμkλkμ+12Θ2+σλμσλμ=0, where the expansion scalar Θ is used to explain expansion of the volume and shear tensor σλμ provides the information about the volume distortion. The vorticity tensor ωλμ explains the rotating curves. The positive parameters χ and τ 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 Θ=-τRλμuλuμ=-χRλμkλkμ. The expression Θ<0 ensures the attractiveness of gravity which leads to Rλμuλuμ≥0 and Rλμkλkμ≥0. In modified theories, the Ricci tensor is replaced by the effective energy-momentum tensor, that is, Tλμ(eff)uλuμ≥0 and Tλμ(eff)kλkμ≥0 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 tensorTλμeff in the corresponding energy conditions. This effective energy-momentum tensor is given as(22)Tλμeff=TλμH+Tλμm, where Tλμ(H) are dark source terms related to the underlying F(T,TG) theory. The condition (violation of NEC) related to Tλμ(eff) 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:pn(eff)+ρ(eff)≥0,  where n=1,2,3.(ii)
WEC:pn(eff)+ρ(eff)≥0,ρ(eff)≥0.(iii)
DEC:pn(eff)±ρ(eff)≥0,ρ(eff)≥0.(iv)
SEC:pn(eff)+ρ(eff)≥0,ρ(eff)+3p(eff)≥0.Solving (18) and (19) for effective energy density and pressure, we evaluate the radial effective NEC as(23)preff+ρeff=1FTT,TG-βrr3+β′rr2+2r1-βrrα′. So, pr(eff)+ρ(eff)<0 represents the violation of effective NEC as(24)-βrr3+β′rr2+2r1-βrrα′<0.If 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 massM has the following form [34]:(25)ρNCL=Mθπ2θ+r22,where θ is the noncommutative parameter. Comparing (18) and (25), that is, ρNCL=ρ, we obtain(26)Mθπ2θ+r22=FT,TG+2β′rFTr2-TFTT,TG-4FT′T,TGr1-βrr-TGFTGT,TG+4FTG′T,TGr35βrr-2-3β2rr2-31-βrrβ′r+8FTG′′T,TGr21-βrr2-βrr.The above equation contains two unknown functions F(T,TG) and β(r). 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 F(T,TG) 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](27)FT,TG=-T+γ1T2+γ2TG+γ3T2+γ4TG2,where γ1, γ2, γ3, and γ4 are arbitrary constants. Here, we take γ2 and γ4 as dimensionless ones whereas γ1 and γ3 have dimensions of lengths. This model involves second-order TG terms and fourth-order contribution from torsion term T. Using (14), (15), and (27) in (26), we achieve a complicated differential equation in terms of β(r) that cannot be handled analytically. So, we solve it numerically by choosing the corresponding parameters as γ1=81, γ2=-0.0091, γ3=12, and γ4=32. The values of the remaining parameters M=15, θ=0.5, and ψ=1 are taken from [28]. To plot the graph of β(r), we take the initial values as β(1)=0.7, β′(1)=9.9, and β′′(1)=5.5. Figure 1(a) represents the increasing behavior of shape function β(r). We discuss the wormhole throat by plotting β(r)-r in Figure 1(b).Figure 1
Plots ofβ(r), β(r)-r and β(r)/r versus r for the first model.
(a)
(b)
(c)As we know, throat radius is the point whereβ(r)-r cuts the r-axis. Here, the throat radius is located at rth=1.029 which also satisfies the condition β(r)=rth up to two digits; that is, β(1.029)=1.028. Figure 1(c) implies that the space-time does not satisfy the asymptotic flatness condition. Figure 2(a) represents the validity of condition (24). Thus, the violation of effective NEC confirms the presence of traversable wormhole. Also, Figure 2(b) shows the plots of ρ+pr, Figure 2(c)  ρ+pt, and Figure 2(d)  ρ for normal matter that exhibit positive behavior in the interval 1.003<r<1.015. This shows that ordinary matter satisfies the NEC and physically acceptable wormhole solution is achieved for this model.Figure 2
Plots ofρ(eff)+pr(eff), ρ+pr, ρ+pt, and ρ versus r for the first model.
(a)
(b)
(c)
(d)


