Noether symmetry approach in \(f(\mathcal {G},T)\) gravity

Open Access
Regular Article - Theoretical Physics

Abstract

We explore the recently introduced modified Gauss–Bonnet gravity (Sharif and Ikram in Eur Phys J C 76:640, 2016), \(f(\mathcal {G},T)\) pragmatic with \(\mathcal {G}\), the Gauss–Bonnet term, and T, the trace of the energy-momentum tensor. Noether symmetry approach has been used to develop some cosmologically viable \(f(\mathcal {G},T)\) gravity models. The Noether equations of modified gravity are reported for flat FRW universe. Two specific models have been studied to determine the conserved quantities and exact solutions. In particular, the well known deSitter solution is reconstructed for some specific choice of \(f(\mathcal {G},T)\) gravity model.

Keywords

Dark Energy Gravity Model Cosmological Solution Bonnet Term Stringy Charged Black Hole 

1 Introduction

The cosmological aspect of research has proven to be the main resource of modern diverse theories of gravity. No doubt, the onset of General relativity (GR) being a physical theory has been a great success of the last century. However GR alone does not provide us with the sufficient fundamental platform to solve the problems like initial singularity, flatness issues, dark energy and dark matter problems. It also fails when one is interested to express this wide universe as a whole, particularly at the extreme conditions for the ultraviolet scales and for the expression of the quantum structure of space-time. Few years back, the significant outcomes of the researchers have confirmed that the universe is expanding itself [2, 3, 4, 5, 6, 7, 8, 9]. A gigantic portion of this accelerating universe consists of mysterious substance, known as the dark energy and is believed to be the main cause of the acceleration of this expansion. Recent developments in cosmology have revealed new ideas to introduce the critical and observational innovations for this accelerated expanding universe.

Modified theories of gravity have provided the researchers with different aspects and directions to unveil the hidden realities behind the expansion of the universe. After being motivated and having started with the original theory, a number of theories have been structured by building intricate Lagrangians. For example, theories of gravity like f(R), f(RT), \(f(\mathcal {G})\) and \(f(R,\mathcal {G})\) have been developed by combining curvature scalars, topological invariants and their derivatives. These modified theories address the purpose of solving the complexities related to the quantum gravity and provide with the conditions through which the accelerated expansion of universe is argued. Nojiri and Odintsov [10] were the pioneers to present the idea of implicit and explicit coupling of the curvature with the matter in f(R) gravity. Some reviews [11, 12, 13] were established about the f(R) gravity by different researchers and the consistency of its different cosmological models were also studied [14]. The equivalence between metric and Palatini formalisms in f(R) gravity is shown to be achieved using divergence free current [15]. Harko et al. [16] introduced a gravitational theory by including both the matter and curvature terms and is well known today as the f(RT) gravity, where R is the scalar curvature and T is the trace of energy-momentum tensor. The evolution of the universe through energy conditions along with the criteria of stability were discussed by Sharif and Zubair [17]. They also re-established a variety of dark energy models, investigated the thermodynamical aspect and exactly solved the anisotropic universe in f(RT) gravity [18].

In recent years, the researchers have considered a new generalized approach of the Gauss–Bonnet (GB) theory named as \(f(\mathcal {G})\) gravity [19, 20, 21, 22, 23]. The GB invariant is defined as
$$\begin{aligned} \mathcal {G}=R^{2}-4R_{\alpha \beta }R^{\alpha \beta }+R_{\alpha \beta \gamma \delta }R^{\alpha \beta \gamma \delta }, \end{aligned}$$
(1)
where \(R_{\alpha \beta \gamma \delta }\) is the Reimann tensor, \(R_{\alpha \beta }\) is the Ricci tensor and R is the Ricci scalar. The interesting feature of the theory is that involvement of GB term may avoid ghost contributions and regularize the gravitational action [24]. Further modification of the theory by involving scalar curvature along with GB invariant has been presented which is named as \(f(R,\mathcal {G})\) gravity [25]. A reasonable amount of work has been published so far in these theories [26, 27, 28, 29, 30, 31, 32, 33, 34, 35]. In a recent paper [1], Sharif and Ikram presented a new modified theory named as \(f(\mathcal {G},T)\) gravity by involving the trace of the energy-momentum tensor in the function. They investigated energy conditions for Friedmann–Robertson–Walker (FRW) universe and concluded that the massive test particles followed non-geodesic lines of geometry due to the presence of extra force. It is expected that this theory may describe the late-time cosmic acceleration for some specific choices of \(f(\mathcal {G},T)\) gravity models.

