# Dynamics of an Anisotropic Universe inf(R,T) Theory

Authors: B. Mishra; Sankarsan Tarai; S. K. Tripathy
Journal: Advances in High Energy Physics
 (2016)

---

## Abstract

Dynamics of an anisotropic universe is studied inf(R,T) gravity using a rescaled functional f(R,T), where R is the Ricci Scalar and T is the trace of energy-momentum tensor. Three models have been constructed assuming a power law expansion of the universe. Physical features of the models are discussed. The model parameters are constrained from a dimensional analysis. It is found from the work that the anisotropic Bianchi type VIh (BVIh) model in the modified gravity generally favours a quintessence phase when the parameter h is either -1 or 0. We may not get viable models in conformity with the present day observation for h=1.


---

## Body

## 1. Introduction

In the past decade the idea of modifying gravity on cosmological scale has attracted a lot of attention. It gains momentum through the theoretical developments involving higher dimensional theories and in constructing renormalizable theories of gravity. Modified gravity represents an intriguing possibility for resolving the theoretical challenge posed by late time acceleration. However, it turns out to be extremely difficult to modify general relativity at low energy regime without violating observational constraints.Observations from type Ia supernova [1–3], large scale structures [4–6], and cosmic microwave background [7, 8] confirm that the cosmic expansion is accelerating. The very cause behind this acceleration may be a mysterious energy source called dark energy which accounts for two-thirds of the total energy budget of the universe.The role of modified theories to understand the mechanism behind the cosmic speed-up is more promising. The objective behind such theories is to explain the puzzling late time cosmic dynamics without the need of dark energy components in the field equations. Several modified theories of gravity have been proposed in recent times. Of these a few models such asf(R) gravity [9–11], f(T) gravity [12–16], and f(G) gravity [17–19] are studied widely. In f(R) theory, a more general function of the Ricci Scalar R=gμνRμν is used in place of R whereas f(T) gravity is a generalized version of teleparallel gravity. Motivated by the success of cosmological constant as a simple and good candidate of dark energy, some matter field is also coupled with the function of R in the geometry side of the action in some modified theories of gravity (f(R,Lm) theory).Along the line of interest of incorporating some matter components in the action geometry,f(R,T) theory has been proposed by Harko et al. [20] which, of late, has been an interesting framework to investigate accelerating models. Moreover, the reconstruction of arbitrary FRW cosmologies is possible by an appropriate choice of the functional f(R,T). Many authors have investigated the astrophysical and cosmological implications of the f(R,T) gravity [21–24]. Jamil et al. [25] have reconstructed some cosmological models for some specific forms of f(R,T) in this modified gravity. Shamir et al. [26] obtained exact solution of anisotropic Bianchi type I and type V cosmological models whereas Chaubey and Shukla [27] have obtained a new class of Bianchi cosmological models using special law of variation of parameter. Using a decoupled form of f(R,T), that is, f(R,T)=f(R)+f(T) for Bianchi type V universe, Ahmed and Pradhan [28] have studied the energy conditions of perfect fluid cosmological models and Yadav [29] obtained some string solutions.Singh and Kumar [30] have investigated the effect of bulk viscosity in f(R,T) theory and suggested that inclusion of dissipative energy sources like bulk viscosity may be able to explain the early and late time accelerations of the universe. Mishra and Sahoo [31] have studied Bianchi type VIh cosmological models assuming f(R,T)=R+2f(T). In that work, Mishra and Sahoo have obtained exact solutions to the modified field equations by assuming a specific anisotropic relation among the metric potential. The models constructed in [31] are obtained to be accelerating for the model parameter h=1. Samanta [32] has obtained exact solution of f(R,T) gravitational field equations in Kantowski-Sachs space time and Shamir [33] has constructed some cosmological models in Bianchi type V space time. In the framework of this modified gravity, recently, Mishra et al. [34] have presented the Einstein-Rosen nonstatic cosmological model with quadratic form of f(R,T) gravity. Sahoo et al. [35] have investigated the background cosmology of power law and exponential law of volumetric expansion in f(R,T) gravity in Kaluza-Klein model. Recently Yousaf et al. have investigated the irregularity energy density factor in f(R,T) theory responsible to disturb the stability of homogeneous universe [36] and also explored the evolutionary behaviour of compact objects [37].In this work, we have constructed some cosmological models inf(R,T) theory for general Bianchi type VIh (BVIh) universe. The present work differs from the work of Mishra and Sahoo [31] in the sense that here we have used a rescaled functional f(R,T) instead of the one used in [31]. We have reconstructed some viable accelerating models in conformity with the recent observations from some physical basis. Our work is organised as follows. In Section 2, the basic formalism of the f(R,T) theory has been presented. The dynamics of anisotropic VIh model has been presented in a general form. In Section 3, some specific models have been constructed to study the dynamics. We presented the conclusions of the works at the end in Section 4.


