# Anisotropic Universe inf(G,T) Gravity

Authors: M. Farasat Shamir
Journal: Advances in High Energy Physics
 (2017)

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## Abstract

This paper is devoted to investigating the recently introducedf(G,T) theory of gravity, where G is the Gauss-Bonnet term and T is the trace of the energy-momentum tensor. For this purpose, anisotropic background is chosen and a power law f(G,T) gravity model is used to find the exact solutions of field equations. In particular, a general solution is obtained which is further used to reconstruct some important solutions in cosmological contexts. The physical quantities like energy density, pressure, and equation of state parameter are calculated. A Starobinsky-like f2(T) model is proposed which is used to analyze the behavior of universe for different values of equation of state parameter. It is concluded that presence of term T in the bivariate function f(G,T) may give many cosmologically important solutions of the field equations.


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## Body

## 1. Introduction

Some important modifications of general relativity (GR) have been proposed in the last two decades. The mostly discussed theories aref(R) and f(R,T) theories of gravity (R is the Ricci scalar and T is the trace of energy-momentum tensor) which have been treated most seriously [1–14]. However, recently f(R,T) cosmology has been severely challenged [15]. On the other hand, modified Gauss-Bonnet (GB) gravity is another theory which has gained popularity in the last few years [16–18]. It is also known as f(G) theory of gravity, where f(G) is a generic function of GB invariant G. GB term plays an important role as it may avoid ghost contributions and helps in regularizing the gravitational action [19]. Thus, to save f(T) theories, one may include f(G) terms. A theory with a similar idea has been recently proposed named as f(G,T) gravity [20]. Some interesting work has been done in the recent past using modified GB theories.Anisotropic compact stars in modifiedf(G) gravity have been discussed by Abbas et al. [21]. Houndjo et al. [22] found the exact solutions of f(G) field equations using cylindrical symmetry and it was concluded that there existed seven families of exact solutions for three different forms of f(G) models. The exact cylindrically symmetric solutions of modified field equations recovered cosmic string space-time [23]. A more generalized version of GB gravity known as f(R,G) gravity has also been discussed widely. Wu and Ma [24] investigated the spherically symmetric solutions at low energy where the weak-field and slow-motion limit of f(R,G) gravity was developed. Laurentis et al. [25] discussed cosmological inflation in f(R,G) theory. Sharif and Ikram [26] examined warm inflation in f(G) theory of gravity using scalar fields for the Friedmann-Robertson-Walker (FRW) universe model. Conserved quantities have been recently explored in FRW background using Noether symmetry [27]. Sharif and Fatima [28] discussed the role of GB term for the early and late-time accelerating phases of the universe by considering two viable f(G) models. García et al. [29] explored energy conditions to prove the viability of some f(G) gravity models. f(R,G) gravity energy conditions have been recently explored where the WEC was used along with the recent estimated values of cosmological parameters to determine the viability of some specific choices of f(R,G) gravity models [30].In the context off(G,T) gravity, Sharif and Ikram proved that the massive test particles followed nongeodesic lines of geometry due to the presence of extra force and examined the energy conditions for flat FRW universe [20]. The same authors [31] used reconstruction techniques to reproduce the cosmic evolution corresponding to de Sitter universe, power law solutions, and phantom/nonphantom eras in this theory. In a recent paper [32], f(G,T) theory of gravity was discussed using Noether symmetry approach. Two specific models were studied to determine the conserved quantities and it was concluded that the well-known de Sitter solution could be reconstructed for some specific choice of f(G,T) gravity model. In a recent paper, Sharif and Ikram [33] studied the wormhole solutions using power law f(G,T) gravity models and it was shown that traversable wormhole solutions were physically acceptable in f(G,T) theory of gravity. In another work [34], Noether symmetry methodology has been used to study some cosmologically important f(G,T) gravity models with anisotropic background. It is concluded that the specific models of modified GB gravity may be used to reconstruct ΛCDM cosmology without involving any cosmological constant. For some particular choices of f(G,T) gravity models, it is anticipated that this theory may explain the late-time cosmic acceleration. Thus it seems interesting to explore further the modified f(G,T) gravity. Moreover, in comparison with f(R,G) gravity, the presence of the matter term T in the bivariate function f(G,T) may give many solutions of the field equations and the theory may support the accelerated expansion of universe under certain conditions for the model under consideration.In this paper, we are focussed to investigate the dynamics off(R) gravity with anisotropic background. It is well-known that the isotropic models are among the best choices to study large scale structure of the universe. Moreover, according to the cosmological observations including the cosmic microwave background (CMB) radiation, the current universe is isotropic. However, it is believed that the early universe may not have been exactly uniform. Also the local anisotropies that we observe today in galaxies and super clusters also motivate us to model the universe with anisotropic background. Bianchi type models are among the simplest models with anisotropic background. In particular, the investigation of Bianchi type universe in context of modified theories is interesting. In this work, we are interested to explore f(G,T) gravity using locally rotationally symmetric (LRS) Bianchi type I space-time. We find the exact solutions of the LRS Bianchi type I field equations in f(G) theory of gravity. In particular, a general solution with power law f(G,T) gravity model is reported. The plan of the paper is as follows: some basics of f(G) gravity and field equations are discussed in Section 2. Section 3 is devoted to exploring the exact solutions of modified field equations. Section 4 is used to reconstruct some important cosmological solutions. Final remarks are given in the last section.