The symmetry methods of approximations have played a pivotal role to work out the exact solutions of differential equations. These approximations smartly reduce the complexity involved in a system of non-linear equations by finding the unknown parameters of equations. In particular, the Noether symmetries are not just a tool to deal with the solution of the dynamics, but also their existence provides favorable conditions so that we can choose physically and analytically the universe models according to our calculated observations. Sharif and Waheed [36] re-scaled the energy of stringy charged black hole solutions using approximate symmetries. Kucukakca [37] determined the exact solutions of Bianchi type-I model, using Noether symmetries. Jamil et al. [38] used the Noether symmetry approach to find out \(f(\mathcal {T})\) explicitly for the phantom and quintessence models, where \(\mathcal {T}\) is the torsion scalar. Sharif and Shafique [39] discussed Noether symmetries in a modified scalar-tensor gravity. The exact solutions in f(R) gravity were also explored using Noether symmetries methods for FRW spacetime [42]. Similarly many authors have used Noether symmetries to investigate the cosmology in different contexts [43, 44, 45, 46, 47, 48, 49, 50, 51].

In this paper, we are interested to investigate \(f(\mathcal {G},T)\) gravity using Noether symmetries. For this purpose, we consider the flat FRW universe model. The arrangement for the paper is as follows. In Sect. 2, we provide the preliminary formalism for \(f( \mathcal {G},T)\) gravity. Section 3 gives the Noether equations of FRW universe model for \(f(\mathcal {G},T)\) gravity. Reconstruction of cosmological solutions is presented in Sect. 4. Last section provides a brief outlook of the paper.