## 2. Basic Formalism

The modified four-dimensional Einstein-Hilbert action inf(R,T) gravity theory with a specific choice of matter Lagrangian can be considered as(1)S=116π∫fR,T-gd4x+∫Lm-gd4x.Here, f(R,T) is an arbitrary function of R and T. Following the work of Harko et al. [20], we have considered the matter Lagrangian as Lm=-p, where p is the pressure of the perfect cosmic fluid. The trace T=gijTij of the energy-momentum tensor is obtained from Tij=(ρ+p)uiuj-pgij. ρ is the rest energy density and ui=δ0i is the four velocity vectors.The field equations can be obtained from the action in (1) for the choice of the functional f(R,T)=f(R)+f(T) as [20](2)fRRij-12fRgij+gij□-∇i∇jfRR=8πTij+fTTTij+pfTT+12fTgij.fR=∂f(R)/∂R and fT=∂f(T)/∂T are the partial differentiation of the respective functional with respect to their arguments. The functional f(R,T) can be chosen arbitrarily to get viable cosmological models. Here we chose the functional f(R) and f(T) to be linear in their arguments, f(R)=λR and f(T)=λT, so that f(R,T)=λ(R+T). λ is a constant scaling factor.Equation (2) now reduces to(3)Rij-12Rgij=8π+λλTij+ΛTgij.Equation (3) can now be recast as the usual Einstein Field Equation where Λ(T)=p+1/2T can be identified with the cosmological constant that evolves with cosmic time. The role of the particular choice of the functional f(R,T)=λ(R+T) can be well understood in getting such a simplified approach to a modified theory which does not contain any dark sector component but can be instrumental in providing viable accelerating models.For a spatially homogeneous and anisotropic Bianchi typeVIh (BVIh) space time considered in the form(4)ds2=dt2-A2dx2-B2e2xdy2-C2e2hxdz2,(3) can be explicitly written as(5)B¨B+C¨C+B˙C˙BC-hA2=16π+3λ2λp-ρ2,A¨A+C¨C+A˙C˙AC-h2A2=16π+3λ2λp-ρ2,A¨A+B¨B+A˙B˙AB-1A2=16π+3λ2λp-ρ2,-A˙B˙AB-B˙C˙BC-C˙A˙CA+1+h+h2A2=16π+3λ2λρ-p2,B˙B+hC˙C-1+hA˙A=0,where the metric potentials A, B, and C are functions of cosmic time t. The constant exponent h decides the behaviour of the model and can take integral values such as -1,0, and 1. An overdot on a field variable denotes differentiation with respect to time t. We define the directional Hubble parameters along different directions as Hx=A˙/A, Hy=B˙/B, and Hz=C˙/C. The mean Hubble parameter becomes H=1/3(Hx+Hy+Hz). The field equations (5) can now be expressed as(6)H˙y+H˙z+Hy2+Hz2+HyHz-hA2=αp-ρ2,(7)H˙x+H˙z+Hx2+Hz2+HxHz-h2A2=αp-ρ2,(8)H˙x+H˙y+Hx2+Hy2+HxHy-1A2=αp-ρ2,(9)-HxHy-HyHz-HzHx+1+h+h2A2=αρ-p2,(10)Hy+hHz-1+hHx=0,where α=16π+3λ/2λ.The pressurep and rest energy density ρ can