## 2. Some Basics off(G,T) Gravity

The modified GB gravity is given by the action [20](1)A=12κ2∫d4x-gR+fG,T+∫d4x-gLM.HereG and T denote the GB term and the trace of the energy-momentum tensor, respectively, whereas LM is the standard matter Lagrangian, R is the Ricci scalar, g is the determinant of metric tensor, and κ is a coupling constant. The field equations can be obtained by varying the action equation (1) with respect to the metric tensor [20](2)Rζη-12gζηR=-2Rgζη∇2-2R∇ζ∇η-4gζηRμν∇μ∇ν-4Rζη∇2+4Rζμ∇η∇μ+4Rημ∇ζ∇μ+4Rζμην∇μ∇νfGG,T+12gζηfG,T-Tζη+ΘζηfTG,T-2RRζη-4RζμRμη-4RζμηνRμν+2RζμνδRημνδfGG,T+κ2Tζη,where the symbols involved have their usual meanings and Θζη=gμν(δTμν/δgζη) and the subscript G or T in the functions denotes the partial derivatives. It would be interesting to notice that if we substitute f(G,T)=f(G) in (2), then the field equations of f(G) gravity are recovered. Moreover, the case f(G,T)=0 reduces the modified field equations to the usual GR equations. For the sake of simplicity, from now onwards we consider f(G,T)≡f, fG(G,T)≡fG, and so forth. The trace of (2) gives(3)R+κ2T-T+ΘfT+2f+2GfG-2R∇2fG+4Rζη∇ζ∇ηfG=0.It may be noticed that this relatesR, G, and T differentially and not algebraically as in GR, where R=-κT. This indicates that the modified field equations may admit many solutions in addition to other modified theories and GR. The covariant divergence of (2) is given by(4)∇ζTζη=fTκ2-fTTζη+Θζη∇ζln⁡fT+∇ζΘζη-gζη2∇ζT,which is not zero. It is due to the presence of higher order derivatives of the energy-momentum tensor that are naturally present in the field equations. Thus the theory might be plagued by divergences at astrophysical scales. This seems to be an issue with some other higher order derivatives theories as well that include higher order terms of energy-momentum tensor. However, to deal with the issue, one can put some constraints to (4) to obtain standard conservation equation [20]. Here we take the spatially homogeneous, anisotropic, LRS Bianchi type I space-time(5)ds2=dt2-X2tdx2-Y2tdy2+dz2,where X and Y are cosmic scale factors. Moreover, we consider that the universe is composed of perfect fluid(6)Tμν=ρ+puμuν-pgμν,where ρ and p denote the energy density and pressure of the fluid, respectively. The Ricci scalar and GB invariant for (5) are given as(7)R=-2X¨X+2Y¨Y+2X˙Y˙XY+Y˙2Y2,G=8X¨Y˙2XY2+2X˙Y˙Y¨XY2,where the overdot denotes the derivative with respect to the time coordinate. Now we define some textbook physical quantities. The average scale factor a and average Hubble parameter H for the model under consideration take the form(8)a=XY23,H=13X˙X+2Y˙Y.The expansion scalarθ and shear scalar σ are given as follows:(9)θ=u;μμ=X˙X+2Y˙Y,σ2=12σμνσμν=13X˙X-Y˙Y2,where(10)σμν=12uμ;αhνα+uν;αhμα-13θhμν,and hμν=gμν-uμuν is the projection tensor. Now, for LRS Bianchi type I space-time (5), the field equations (2) take the form(11)22X˙Y˙XY+Y˙2Y2-24X˙Y˙2XY2f˙G+GfG-f-2ρ+pfT=2κ2ρ,-22Y¨Y+Y˙2Y2+16Y˙Y¨Y2f˙G+8Y˙2Y2f¨G-GfG+f=2κ2p,-2X¨X+Y¨Y+X˙Y˙XY+8X˙Y¨XY+Y˙X¨YXf˙G+8X˙Y˙XYf¨G-GfG+f=2κ2p.These are three highly nonlinear and difficult differential equations with five unknowns. Thus we need an additional constraint to investigate any exact solution. Here we may consider a physical condition that shear scalarσ is proportional to expansion scalar θ which provides(12)X=Yn,where n is an arbitrary real number. In literature [35–38], many authors explored the exact solutions of field equations using this condition. Thus, using (12), field equations (11) take the form(13)22n+1Y˙2Y2-24nY˙3Y3f˙G+GfG-f-2ρ+pfT=2κ2ρ,(14)-22Y¨Y+Y˙2Y2+16Y˙Y¨Y2f˙G+8Y˙2Y2f¨G-GfG+f=2κ2p,(15)-2n+1Y¨Y+n2Y˙2Y2+82nY˙Y¨Y2+nn-1Y˙3Y3f˙G+8nY˙2Y2f¨G-GfG+f=2κ2p.Now we investigate the exact solutions of these field equations.