### 3.2. Second Model

We assume the second model as [10](28)FT,TG=-T+η1T2+η2TG,where η1 and η2 are the arbitrary constants. We get a differential equation by substituting (14), (15), and (28) in (26). The numerical technique is used to calculate β(r) from the differential equation by assuming same values of θ, M, and ψ as above. The model parameters are taken as η1=-1.1259 and η2=-0.9987. Also, we take the following conditions: β(1.5)=2.1, β′(1.5)=-133.988, and β′′(1.5)=-60000. We discuss the properties necessary for the development of wormhole structure. The plot of shape function is shown in Figure 3(a) which represents increasing behavior for all values of r. It can be noted that β(0.5)=0.5. In Figure 3(b), we plot β(r)-r versus r to discuss the location of wormhole throat. It can be observed that small values of r refer to the throat radius.Figure 3
Plots ofβ(r), β(r)-r, and β(r)/r versus r for the second model.
(a)
(b)
(c)Figure3(c) represents the behavior of β(r)/r. It can be seen that as the value of r increases, the curve of β(r)/r approaches 0. Hence, the space-time satisfies asymptotically flatness condition of Figure 4(a) which represents the negative behavior and shows the validity of condition (24). For physically acceptable wormhole solution, we check the graphical behavior of NEC and WEC for matter energy density and pressure. Figure 4 shows that ρ+pr, ρ+pt, and ρ behave positively in the intervals 1.32≤r≤1.474, 1.28≤r≤1.342, and 1.307≤r≤1.471, respectively. The common region of these intervals is 1.28≤r≤1.342. This indicates that NEC and WEC are satisfied in a very small interval. Thus there can exist a micro or tiny physically acceptable wormhole for this model. Tiny wormhole means small radius with narrow throat.Figure 4
Plots ofρ(eff)+pr(eff), ρ+pr, ρ+pt, and ρ versus r for the second model.
(a)
(b)
(c)
(d)


## 3.1. First Model

The first model is considered as [15](27)FT,TG=-T+γ1T2+γ2TG+γ3T2+γ4TG2,where γ1, γ2, γ3, and γ4 are arbitrary constants. Here, we take γ2 and γ4 as dimensionless ones whereas γ1 and γ3 have dimensions of lengths. This model involves second-order TG terms and fourth-order contribution from torsion term T. Using (14), (15), and (27) in (26), we achieve a complicated differential equation in terms of β(r) that cannot be handled analytically. So, we solve it numerically by choosing the corresponding parameters as γ1=81, γ2=-0.0091, γ3=12, and γ4=32. The values of the remaining parameters M=15, θ=0.5, and ψ=1 are taken from [28]. To plot the graph of β(r), we take the initial values as β(1)=0.7, β′(1)=9.9, and β′′(1)=5.5. Figure 1(a) represents the increasing behavior of shape function β(r). We discuss the wormhole throat by plotting β(r)-r in Figure 1(b).Figure 1
Plots ofβ(r), β(r)-r and β(r)/r versus r for the first model.
(a)
(b)
(c)As we know, throat radius is the point whereβ(r)-r cuts the r-axis. Here, the throat radius is located at rth=1.029 which also satisfies the condition β(r)=rth up to two digits; that is, β(1.029)=1.028. Figure 1(c) implies that the space-time does not satisfy the asymptotic flatness condition. Figure 2(a) represents the validity of condition (24). Thus, the violation of effective NEC confirms the presence of traversable wormhole. Also, Figure 2(b) shows the plots of ρ+pr, Figure 2(c)  ρ+pt, and Figure 2(d)  ρ for normal matter that exhibit positive behavior in the interval 1.003<r<1.015. This shows that ordinary matter satisfies the NEC and physically acceptable wormhole solution is achieved for this model.Figure 2
Plots ofρ(eff)+pr(eff), ρ+pr, ρ+pt, and ρ versus r for the first model.
(a)
(b)
(c)
(d)


## 3.2. Second Model

We assume the second model as [10](28)FT,TG=-T+η1T2+η2TG,where η1 and η2 are the arbitrary constants. We get a differential equation by substituting (14), (15), and (28) in (26). The numerical technique is used to calculate β(r) from the differential equation by assuming same values of θ, M, and ψ as above. The model parameters are taken as η1=-1.1259 and η2=-0.9987. Also, we take the following conditions: β(1.5)=2.1, β′(1.5)=-133.988, and β′′(1.5)=-60000. We discuss the properties necessary for the development of wormhole structure. The plot of shape function is shown in Figure 3(a) which represents increasing behavior for all values of r. It can be noted that β(0.5)=0.5. In Figure 3(b), we plot β(r)-r versus r to discuss the location of wormhole throat. It can be observed that small values of r refer to the throat radius.Figure 3
Plots ofβ(r), β(r)-r, and β(r)/r versus r for the second model.
(a)
(b)
(c)Figure3(c) represents the behavior of β(r)/r. It can be seen that as the value of r increases, the curve of β(r)/r approaches 0. Hence, the space-time satisfies asymptotically flatness condition of Figure 4(a) which represents the negative behavior and shows the validity of condition (24). For physically acceptable wormhole solution, we check the graphical behavior of NEC and WEC for matter energy density and pressure. Figure 4 shows that ρ+pr, ρ+pt, and ρ behave positively in the intervals 1.32≤r≤1.474, 1.28≤r≤1.342, and 1.307≤r≤1.471, respectively. The common region of these intervals is 1.28≤r≤1.342. This indicates that NEC and WEC are satisfied in a very small interval. Thus there can exist a micro or tiny physically acceptable wormhole for this model. Tiny wormhole means small radius with narrow throat.Figure 4
Plots ofρ(eff)+pr(eff), ρ+pr, ρ+pt, and ρ versus r for the second model.
(a)
(b)
(c)
(d)