be obtained from (8) and (9) in general forms as(11)p=24α2-12αχHx,Hy-ξHx,Hy,Hz,h,(12)ρ=24α2-1χHx,Hy-2αξHx,Hy,Hz,h,where χHx,Hy=H˙x+H˙y+Hx2+Hy2+HxHy-1/A2 and ξ(Hx,Hy,Hz,h)=HxHy+HyHz+HzHx-1+h+h2/A2.From (11) and (12), we obtain the equation of state parameter ω=p/ρ and the effective cosmological constant Λ as(13)ω=2α+4α2-1ξHx,Hy,Hz,hχHx,Hy-2αξHx,Hy,Hz,h,Λ=-χHx,Hy+ξHx,Hy,Hz,h2α+1.Equations (11)–(13) provide the dynamical behaviour of the universe. However, the dynamics can only be assessed if the behaviour of these properties is known in terms of the directional Hubble rates for a given value of the exponent h. In other words, the formalism as described above can help us to study a background cosmology for an assumed dynamics of the universe. In this context, we can consider the power law cosmology, where the cosmic expansion is governed through a volume scale factor of the form v=tm. m is an arbitrary positive constant usually determined from the background cosmology. Power law cosmology has been widely studied in recent times because of its functional simplicity and ability to provide a first-hand information about the dynamics of the universe. For such an assumption, the radius scale factor can be a=(ABC)1/3=tm/3. The deceleration parameter for power law expansion of the universe is a constant quantity: q=-1+3/m, which can be negative for m>3 and positive for m<3. It is worth mentioning here that a positive q describes a decelerating universe whereas a negative q describes an accelerating universe. In order to keep a pace with the recent observational data favouring an accelerating universe, m should be greater than 3.Some other kinematical parameters of the universe are the scalar expansionθ, shear scalar σ2, and the average anisotropy parameter A defined, respectively, as(14)θ=ΣHi,σ2=12σijσij=12ΣHi2-13θ2,A=13ΣΔHiH2,where ΔHi=Hi-H with i=x,y,z. A is a measure of deviation from isotropic expansion. One can get the isotropic behaviour of the model for A=0. For the power law cosmology with v=tm, the scalar expansion becomes θ=m/t and consequently the mean Hubble rate becomes H=m/3t.Geometrical analysis of dark energy models is usually performed through the statefinder pairj and s given by j=a⃛/aH3 and s=j-1/3(q-1/2). In the present model, we obtain these parameters as j=9/m2/m-1+1 and s=2/m. These parameters are constants of cosmic time and depend only on the exponent m. It can be emphasized here that exact determination of these parameters from different observational bounds can constrain the exponent m in narrow ranges.