## 3. Exact Solutions of Modified Field Equations

We consider thef(G,T) model as(16)fG,T=αf1G+βf2T,where α and β are arbitrary constants. Further, we choose f1(G) in power law form; that is,(17)f1G=Gm+1.This model has already been proposed by Cognola et al. [18] and it is interesting because the chances of the appearing of Big-Rip singularity vanish using this model. Subtraction of (14) and (15) yields(18)Y¨Y+n+1Y˙2Y2-42Y˙Y¨Y2+nY˙3Y3f˙G-4Y˙2Y2f¨G=0.Using (17) in (16), it follows that(19)fG=αm+1Gm.For simplicity and without loss of any generality, we chooseα=1/m+1 so that (18) takes the form(20)Y¨Y+n+1Y˙2Y2-4mGm2Y˙Y¨Y2+nY˙3Y3G˙G+Y˙2Y2m-1G˙2G2+G¨G=0.After inserting the value of GB invariant (20) reduces to differential equations with three unknowns Y, m, and n. It would be worthwhile to mention here that many solutions can be found using (20). Here we consider the power law form; that is,(21)Yt=γtk,where γ and k are arbitrary constants. Using this in (20), we obtain a constraint equation(22)t2+4mkn+2k-1+16mk8nk3kn+2k-3mkn+2k-4m-3=0.This equation is satisfied fork=1/n+2 such that(23)m2m+1=0.Thus, corresponding to two roots of this equation, we obtain two choices off1(G) models:(24)f1G=G+c1,f1G=2G+c2,where c1 and c2 are integration constants. The first model recovers the usual GB gravity for c1=0 and f2(T)=0. The second model with square root term is important as it leads to a viable inflation in the presence of massive scalar field [39]. It is mentioned that different forms of f2(T) can be assumed to reconstruct the solutions. However, we propose only two models for the present analysis.Case I (linearf2(T) model).
We consider linear form here for the sake of simplicity. Thus, consideringf2(T)=T and using (13)–(15), the expressions for energy density and pressure of universe turn out to be(25)ρ=1t4m+1n+23κ2κ2+1t2m+1κ2-12n2+5n+2-8-16nt4n+23m4m3n+2+m2n2+10n-6κ2n+12+mn2+7n-5κ2n+4-βf2T2κ2,p=1t4m+1n+23κ2t2m+12n2+5n+2+8-16nt4n+23m4m3n+2+m2n2+10n+12+mn2+7n+4+βf2T2κ2.It is evident from (25) that energy density and pressure of the universe are defined for -∞<n<-2 and -2<n<0 for m=-1/2. Adding (25), we obtain(26)ρ+p=2t22n2+5n+2+8-16nt4n+23m4m2n+2+mn2+12n+4t4n+23κ2+1.The behaviour of energy density plus pressure of universe can be seen from Figure1(a) for the model f(G,T)=G+T with κ=1. It is clear that ρ+p→0 as time grows which further suggests EoS parameter ω→-1. This is interesting as the phantom-like dark energy is found to be in the region where ω<-1. The universe with phantom dark energy ends up with a finite time future singularity known as cosmic doomsday or Big Rip [40, 41]. Moreover, accelerated expansion of universe is described when ω≈-1 [42–44]. Figure 1(b) depicts the behavior of ρ for radiation universe.Figure 1
(a) Behavior ofρ+p for m=-1/2 with κ=1. (b) Behavior of ρ for radiation universe.