2 \(f(\mathcal {G},T)\) gravity with field equations

In 4-dimensions the general action for \(f(\mathcal {G},T)\) gravity is given by [1],
$$\begin{aligned} \mathcal {A}= \frac{1}{2{\kappa }^{2}}\int \mathrm{d}^{4}x \sqrt{-g}[R+f(\mathcal {G},{T})]+\int \mathrm{d}^{4}x\sqrt{-g}\mathcal {L}_{M}, \end{aligned}$$
(2)
where \(\mathcal {L}_{M}\) stands for the matter Lagrangian, R is the Ricci Scalar, \(\mathcal {G}\) is the Gauss–Bonnet term, \(\mathrm {T}\) is the trace of the energy-momentum tensor, g is the metric determinant, and \(\kappa \) is the coupling constant. The energy-momentum tensor \({T}_{\zeta \eta }\) can be calculated using the following equation:
$$\begin{aligned} {T}_{\zeta \eta }=-\frac{2}{\sqrt{-g}}\frac{\delta (\sqrt{-g}\mathcal {L}_{M})}{\delta g^{\zeta \eta }}. \end{aligned}$$
(3)
However if the distribution of the matter is dependent on the metric tensor \(g_{\zeta \eta }\) only then Eq. (3) takes the form
$$\begin{aligned} {T}_{\zeta \eta }=g_{\zeta \eta }\mathcal {L}_{M}-2\frac{\partial \mathcal {L}_{M}}{\partial g^{\zeta \eta }}. \end{aligned}$$
(4)
Now varying the action Eq. (2) with respect to the metric tensor and using Eq. (4), we obtain the following field equations:
$$\begin{aligned} G_{\zeta \eta }= & {} -[2Rg_{\zeta \eta }\nabla ^{2}-2R\nabla _{\zeta }\nabla _{\eta }-4g_{\zeta \eta }R^{\mu \nu }\nabla _{\mu }\nabla _{\nu }\nonumber \\&- 4R_{\zeta \eta }\nabla ^{2}+4R^{\mu }_{\zeta }\nabla _{\eta }\nabla _{\mu }+\,4R^{\mu }_{\eta }\nabla _{\zeta }\nabla _{\mu }\nonumber \\&+4R_{\zeta \mu \eta \nu }\nabla ^{\mu }\nabla ^{\nu }]f_{\mathcal {G}}(\mathcal {G},\mathrm {\textit{T}})+ \frac{1}{2}g_{\zeta \eta }f(\mathcal {G},\mathrm {\textit{T}})\nonumber \\&-\, [\mathrm {\textit{T}}_{\zeta \eta }+\Theta _{\zeta \eta }]f_{\mathrm {\textit{T}}}(\mathcal {G},\mathrm {\textit{T}})\; \mathrm{with~respect~to~them}\nonumber \\&-\,[2RR_{\zeta \eta }-4R^{\mu }_{\zeta }R_{\mu \eta }-4R_{\zeta \mu \eta \nu }R^{\mu \nu }\nonumber \\&+2R^{\mu \nu \delta }_{\zeta }R_{\eta \mu \nu \delta }] f_{\mathcal {G}}(\mathcal {G},\mathrm {T})+\kappa ^{2}\mathrm {\textit{T}}_{\zeta \eta }, \end{aligned}$$
(5)
where \({G}_{\zeta \eta }=R_{\zeta \eta }-\frac{1}{2}g_{\zeta \eta }R\) is the Einstein tensor, \(\Box =\nabla _{\zeta }\nabla ^{\zeta }=\nabla ^{2}\) represents the d’Alembertian operator and \(\Theta _{\zeta \eta }= g^{\mu \nu }\frac{\delta \mathrm {\textit{T}}_{\mu \nu }}{\delta g_{\zeta \eta }}\). Also, \(f_{\mathcal {G}}(\mathcal {G},\mathrm {\textit{T}}))\) and \(f_{\mathrm {\textit{T}}}(\mathcal {G},\mathrm {\textit{T}}))\) represent the partial derivatives of the function \(f( \mathcal {G},T)\) with respect to \(\mathcal {G}\) and \(\textit{T}\) respectively. It is to be noted that if we take \(f(\mathcal {G},\mathrm {\textit{T}})=f(\mathcal {G})\) in Eq. (5), then the resulting equation represents the field equations of \(f(\mathcal {G})\) gravity. Moreover, by putting \(f(\mathcal {G}, \mathrm {\textit{T}})=0\), one can recover the usual Einstein field equations. The trace of Eq. (5) yields