## 3. Dynamics of AnisotropicBVIh Universe

Once the cosmic expansion behaviour is known, it becomes simpler to study the background cosmology of the diagonalBVIh universe. However, the exponent h in the metric can assume integral values such as -1, 0, and 1. Each value of h corresponds to a different cosmological model with different dynamical behaviour. In view of this, in the following, we discuss the dynamical features of the three possible models in the framework of fR,T theory.


### 3.1. Model-Ih=-1

A substitution ofh=-1 in (10) yields Hy=Hz, where the integration constant has been rescaled to unity. Assuming an anisotropic relationship Hx=kHy, we can write the functionals χ(Hx,Hy) and ξ(Hx,Hy,Hz,h) as(15)χ=k+1H˙y+k2+k+1Hy2-1A2,ξ=2k+1Hy2-1A2,where k is an arbitrary positive constant. For a power law cosmology, we have Hx=km/k+21/t, Hy=Hz=m/k+21/t. Consequently the directional scale factors are A=tkm/k+2 and B=C=tm/k+2. Thus we can have(16)χ=m2k2+k+1-mk+1k+2k+221t2-1t2mk/k+2,ξ=2k+1m2k+221t2-1t2mk/k+2.The dynamical behaviour of the model is decided from the behaviour of the equation of state parameter ω and the effective cosmological constant Λ. However, these two parameters depend on the time varying nature of functionals χ(t) and ξ(t) which in turn depend on the parameters m and k. If mk>k+2, the terms within the square brackets in (16) dominate at late times of cosmic evolution whereas the terms containing t-2mk/k+2 dominate at early phase of cosmic evolution. Here we wish to adopt a dimensional analysis to get some idea into the general behaviour of these functionals. Since m and k are two dimensionless constants, it appears that the dimensionality of the time dependent factors for a given functional should remain the same. In other words, we can have m=1+2/k so that χ(t) and ξ(t) become(17)χt=1-k2k21t2,ξt=1+2k-k2k21t2.The equation of state parameter and the effective time varying cosmological constant are obtained from (13) as(18)ω=2α+4α2-11+2k-k21-2α1-k2+4αk,Λt=22α+1k2-k-1k21t2.It is obvious from the above expressions that the equation of state parameterω is a constant quantity for a given value of scaling constant λ and the anisotropic parameter k. However, the effective cosmological constant decreases quadratically with cosmic time. In order to get viable cosmological models in conformity with recent observations, the cosmological constant should be dynamically varying from large positive values at an initial epoch to vanishingly null values at late times of cosmic evolution. Similarly, the equation of state parameter should be negative with values less than -1/3 at late times. This behaviour will enable us to constrain the parameter k. In Figure 1, we have shown the variation of ω as a function of k. Here we chose a negative value of the scaling constant λ; that is, λ=-8π/8π+1. Accordingly the model parameter α is decided from the relation α=16π+3λ/2λ. The reason behind this particular choice is to look at the present problem from the backdrop of general relativity where the modified gravity field equation (3) appears as the Einstein Field Equation with a time varying effective cosmological constant Λ. It can be inferred from the figure that the equation of state parameter ω increases almost linearly from a negative value for lower k to zero at higher k. One can note that the present model will collapse at k=1 and therefore we restrict the values of k below 1. For k≤0.64, ω remains in the quintessence region. One can note that the results may be sensitive to the choice of the parameter α. In Figure 2, we have shown the dynamical variation of the effective cosmological constant for some representative values of k. As is required for an explanation to the late time cosmic acceleration, Λ varies from large positive values in the beginning to vanishingly small values at late times. In Figure 2(a), the evolution of Λ is shown as a function of cosmic time where as in Figure 2(b) its evolution is shown as function of redshift z=1/a-1 with the scale factor at present epoch being unity. As it appears from the figure, the evolutionary behaviour of Λ is affected by the choice of the values of k. At remote past, curves of Λ with low values of k remain below the curves with higher values of k. However, at certain point of cosmic time corresponding to a redshift of z=6.2, there occurs a reversal of the behaviour; that is, curves of Λ with higher values of k remain below the curves with lower values of k. The choice of the model parameter α does not affect the general time varying trend of the effective cosmological constant.Figure 1
Variation of the equation of state parameterω with the parameter k for h=-1.Figure 2
Evolution of the effective cosmological constant for three representative values ofk in the model h=-1. (a) Λ is shown as a function of time. (b) Evolution of Λ shown as a function of redshift.
(a) (b)