(a)
(b)Case II (Starobinsky-likef2(T) model).
Here we proposef2(T)=T+ϵT2, where ϵ is an arbitrary constant. For this model, manipulation of (13)–(15) yields (27)ρ+p1+κ2+2ϵρ-6ϵp=2t4n+23t22n2+5n+2+8-16nt4n+23m2m2n2+3n+2+mn2+7n+2.Using EoS parameterp=ωρ, it follows that(28)2ϵ1-2ω-3ω2ρ2+1+κ21+ωρ-2t4n+23t22n2+5n+2+8-16nt4n+23m2m2n2+3n+2+mn2+7n+2=0.Using (28), we may analyze the behavior of universe by choosing different values of EoS parameter.(i)
ω=0 (dust fluid).In this case, the energy density of the universe turns out to be(29)ρ=-1+κ2±1+κ22+4l2ϵ,where(30)l=2t4n+23t22n2+5n+2+8-16nt4n+23m2m2n2+3n+2+mn2+7n+2.The graphical behavior of energy density for both the roots is shown in Figures2(a) and 2(b). The first root gives positive energy density but it approaches zero as t grows. However, the second root provides unrealistic behavior as energy density approaches -2 at later times.(ii)
ω=1/4 (subrelativistic fluid).Here the energy density of the universe turns out to be(31)ρ=-101+κ2±2251+κ22+20l5ϵ.In this case, the first root, Figure3(a), gives positive energy density having similar limiting value as in the dust case. However, the second root, Figure 3(b), gives negative energy density which corresponds to negative pressure universe. It is interesting because it is believed that dark energy has negative pressure causing accelerated expansion of universe.(iii)
ω=1/3 (radiation fluid).In this case, (28) becomes linear and the energy density of the universe turns out to be(32)ρ=3l41+κ2.The graphical behavior of energy density in this case is shown in Figure1(b).(iv)
ω=1/2 (ultrarelativistic fluid).Here the energy density of the universe turns out to be(33)ρ=31+κ2∓1+κ22-12l3ϵ.Here both the roots give positive energy density. However, the first root shows a decreasing behavior, Figure4(a), while the second root gives increasing trend as the time passes, Figure 4(b).(v)
ω=1 (stiff fluid).Here the energy density of the universe turns out to be(34)ρ=1+κ2∓1+κ22-4l4ϵ.The graphical behavior in this case is similar to that of ultrarelativistic fluid universe, Figures5(a) and 5(b).Figure 2
Behaviour ofρ for dust universe.
(a)
(b)Figure 3
Behaviour ofρ for subrelativistic universe.
(a)
(b)Figure 4
Behaviour ofρ for ultrarelativistic universe.
(a)
(b)Figure 5
Behaviour ofρ for stiff universe.
(a)
(b)Thus, the solution metric takes the form(35)ds2=dt2-γ2nt2n/n+2dx2-γ2t2/n+2dy2+dz2.Thus many physical solutions with different values of EoS parameter are possible. This is due to the fact that the presence of termT in the bivariate function f(G,T) may give many constraints which ultimately yield different solutions of the field equations and the theory may support the accelerated expansion of universe under certain conditions for the model under consideration.