$$\begin{aligned}&R+\kappa ^{2}{T}-(\mathrm {\textit{T}}+\Theta )f_{{T}}(\mathcal {G},{T})+2f(\mathcal {G},{T})+2\mathcal {G}f_{\mathcal {G}}(\mathcal {G},{T})\nonumber \\&\quad -2R\nabla ^{2}f_{\mathcal {G}}(\mathcal {G},{T}) +4R^{\zeta \eta }\nabla _{\zeta }\nabla _{\eta }f_{\mathcal {G}}(\mathcal {G},{T})=0. \end{aligned}$$
(6)
This is an important equation as it can be used to find the corresponding \(f(\mathcal {G},{T})\) models. The covariant divergence of Eq. (5) is given as
$$\begin{aligned} \nabla ^{\zeta }T_{\zeta \eta }= & {} \frac{f_{{T}}(\mathcal {G},\mathrm {\textit{T}})}{\kappa ^{2}-f_{{T}}(\mathcal {G},\mathrm {\textit{T}})}\bigg [({T}_{\zeta \eta }+\Theta _{\zeta \eta }) \nabla ^{\zeta }(\text {ln}f_{{T}}(\mathcal {G},{T}))\nonumber \\&+ \nabla ^{\zeta }\Theta _{\zeta \eta }- \frac{g_{\zeta \eta }}{2}\nabla ^{\zeta }T\bigg ], \end{aligned}$$
(7)
The theory might be plagued by divergences, e.g. at astrophysical scales, due to the presence of higher-order derivatives of the stress-energy tensor that are naturally present in the field equations. This seems to be an issue with higher order derivative theories that include higher order terms of stress-energy tensor. Modification of Einstein’s theory by adding auxiliary fields does not compromise the weak equivalence principle and admits a covariant Lagrangian formulation [41]. However one can put some constraints to Eq. (7) to obtain standard conservation equation for stress-energy tensor [1].
In this paper, we restrict ourselves to flat Friedmann–Robertson–Walker (FRW) spacetime,
$$\begin{aligned} \mathrm{d}s^{2}=\mathrm{d}t^{2}-a^{2}(t)(\mathrm{d}x^{2}+\mathrm{d}y^{2}+\mathrm{d}z^{2}). \end{aligned}$$
(8)
The standard matter energy-momentum tensor is defined as
$$\begin{aligned} T_{\mu \nu }=(\rho + p)u_\mu u_\nu -pg_{\mu \nu }, \end{aligned}$$
(9)
satisfying the EoS
$$\begin{aligned} p=w\rho , \end{aligned}$$
(10)
where \(u_\mu =\sqrt{g_{00}}(1,0,0,0)\) is the four-velocity in co-moving coordinates and \(\rho \) and p denote energy density and pressure of the fluid respectively. The scheme of our paper can be mainly divided into two points as follows:
  • Equation (5) are highly non-linear differential equations and its not an easy task to solve them analytically. It is mentioned here that fiat FRW modified field equations are fourth-order differential equations involving unknowns like \(f(\mathcal {G}, {T})\). Here we are interested to find the Noether symmetries of \(f(\mathcal {G},T)\) gravity with fiat FRW background.