### 3.2. Model-IIh=0

In the present case withh=0, (10) reduces to Hx=Hy. An anisotropic relation Hz=nHy among the respective directional Hubble rates in the power law expansion of volume scale factor yields Hx=Hy=m/n+21/t and Hz=mn/n+21/t. The directional scale factors become A=B=tm/n+2 and C=tmn/n+2. Here n is a constant parameter. If n=1, the model reduces to be isotropic.The functionalsχ(t) and ξ(t) for this model are obtained as(19)χt=3m2-2mn+2n+221t2-1t2m/n+2,ξt=2n+1m2n+221t2-1t2m/n+2.The dimensional consistency of terms involved in the expressions ofχ(t) and ξ(t) constrains the exponent m to be m=n+2. With this constraint, the equation of state parameter and the effective cosmological constant become(20)ω=12α,(21)Λt=-2n2α+1t2.As in the previous model, the equation of state parameter in the present model is also a constant quantity that depends on the scaling constantλ through α. In the present work, we chose λ to assume a negative value so that α becomes negative. This puts ω in the negative domain. It is interesting to note here that the equation of state parameter is, in general, not affected by the choice of anisotropy in the model. In Figure 3, we have plotted ω as a function of α in its negative domain. It is clear that ω lies in the quintessence region (shaded portion in the plot) for the range -1.5≤α≤-0.5. For α>-0.5, the equation of state parameter enters into the phantom region. It is certain from (21) that the effective cosmological constant can be positive for α<-0.5. In other words, an accelerated expansion with positive cosmological constant in this model favours a quintessence phase. The time evolution of the effective cosmological constant is shown for different values of the anisotropic parameter n in Figure 4. Here, the parameter α is chosen to be -1. A change in this value within the quintessence bound will result in a change in Λ without changing its general behaviour. Within the quintessence bound, higher value of α will yield higher Λ. The values of n in Figure 4 are chosen so as to get negative deceleration parameter. In order to satisfy this condition, n has to be constrained in the range n>1. It is clear from the figure that Λ decreases from large positive values to small positive values during the cosmic evolution and vanishes at late times. One interesting thing in the present model is that even if the model favours a quintessence phase, the decrement in Λ is bit slower than that of the previous model with h=-1. As in the previous model, the behaviour of Λ is affected by the choice of the anisotropic parameter n. In order to assess the behaviour of the anisotropy dependence of Λ, we have shown its variation as a function of redshift z in Figure 4(b). In the remote past, the curves of Λ with higher values of n remain below the curves with lower values of n. However, there occurs a reversal in this behaviour at a redshift z=2.9.Figure 3
Variation of the equation of state parameterω with the parameter α for h=0. The shaded portion denotes the quintessence region.Figure 4
Evolution of the effective cosmological constant for three representative values ofk in the model h=0. (a) Λ is shown as a function of time. (b) Evolution of Λ shown as a function of redshift. Here we have considered a representative value α=-1 so as to get positive values of the effective cosmological constant. See text for details.
(a) (b)


### 3.3. Model-IIIh=1

In this model withh=1, we obtain from (6) and (7)(22)H˙x-H˙yHx-Hy+θ=0,which can be integrated for the power law cosmology to get(23)Hx=Hy+ϵtm.Here the integration constant ϵ is related to the present day value of the directional Hubble parameters as ϵ=Hx0-Hy0.Equation (10) becomes 2Hx=Hy+Hz which implies Hx=H and consequently(24)Hy=H-ϵtm,Hz=H+ϵtm.One can note that since the dimension of H is that of t-1, ϵ has a dimension of tm-1.The functionalsχ(t) and ξ(t) are obtained as(25)χt=2H˙+3H2+ϵ2t2m-1t2m/3,ξt=3H2-ϵ2t2m-3t2m/3.From dimensional consistency, the parameterm can be constrained as m=3. In order to get accelerating models, the deceleration parameter q should be negative which requires that m should be greater than 3. However, the dimensional analysis yields q=0 for the present model. Also, interestingly the equation of state parameter and the effective cosmological constant are obtained to be ω=1 and Λ=0. Even though a vanishing cosmological constant is acceptable, ω=1 may not be acceptable in the context of dark energy driven cosmic acceleration. In view of this, the BVI1 model may not be in conformity with the present day observations.