### 3.1. Discussion of Some Important Cosmological Parameters

The Ricci scalar and GB invariant for the solution metric (35) take the form(36)R=22n+1n+22t2,G=-16nn+23t4.It is obvious that the singularities exist att=0 and n=-2. The average Hubble parameter, average scale factor, and volume scale factor of universe take the form(37)H=13t,a=γn+2/3t1/3,V=γn+2t.These parameters attain either zero value or tend to infinity at the points of singularity. In particular, the average scale factor is zero at the initial epocht=0 and hence the model has a point type singularity [45]. The redshift for a distant source is directly related to the scale factor of the universe at the time when the photons were emitted from the source. The scale factor a and redshift z are related through the equation(38)a=a01+z,where a0 is the present values of the scale factor. Using (37), we get(39)HH0=t0t,a0a=1+z=t0t1/3,where H0 represents the present values of Hubble’s parameter. We can write the value of Hubble’s parameter in terms of redshift parameter as(40)H=H01+z3.The deceleration, jerk, and snap parameters for the solution are given by(41)q=2,j=10,s=-80.The expansion scalar and shear scalar become(42)θ=1t,σ2=13n-1n+2t2.It is mentioned here that the isotropy conditionσ2/θ→0 as t→∞ is also satisfied in this case. It is also evident that σ2/θ→0 for small values of n even when t is not very large. This indicates that transition to isotropy is also possible for some suitable values of n and t (other than ∞). Thus, anisotropic universe isotropizes in general and FRW limit does exist with power law f(G,T) model under consideration. It can be seen from (37) and (42) that the volume of universe is zero at t=0 while the expansion scalar is infinite, which suggests that the universe started its evolution with zero volume at t=0, that is, big bang scenario.


## 3.1. Discussion of Some Important Cosmological Parameters

The Ricci scalar and GB invariant for the solution metric (35) take the form(36)R=22n+1n+22t2,G=-16nn+23t4.It is obvious that the singularities exist att=0 and n=-2. The average Hubble parameter, average scale factor, and volume scale factor of universe take the form(37)H=13t,a=γn+2/3t1/3,V=γn+2t.These parameters attain either zero value or tend to infinity at the points of singularity. In particular, the average scale factor is zero at the initial epocht=0 and hence the model has a point type singularity [45]. The redshift for a distant source is directly related to the scale factor of the universe at the time when the photons were emitted from the source. The scale factor a and redshift z are related through the equation(38)a=a01+z,where a0 is the present values of the scale factor. Using (37), we get(39)HH0=t0t,a0a=1+z=t0t1/3,where H0 represents the present values of Hubble’s parameter. We can write the value of Hubble’s parameter in terms of redshift parameter as(40)H=H01+z3.The deceleration, jerk, and snap parameters for the solution are given by(41)q=2,j=10,s=-80.The expansion scalar and shear scalar become(42)θ=1t,σ2=13n-1n+2t2.It is mentioned here that the isotropy conditionσ2/θ→0 as t→∞ is also satisfied in this case. It is also evident that σ2/θ→0 for small values of n even when t is not very large. This indicates that transition to isotropy is also possible for some suitable values of n and t (other than ∞). Thus, anisotropic universe isotropizes in general and FRW limit does exist with power law f(G,T) model under consideration. It can be seen from (37) and (42) that the volume of universe is zero at t=0 while the expansion scalar is infinite, which suggests that the universe started its evolution with zero volume at t=0, that is, big bang scenario.


## 4. Reconstruction of Some Important Cosmological Solutions

Here we discuss some special cases to reconstruct some important cosmological solutions.