  • The advantage of exact solutions in modified gravity have gained much importance, particularly in the study of phase transitions and recent phenomenon of accelerated expansion of universe. The viable cosmological models can be found using Noether symmetries and hence some physically important solutions can be reconstructed.

3 Noether symmetries and \(f(\mathcal {G},T)\) gravity

Noether symmetries have become an important tool to solve the system of non-linear equations. We apply Noether symmetry approach to investigate the \(f( \mathcal {G},T)\) gravity. The existence of this approach confirms the uniqueness of the vector field in the tangent space. In this situation, the vector field acts like symmetry generator which produces further the conserved quantities. The expression for the vector field and its first prolongation are given respectively as [52]
$$\begin{aligned}&{W}=\zeta (t,u^{j})\frac{\partial }{\partial t}+\xi ^{i}(t,u^{j})\frac{\partial }{\partial u^{j}},\end{aligned}$$
(11)
$$\begin{aligned}&{W}^{[1]}=\mathrm {\textit{W}}+\left( \xi ^{i}_{~,t}+\xi ^{i}_{~,j}~\dot{u}^{j}-\zeta _{~,t}~\dot{u}^{i}-\xi _{~,j}~ \dot{u}^{j}\dot{u}^{i}\right) \frac{\partial }{\partial \dot{u}^{j}}.\nonumber \\ \end{aligned}$$
(12)
where \(\zeta \) and \(\xi \) are the coefficients of the generator, \(u^i\) provides the n number of positions, and the dot gives the derivative with respect to time t. The vector field \(\textit{W}\) produces Noether gauge symmetry provided the condition
$$\begin{aligned} {W}^{[1]}\mathcal {L}+(D\zeta )\mathcal {L}=DG(t,u^{i}) \end{aligned}$$
(13)
is preserved, where \(G(t,u^i)\) denotes gauge term and D is an operator defined as
$$\begin{aligned} D=\frac{\partial }{\partial t}+\dot{u}^{i}\frac{\partial }{\partial u^{i}}. \end{aligned}$$
The Euler–Lagrange equations are given by
$$\begin{aligned} \frac{\partial \mathcal {L}}{\partial u^{i}}-\frac{\mathrm{d}}{\mathrm{d}t}\Bigg (\frac{\partial \mathcal {L}}{\partial \dot{u}^{i}}\Bigg )=0,~~~~~ \end{aligned}$$
(14)
Contraction of Eq. (14) with some unknown function \(\phi ^{i}\equiv \phi ^{i}(u^{j})\) yields
$$\begin{aligned} \phi ^{i}\Big (\frac{\partial \mathcal {L}}{\partial u^{i}}-\frac{\mathrm{d}}{\mathrm{d}t}\Big (\frac{\partial \mathcal {L}}{\partial \dot{u}^{i}}\Big )\Big )=0. \end{aligned}$$
(15)
It is easy to verify that
$$\begin{aligned} \frac{\mathrm{d}}{\mathrm{d}t}\left( \phi ^{i}\frac{\partial \mathcal {L}}{\partial \dot{u}^{i}}\right) -\left( \frac{\mathrm{d}}{\mathrm{d}t}\phi ^{i}\right) \frac{\partial \mathcal {L}}{\partial \dot{u}^{i}} =\phi ^{i}\frac{\mathrm{d}}{\mathrm{d}t}\left( \frac{\partial \mathcal {L}}{\partial \dot{u}^{i}}\right) . \end{aligned}$$
(16)
Putting this value in Eq. (15) provides us with
$$\begin{aligned} L_\textit{W}\mathcal {L} =\phi ^{i}\frac{\partial \mathcal {L}}{\partial u^{i}}+\left( \frac{\mathrm{d}}{\mathrm{d}t}\phi ^{i}\right) \frac{\partial \mathcal {L}}{\partial \dot{u}^{i}}=\frac{\mathrm{d}}{\mathrm{d}t}\left( \phi ^{i}\frac{\partial \mathcal {L}}{\partial \dot{u}^{i}}\right) , \end{aligned}$$
(17)
where L stands for the Lie derivative along the vector field. The Noether symmetries would exist only if the Lie derivative of the Lagrangian becomes zero, i.e. the condition
$$\begin{aligned} L_{{W}}\mathcal {L}=0. \end{aligned}$$
Since the Lagrangian \(\mathcal {L}\) is invariant along the vector field \(\textit{W}\), consequently the definition for Noether current turns out to be [53]