## 3.1. Model-Ih=-1

A substitution ofh=-1 in (10) yields Hy=Hz, where the integration constant has been rescaled to unity. Assuming an anisotropic relationship Hx=kHy, we can write the functionals χ(Hx,Hy) and ξ(Hx,Hy,Hz,h) as(15)χ=k+1H˙y+k2+k+1Hy2-1A2,ξ=2k+1Hy2-1A2,where k is an arbitrary positive constant. For a power law cosmology, we have Hx=km/k+21/t, Hy=Hz=m/k+21/t. Consequently the directional scale factors are A=tkm/k+2 and B=C=tm/k+2. Thus we can have(16)χ=m2k2+k+1-mk+1k+2k+221t2-1t2mk/k+2,ξ=2k+1m2k+221t2-1t2mk/k+2.The dynamical behaviour of the model is decided from the behaviour of the equation of state parameter ω and the effective cosmological constant Λ. However, these two parameters depend on the time varying nature of functionals χ(t) and ξ(t) which in turn depend on the parameters m and k. If mk>k+2, the terms within the square brackets in (16) dominate at late times of cosmic evolution whereas the terms containing t-2mk/k+2 dominate at early phase of cosmic evolution. Here we wish to adopt a dimensional analysis to get some idea into the general behaviour of these functionals. Since m and k are two dimensionless constants, it appears that the dimensionality of the time dependent factors for a given functional should remain the same. In other words, we can have m=1+2/k so that χ(t) and ξ(t) become(17)χt=1-k2k21t2,ξt=1+2k-k2k21t2.The equation of state parameter and the effective time varying cosmological constant are obtained from (13) as(18)ω=2α+4α2-11+2k-k21-2α1-k2+4αk,Λt=22α+1k2-k-1k21t2.It is obvious from the above expressions that the equation of state parameterω is a constant quantity for a given value of scaling constant λ and the anisotropic parameter k. However, the effective cosmological constant decreases quadratically with cosmic time. In order to get viable cosmological models in conformity with recent observations, the cosmological constant should be dynamically varying from large positive values at an initial epoch to vanishingly null values at late times of cosmic evolution. Similarly, the equation of state parameter should be negative with values less than -1/3 at late times. This behaviour will enable us to constrain the parameter k. In Figure 1, we have shown the variation of ω as a function of k. Here we chose a negative value of the scaling constant λ; that is, λ=-8π/8π+1. Accordingly the model parameter α is decided from the relation α=16π+3λ/2λ. The reason behind this particular choice is to look at the present problem from the backdrop of general relativity where the modified gravity field equation (3) appears as the Einstein Field Equation with a time varying effective cosmological constant Λ. It can be inferred from the figure that the equation of state parameter ω increases almost linearly from a negative value for lower k to zero at higher k. One can note that the present model will collapse at k=1 and therefore we restrict the values of k below 1. For k≤0.64, ω remains in the quintessence region. One can note that the results may be sensitive to the choice of the parameter α. In Figure 2, we have shown the dynamical variation of the effective cosmological constant for some representative values of k. As is required for an explanation to the late time cosmic acceleration, Λ varies from large positive values in the beginning to vanishingly small values at late times. In Figure 2(a), the evolution of Λ is shown as a function of cosmic time where as in Figure 2(b) its evolution is shown as function of redshift z=1/a-1 with the scale factor at present epoch being unity. As it appears from the figure, the evolutionary behaviour of Λ is affected by the choice of the values of k. At remote past, curves of Λ with low values of k remain below the curves with higher values of k. However, at certain point of cosmic time corresponding to a redshift of z=6.2, there occurs a reversal of the behaviour; that is, curves of Λ with higher values of k remain below the curves with lower values of k. The choice of the model parameter α does not affect the general time varying trend of the effective cosmological constant.Figure 1
Variation of the equation of state parameterω with the parameter k for h=-1.Figure 2
Evolution of the effective cosmological constant for three representative values ofk in the model h=-1. (a) Λ is shown as a function of time. (b) Evolution of Λ shown as a function of redshift.
(a) (b)