### 4.1. Flat FRW Solution

For a special case whenn=1 and m=-1/2, space-time (35) takes the form(43)ds2=dt2-γ2t2/3dx2+dy2+dz2,which is the solution of well-known flat FRW metric. In this case ω attains an imaginary value which shows that the model f(G,T)=G+βf2(T) is not viable for flat FRW solution. However, when m=0, using (25), EoS parameter turns out to be(44)ω=1+κ22+3βf2Tt23βf2Tt21+κ2+21-κ2.One can further analyze using different possibilitiesf2(T) and hence in this case the reconstruction flat FRW solution is justified.


### 4.2. Kasner Type Solution

We can recover interesting Kasner type solution by puttingn=-1/2 in (35)(45)ds2=dt2-γ-1t-2/3dx2-γ2t4/3y2+dz2.It is similar to the well-known Kasner’s metric [46] and one can obtain the exact space-time after redefining the parameters. Here EoS parameter takes the form(46)ω=-1+κ264m27+6m1728/t4m+27βf2Tt4m+1729m64m6mκ2+5κ2+7m+6m21728/t4m+27βf2Tt4m+11+κ2729m.It is interesting to notice that, form=0, (46) gives ω=-1 independent of the choice of f2(T) model thus describing accelerated expansion of universe [42–44]. Moreover, when m=-1/2, EoS parameter turns out to be(47)ω=1+κ2163+9βf2Tt4163κ2-1-9βf2Tt41+κ2.Hence our both values ofm incorporate Kasner type solution.


### 4.3. Exponential Law Solutions

It is to be noticed that (20) has an exponential solution of the form(48)Yt=ec3t+c4,with the constraint equation(49)n+2=0,where c3 and c4 are arbitrary constants. Here EoS parameter becomes(50)ω=-1+κ2βf2T-66κ2-1+βf2T1+κ2,which is independent of parameter m and hence any viable power law f1(G) gravity model can be used with an appropriate f2(T) model. The solution metric in this case turns out to be(51)ds2=dt2-e-4c3t+c4dx2-e2c3t+c4dy2+dz2.The average Hubble parameter is zero for this solution. All other dynamical parameters expansion scalarθ, shear scalar σ, and volume scale factor of universe are constant here.


## 4.1. Flat FRW Solution

For a special case whenn=1 and m=-1/2, space-time (35) takes the form(43)ds2=dt2-γ2t2/3dx2+dy2+dz2,which is the solution of well-known flat FRW metric. In this case ω attains an imaginary value which shows that the model f(G,T)=G+βf2(T) is not viable for flat FRW solution. However, when m=0, using (25), EoS parameter turns out to be(44)ω=1+κ22+3βf2Tt23βf2Tt21+κ2+21-κ2.One can further analyze using different possibilitiesf2(T) and hence in this case the reconstruction flat FRW solution is justified.


## 4.2. Kasner Type Solution

We can recover interesting Kasner type solution by puttingn=-1/2 in (35)(45)ds2=dt2-γ-1t-2/3dx2-γ2t4/3y2+dz2.It is similar to the well-known Kasner’s metric [46] and one can obtain the exact space-time after redefining the parameters. Here EoS parameter takes the form(46)ω=-1+κ264m27+6m1728/t4m+27βf2Tt4m+1729m64m6mκ2+5κ2+7m+6m21728/t4m+27βf2Tt4m+11+κ2729m.It is interesting to notice that, form=0, (46) gives ω=-1 independent of the choice of f2(T) model thus describing accelerated expansion of universe [42–44]. Moreover, when m=-1/2, EoS parameter turns out to be(47)ω=1+κ2163+9βf2Tt4163κ2-1-9βf2Tt41+κ2.Hence our both values ofm incorporate Kasner type solution.


## 4.3. Exponential Law Solutions

It is to be noticed that (20) has an exponential solution of the form(48)Yt=ec3t+c4,with the constraint equation(49)n+2=0,where c3 and c4 are arbitrary constants. Here EoS parameter becomes(50)ω=-1+κ2βf2T-66κ2-1+βf2T1+κ2,which is independent of parameter m and hence any viable power law f1(G) gravity model can be used with an appropriate f2(T) model. The solution metric in this case turns out to be(51)ds2=dt2-e-4c3t+c4dx2-e2c3t+c4dy2+dz2.The average Hubble parameter is zero for this solution. All other dynamical parameters expansion scalarθ, shear scalar σ, and volume scale factor of universe are constant here.