$$\begin{aligned} j^{t}=\left( \phi ^{i}\frac{\partial \mathcal {L}}{\partial \dot{u}^{i}}\right) , \end{aligned}$$
(18)
and for the Noether current to be a conserved quantity, we must have
$$\begin{aligned} j^{t}_{,t}=0. \end{aligned}$$
(19)
Now we write again the action (2) for the case of perfect fluid as
$$\begin{aligned} \mathcal {A}=\int \mathrm{d}t\sqrt{-g}[R+f(\mathcal {G},{T})-\mu _{1}(\mathcal {G}-\mathcal {\bar{G}})-\mu _{2}({T}-\bar{T})+\mathcal {L}_{M}]. \end{aligned}$$
(20)
Here \(\textit{T}\) is the trace of energy-momentum tensor, \(\sqrt{-g}=a^{3}(t),\bar{\mathcal {G}}\) and \(\bar{{T}}\) stand for dynamical constraints, while \(\mu _{1}\) and \(\mu _{2}\) are the multipliers, worked out as
$$\begin{aligned} \mu _{1}=f_{\mathcal {G}}(\mathcal {G},{T}),~~ \mu _{2}=f_{{T}}(\mathcal {G},\mathrm {\textit{T}}),~~ \bar{{T}}=\rho (a)-3p(a). \end{aligned}$$
Since there does not exist any unique definition of matter Lagrangian, so we consider \(\mathcal {L}_{M}=-p(a)\) and after an integration by parts, the point-like Lagrangian takes the following form
$$\begin{aligned} \nonumber&\mathcal {L}(a,R,\mathcal {G},{T},\dot{a},\dot{R},\dot{\mathcal {G}},{T})\\&\nonumber \quad = a^{3}[R+f-\mathcal {G}f_{\mathcal {G}} -f_{T}\{\mathrm {\textit{T}}-(\rho (a)-3p(a))\}-p(a)]\\&\qquad -8\dot{a}^{3}\dot{\mathcal {G}}f_{\mathcal {GG}}- 8\dot{a}^{3}\dot{{T}}f_{{\mathcal {G}}{T}}, \end{aligned}$$
(21)
where \(f\equiv f(\mathcal {G})\), \(f_{\mathcal {G}}\equiv f_{\mathcal {G}}(\mathcal {G},{T})\) etc. Using Eq. (21), the Euler–Lagrangian equations turn out to be
$$\begin{aligned}&3a^{2}[R+f-\mathcal {G}f_{\mathcal {G}}- f_{{T}}\{\mathrm {T}-(\rho (a)-3p(a))\}-p(a)]\nonumber \\&\qquad +a^{3}[-f_{{T}}\{-3p_{,a}(a)+\rho _{,a}(a)\}-p_{,a}(a)]- [\dot{\mathcal {G}}^{2}f_{\mathcal {G}\mathcal {G}\mathcal {G}}\nonumber \\&\qquad +2\dot{\mathcal {G}}\dot{{T}}f_{\mathcal {G}\mathcal {G} {T}} \ddot{\mathcal {G}}f_{\mathcal {G}\mathcal {G}}+\dot{{T}}^{2}f_{\mathcal {G}\mathcal {G}{T}}+\ddot{\mathrm {\textit{T}}} f_{\mathcal {G} {T}}]\nonumber \\&\quad =\frac{2\ddot{a}}{\dot{a}}\bigg (\dot{\mathcal {G}}f_{\mathcal {G}\mathcal {G}}+\dot{{T}} f_{\mathcal {G}{T}}\bigg ), \end{aligned}$$
(22)
$$\begin{aligned} \bigg (\frac{\dot{a}}{a}\bigg )^{2}\bigg (\frac{\ddot{a}}{a}\bigg )= & {} -\frac{1}{24f_{\mathcal {GG}}}\big [-\mathcal {G}f_{\mathcal {GG}}-{T}f_{\mathcal {G}}- f_{\mathcal {G}{T}}\{\mathrm {\textit{T}}\nonumber \\&-(\rho (a)-3p(a))\}\big ], \end{aligned}$$
(23)
$$\begin{aligned} \bigg (\frac{\dot{a}}{a}\bigg )^{2}\bigg (\frac{\ddot{a}}{a}\bigg )= & {} -\frac{1}{24f_{\mathcal {G}{T}}} \big [f_{\mathrm {\textit{T}}}- \mathcal {G}f_{\mathcal {G}{T}}-f_{{TT}} \{\rho (a)\nonumber \\&-3p(a)\}-f_{\mathrm {\textit{T}}}\big ]. \end{aligned}$$
(24)
Also the corresponding vector field takes the form
$$\begin{aligned} \mathrm {\textit{W}}=\alpha \frac{\partial }{\partial a}+\beta \frac{\partial }{\partial R}+\gamma \frac{\partial }{\partial \mathcal {G}}+\delta \frac{\partial }{\partial \mathrm {\textit{T}}}+\dot{\alpha }\frac{\partial }{\partial \dot{a}}+\dot{\beta }\frac{\partial }{\partial \dot{R}}+\dot{\gamma }\frac{\partial }{\partial \dot{\mathcal {G}}}+\dot{\delta }\frac{\partial }{\partial \dot{\mathrm {\textit{T}}}}, \end{aligned}$$
(25)