## 3.2. Model-IIh=0

In the present case withh=0, (10) reduces to Hx=Hy. An anisotropic relation Hz=nHy among the respective directional Hubble rates in the power law expansion of volume scale factor yields Hx=Hy=m/n+21/t and Hz=mn/n+21/t. The directional scale factors become A=B=tm/n+2 and C=tmn/n+2. Here n is a constant parameter. If n=1, the model reduces to be isotropic.The functionalsχ(t) and ξ(t) for this model are obtained as(19)χt=3m2-2mn+2n+221t2-1t2m/n+2,ξt=2n+1m2n+221t2-1t2m/n+2.The dimensional consistency of terms involved in the expressions ofχ(t) and ξ(t) constrains the exponent m to be m=n+2. With this constraint, the equation of state parameter and the effective cosmological constant become(20)ω=12α,(21)Λt=-2n2α+1t2.As in the previous model, the equation of state parameter in the present model is also a constant quantity that depends on the scaling constantλ through α. In the present work, we chose λ to assume a negative value so that α becomes negative. This puts ω in the negative domain. It is interesting to note here that the equation of state parameter is, in general, not affected by the choice of anisotropy in the model. In Figure 3, we have plotted ω as a function of α in its negative domain. It is clear that ω lies in the quintessence region (shaded portion in the plot) for the range -1.5≤α≤-0.5. For α>-0.5, the equation of state parameter enters into the phantom region. It is certain from (21) that the effective cosmological constant can be positive for α<-0.5. In other words, an accelerated expansion with positive cosmological constant in this model favours a quintessence phase. The time evolution of the effective cosmological constant is shown for different values of the anisotropic parameter n in Figure 4. Here, the parameter α is chosen to be -1. A change in this value within the quintessence bound will result in a change in Λ without changing its general behaviour. Within the quintessence bound, higher value of α will yield higher Λ. The values of n in Figure 4 are chosen so as to get negative deceleration parameter. In order to satisfy this condition, n has to be constrained in the range n>1. It is clear from the figure that Λ decreases from large positive values to small positive values during the cosmic evolution and vanishes at late times. One interesting thing in the present model is that even if the model favours a quintessence phase, the decrement in Λ is bit slower than that of the previous model with h=-1. As in the previous model, the behaviour of Λ is affected by the choice of the anisotropic parameter n. In order to assess the behaviour of the anisotropy dependence of Λ, we have shown its variation as a function of redshift z in Figure 4(b). In the remote past, the curves of Λ with higher values of n remain below the curves with lower values of n. However, there occurs a reversal in this behaviour at a redshift z=2.9.Figure 3
Variation of the equation of state parameterω with the parameter α for h=0. The shaded portion denotes the quintessence region.Figure 4
Evolution of the effective cosmological constant for three representative values ofk in the model h=0. (a) Λ is shown as a function of time. (b) Evolution of Λ shown as a function of redshift. Here we have considered a representative value α=-1 so as to get positive values of the effective cosmological constant. See text for details.
(a) (b)


## 3.3. Model-IIIh=1

In this model withh=1, we obtain from (6) and (7)(22)H˙x-H˙yHx-Hy+θ=0,which can be integrated for the power law cosmology to get(23)Hx=Hy+ϵtm.Here the integration constant ϵ is related to the present day value of the directional Hubble parameters as ϵ=Hx0-Hy0.Equation (10) becomes 2Hx=Hy+Hz which implies Hx=H and consequently(24)Hy=H-ϵtm,Hz=H+ϵtm.One can note that since the dimension of H is that of t-1, ϵ has a dimension of tm-1.The functionalsχ(t) and ξ(t) are obtained as(25)χt=2H˙+3H2+ϵ2t2m-1t2m/3,ξt=3H2-ϵ2t2m-3t2m/3.From dimensional consistency, the parameterm can be constrained as m=3. In order to get accelerating models, the deceleration parameter q should be negative which requires that m should be greater than 3. However, the dimensional analysis yields q=0 for the present model. Also, interestingly the equation of state parameter and the effective cosmological constant are obtained to be ω=1 and Λ=0. Even though a vanishing cosmological constant is acceptable, ω=1 may not be acceptable in the context of dark energy driven cosmic acceleration. In view of this, the BVI1 model may not be in conformity with the present day observations.


## 4. Conclusion

In view of the recent interest in modified theories of gravity, we have studied the dynamics of some Bianchi typeVIh models in f(R,T) theory. We choose fR,T=fR+fT, where fR=λR and fT=λT. These linear functions fR and fT rescale the modified gravity theory and generate the concept of a time varying effective cosmological constant. We have investigated three different models corresponding to three values of the metric parameter h, that is, -1, 0, and 1. The dynamics of the models are studied for a presumed power law expansion of the volume scale factor. We have adopted dimensional analysis method to constrain some of the model parameters. In the anisotropic models with h=-1 and h=0, the effective cosmological constant is found to evolve from large positive values at the beginning to small values at late times. This result is in accordance with the observations concerning the dark energy driven cosmic acceleration. The equation of state parameter for these two models becomes negative. With suitable choice of the model parameters both the models (h=-1 and h=0) favour the quintessence phase. However, for the third model with h=1, viable cosmological models could not be obtained. Anisotropy, in general, affects the dynamics of the universe. Of course, in the second model with h=0, the present analysis shows that the effective equation of state parameter is not affected by the anisotropy rather it depends on the scaling factor λ.



---

*Source: 8543560-2016-09-14.xml*