## 4. Equilibrium Condition

In this section, we investigate equilibrium structure of wormhole solutions. For this purpose, we consider generalized Tolman-Oppenheimer-Volkoff equation in an effective manner as(29)-pr′eff-preff+ρeffα′2+pteff-preff2r=0,with the metric ds2=diag⁡(e2αr,-eνr,-r2,-r2sin2⁡θ), where eν(r)=1-βr/r-1. The above equation can be written as(30)-pr′eff-preff+ρeffMeffeα-ν/2r2+pteff-preff2r=0,where the effective gravitational mass is described as M(eff)=1/2r2eν-α/2ν′. The equilibrium picture describes the stability of corresponding wormhole solutions with the help of three forces known as gravitational force Fgf, anisotropic force Faf, and hydrostatic force Fhf. The gravitational force exists because of gravitating mass, anisotropic force occurs in the presence of anisotropic system, and hydrostatic force is due to hydrostatic fluid. We can rewrite (30) as(31)Fhf+Fgf+Faf=0,where(32)Fgf=-preff+ρeffeα-ν/2Meffr2,Fhf=-pr′eff,Faf=pteff-preff2r. Further, we examine the stability of wormhole solutions for first and second model through equilibrium condition. Using (18)–(20) and (27) in (31), we obtain a difficult equation for the first model. By applying numerical technique, we plot the graphs of the three above defined forces. In Figure 5, it can be easily analyzed that all the three forces cancel their effects and balance each other in the interval 4.8≤r≤5. This means that wormhole solution satisfies the equilibrium condition for the first model. Next, we take the second model and follow the same procedure by using (28). After simplification, we finally get a differential equation and solve it numerically. Figure 6 indicates that the gravitational force is zero but anisotropic and hydrostatic forces completely cancel their effects. Hence, for this model, the system is balanced which confirms the stability of the corresponding wormhole solution.Figure 5
Plot of equilibrium condition for first model.Figure 6
Plot of equilibrium condition for second model.


## 5. Concluding Remarks

In general relativity, the structure of wormhole is based on the condition that NEC is violated. This violation supports the fact that there exists a mysterious matter in the universe famous as exotic matter and distinguished by its negative energy density. The amount of this amazing matter would be minimized to obtain a physically viable wormhole. However, in modified theories, the situation may be completely different. This paper investigates noncommutative wormhole solutions with Lorentzian distribution inF(T,TG) gravity. For this purpose, we have assumed a diagonal tetrad and a particular redshift function. We have examined these wormhole solutions graphically.For the first model, all the properties are satisfied which are necessary for wormhole geometry regarding the shape function except asymptotic flatness. In this case, WEC and NEC for normal matter are also satisfied. Hence, this model provides realistic wormhole solution in a small interval threaded by normal matter rather than exotic matter. The violation of effective NEC confirms the traversability of the wormhole. Furthermore, the second model fulfills all properties regarding shape function and also satisfies WEC and NEC for normal matter. There exists a micro wormhole solution which is supported by normal matter. This model satisfies traversability condition (24). We have investigated stability of both models through equilibrium condition. It is mentioned here that stability is attained for both models.Bhar and Rahaman [27] examined in GR whether the wormhole solutions exist in different dimensional noncommutative space-time with Lorentzian distribution. They found that wormhole solutions appear only for four and five dimensions but no solution exists for higher dimensions. It is interesting to mention here that we have also obtained wormhole solutions that satisfy all the conditions and are stable in F(T,TG) gravity. Our results show consistency with the teleparallel equivalent of GR limits. For the first model, if we substitute γ1=γ3=0, then the behavior of shape function β(r) and energy conditions in teleparallel theory remains the same as in this theory. For the second model, η1=0 provides no result but if we consider η2=0, then β(r) as well as energy conditions represent consistent behavior.InF(T) gravity [35], the resulting noncommutative wormhole solutions are supported by normal matter by assuming diagonal tetrad. In the underlying work, we have also obtained solutions that are threaded by normal matter. Kofinas et al. [36] discussed spherically symmetric solutions in scalar-torsion gravity in which a scalar field is coupled to torsion with a derivative coupling. They obtained exact solution which represents a new wormhole-like solution having interesting physical features. We can conclude that, in F(T,TG) gravity, noncommutative geometry with Lorentzian distribution is a more favorable choice to obtain physically acceptable wormhole solutions rather than noncommutative geometry [29].



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