where \(\alpha ,~\beta ,~\gamma \) and \(\delta \) are functions of \(a,~R,~\mathcal {G}\) and \(\mathrm {\textit{T}}\). Now using Lagrangian (21) and Noether equation (13), an over-determined system of partial differential equations (PDE’s) is obtained:
$$\begin{aligned}&-8\frac{\partial \gamma }{\partial R}f_{\mathcal {G}\mathcal {G}}-8\frac{\partial \delta }{\partial R}f_{\mathcal {G}\mathrm {\textit{T}}}=0,\end{aligned}$$
(26)
$$\begin{aligned}&-8\gamma f_{\mathcal {G}\mathcal {G}\mathcal {G}}-8\delta f_{\mathcal {G}\mathcal {G}\mathrm {\textit{T}}}-24\frac{\partial \alpha }{\partial a}f_{\mathcal {G}\mathcal {G}}-8\frac{\partial \gamma }{\partial \mathcal {G}}f_{\mathcal {G}\mathcal {G}}\nonumber \\&\quad -8\frac{\partial \delta }{\partial \mathcal {G}}f_{\mathcal {G}\mathrm {\textit{T}}}=0,\end{aligned}$$
(27)
$$\begin{aligned}&-8\gamma f_{\mathcal {G}\mathcal {G}\mathrm {\textit{T}}}-8f_{\mathcal {G}\mathrm {\textit{T}}\mathrm {\textit{T}}}-24\frac{\partial \alpha }{\partial a}f_{\mathcal {G}\mathrm {\textit{T}}}\nonumber \\&\quad -8\frac{\partial \gamma }{\partial \mathrm {\textit{T}}}f_{\mathcal {G}\mathcal {G}}-8\frac{\partial \delta }{\partial \mathrm {\textit{T}}}f_{\mathcal {G}\mathrm {\textit{T}}}=0,\end{aligned}$$
(28)
$$\begin{aligned}&-8\frac{\partial \gamma }{\partial a}f_{\mathcal {G}\mathcal {G}}-8\frac{\partial \delta }{\partial a}f_{\mathcal {G}\mathrm {\textit{T}}}=0,\end{aligned}$$
(29)
$$\begin{aligned}&-24\frac{\partial \alpha }{\partial \mathcal {G}}f_{\mathcal {G}\mathrm {\textit{T}}}-24\frac{\partial \alpha }{\partial \mathrm {\textit{T}}}f_{\mathcal {G}\mathcal {G}}=0,\end{aligned}$$
(30)
$$\begin{aligned}&-24\frac{\partial \alpha }{\partial R}f_{\mathcal {G}\mathrm {\textit{T}}}=0,\end{aligned}$$
(31)
$$\begin{aligned}&-24\frac{\partial \alpha }{\partial R}f_{\mathcal {G}\mathcal {G}}=0,\end{aligned}$$
(32)
$$\begin{aligned}&-24\frac{\partial \alpha }{\partial \mathcal {G}}f_{\mathcal {G}\mathcal {G}}=0,\end{aligned}$$
(33)
$$\begin{aligned}&-24\frac{\partial \alpha }{\partial \mathrm {\textit{T}}}f_{\mathcal {G}\mathrm {\textit{T}}}=0, \end{aligned}$$
(34)
$$\begin{aligned}&3a^{2}\alpha [R+f-\mathcal {G}f_{\mathcal {G}}-f_{\mathrm {\textit{T}}} \{\mathrm {\textit{T}}-(\rho (a)-3p(a))\}-p(a)]\nonumber \\&\quad -a^{3}\alpha [f_{\mathrm {\textit{T}}}\{-3p_{,a}(a)+\rho _{,a}(a)\}-p_{,a}(a)]+a^{3}\beta \nonumber \\&\quad +\gamma a^{3}[-\mathcal {G}f_{\mathcal {G}\mathcal {G}} -f_{\mathcal {G}\mathrm {\textit{T}}}\times \{\mathrm {\textit{T}}-(\rho (a)-3p(a))\}]\nonumber \\&\quad + \delta a^{3}[-\mathcal {G}f_{\mathcal {G}\mathrm {\textit{T}}}-\mathrm {\textit{T}}f_{\mathrm {\textit{T}} \mathrm {\textit{T}}}+f_{\mathrm {\textit{T}}\mathrm {\textit{T}}}(\rho (a)-3p(a))]=0. \end{aligned}$$
(35)
It is mentioned here that for the sake of simplicity, we have considered the gauge term zero. Using Eq. (19), conservation equation for Noether charge takes the form
$$\begin{aligned}&\frac{d}{dt}\Bigg [\alpha \Big \{\frac{\partial }{\partial \dot{a}}\big (8\dot{a}^{3}\dot{\mathcal {G}}f_{\mathcal {GG}}+ 8\dot{a}^{3}\dot{\mathrm {T}}f_{\mathcal {G}\mathrm {T}}\big )\Big \}\nonumber \\&\quad + \gamma \frac{\partial }{\partial \dot{\mathcal {G}}}(8\dot{a}^{3}\dot{\mathcal {G}}f_{\mathcal {GG}})-\delta \frac{\partial }{\partial \dot{\mathrm {T}}}(\dot{a}^{3}\dot{\mathrm {T}}f_{\mathcal {G}\mathrm {T}})\Bigg ]=0.\nonumber \\ \end{aligned}$$
(36)
Now we solve the system of PDE’s (2635) for different cases.