## 5. Final Remarks

The main purpose of this work is to investigate newly introduced modified GB theory, namely,f(G,T) gravity. For this purpose, anisotropic background is chosen. LRS Bianchi type I space-time is the simplest model and has been used frequently in different contexts. To our knowledge, this is the first attempt to investigate the exact solutions of f(G,T) gravity for LRS Bianchi type I space-time. Moreover, we have not used any conventional assumption like constant deceleration parameter to investigate the exact solutions. It is mentioned here that the field equations are highly nonlinear and it is due to the inclusion of bivariate function in the standard action. So we assume that the shear scalar σ is proportional to the expansion scalar θ which gives X=Yn, where X, Y are the metric coefficients and n is an arbitrary constant. We consider the model f(G,T)=αf1(G)+βf2(T), where α and β are arbitrary constants. Moreover, we have used a power law form f1(G) gravity model already available in literature [18]. The interesting feature of this model is that the chances of the appearing of Big-Rip singularity are minimized. Further, the viability of this model has already been discussed in different cosmological contexts [47–49]. We have also proposed a Starobinsky-like f2(T) model; that is, f2(T)=T+ϵT2, where ϵ is an arbitrary constant. The interesting aspect of the Starobinsky-like f2(T) model is that it provides many exact solutions and one can choose the best fit solutions according to the requirements.Using the modified field equations, we have formulated a general differential equation (20) which can further be used to investigate exact solutions. Mainly we used power law and exponential forms of metric coefficients to explore the exact solutions of modified field equations. It is shown that two f1(G) gravity models are associated with the power law solution. The first model recovers the usual GB gravity for c1=0 and f2(T)=0. However, the second model with square root term looks important as it leads to a viable inflation in the presence of massive scalar field [39]. It is mentioned here that different forms of f2(T) can be assumed to reconstruct the solutions. However, we have discussed only two models for the present analysis. Firstly, we choose linear f2(T) gravity model. The expressions for energy density and pressure of universe are defined for anisotropy parameters -∞<n<-2 and -2<n<0 with m=-1/2. The graphical behavior (see Figure 1(a)) shows that ρ+p→0 as time grows which implies that EoS parameter ω→-1. This is interesting as the phantom-like dark energy is found to be in the region where ω<-1. The universe with phantom dark energy ends up with a finite time future singularity known as cosmic doomsday or Big Rip [40, 41]. Moreover, accelerated expansion of universe with de Sitter type evolution is described when ω≈-1 [42–44]. However, the second model proposed as Starobinsky-like model involves squared term of T. This gives a quadratic equation in ρ and we have analyzed the behavior of universe by choosing different values of EoS parameter. In particular, analysis is given for ω=0 (dust fluid), ω=1/4 (subrelativistic fluid), ω=1/3 (radiation fluid), ω=1/2 (ultrarelativistic fluid), and ω=1 (stiff fluid). The graphical behavior of energy density for cases is discussed. In particular, in case of subrelativistic fluid, one root corresponds to negative pressure universe. It is interesting because it is believed that dark energy has negative pressure causing accelerated expansion of universe. Thus, it is concluded that presence of term T in the bivariate function f(G,T) may give many solutions of the field equations and the theory supports the accelerated expansion of universe under certain conditions for the model under consideration.Lastly, we have reconstructed some important cosmological solutions. The first solution corresponds to flat FRW space-time. This solution is valid forω=1 describing the stiff fluid universe for the first model. However, the solution is not physical for the second model as ω is imaginary. The second solution provides the well-known Kasner universe and it gives the value of anisotropy parameter n=-1/2. The third solution is obtained by exponential law assumption. It gives the average Hubble parameter zero and all other dynamical parameters like expansion scalar θ, shear scalar σ, and volume scale factor of universe constant. EoS parameter is independent of the parameter m for this solution and we get an explicit expression for ω involving f2(T). Thus any power law f1(G) gravity model may be used with an appropriate f2(T) model to reconstruct some important cosmological solutions.



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