Case(i):

Let us assume that \(f_{\mathcal {G}\mathcal {G}}=0\). Manipulating the Eqs. (2635), we obtain \(\alpha =0\), \(\beta =0\), \(\gamma =0\), and \(\delta =0\), hence providing us with a trivial solution. Moreover, the conservation Eq. (36) is also satisfied in this case. Thus, we have to consider \(f_{\mathcal {G}\mathcal {G}}\ne 0\) to obtain a non-trivial solution.

Case(ii):

Now let us assume that \(f_{\mathcal {G}\mathcal {\textit{T}}}=0\) and \(f_{\mathcal {G}\mathcal {G}}\ne 0\). Therefore, the cosmological model takes the form \(f(\mathcal {G},\textit{T})=a_{0}\mathcal {G}^{2}+b_{0}{} \textit{T}^{2}\), where \(a_{0}\) and \(b_{0}\) are the arbitrary constants. Here the manipulation of Noether equations provides \(\alpha =0=\gamma \), \(\delta =c_{1}\) and \(\beta =c_{1}{} \textit{T}+c_{2}\). Thus the symmetry generator becomes
$$\begin{aligned} \textit{W}=(c_{1}{} \textit{T}+c_{2})\frac{\partial }{\partial R}+c_{1}\frac{\partial }{\partial \textit{T}}. \end{aligned}$$
(37)
Now the conservation Eq. (36) referring to the Noether current gives
$$\begin{aligned} \dot{a}^{3}f_{\mathcal {G}\mathrm {T}}=c_3, \end{aligned}$$
(38)
where \(c_3\) is an integration constant. It is mentioned here that this case satisfies the conservation Eq. (38) when we choose the integration constant equal to zero. The corresponding Lagrangian becomes
$$\begin{aligned} \mathcal {L}&=a^{3}\big [R-a_{0}\mathcal {G}^{2}-b_{0}\mathrm {\textit{T}}^{2}+2b_{0}\mathrm {\textit{T}}\{\rho (a)\nonumber \\&\quad -3p(a)\}-p(a)\big ]-16\dot{a}^{3}a_{0}\dot{\mathcal {G}}. \end{aligned}$$
(39)
The corresponding Euler–Lagrangian equations are calculated as
$$\begin{aligned}&a^{2}(R-a_{0}\mathcal {G}^{2}-b_{0}\mathrm {\textit{T}}^{2}+2b_{0}\{\rho (a)\nonumber \\&\quad -3p(a)\}\mathrm {\textit{T}}-p)+32a_{0}\dot{a}\ddot{a}\dot{\mathcal {G}}+16a_{0}\dot{a}^{2}\ddot{\mathcal {G}}=0,\nonumber \\&a^{3}(R-2a_{0}\mathcal {G})+48a_{0}\dot{a}^{2}\ddot{a}=0,\nonumber \\&\quad -2a^{3}b_{0}(T-\{\rho (a)-3p(a)\})=0. \end{aligned}$$
(40)
Using Eq. (40), it follows that
$$\begin{aligned} a=c_{4}\sqrt{2t+c_{5}}, ~~~~ \mathcal {G}=\frac{-24}{(2t+c_{5})^{4}}. \end{aligned}$$
(41)
where \(c_{4}\) and \(c_{5}\) are the constants of integration.

4 Reconstruction of cosmological solutions

In this section, we provide the cosmological solutions by considering \(f(\mathcal {G},\textit{T})=\mathcal {G}^{k}{} \textit{T}^{1-k}\), where k is an arbitrary real number. We reconstruct the solutions for the case \({k}=2\). The Lagrangian takes the shape
$$\begin{aligned} \mathcal {L}=a^{3}\bigg [R-\frac{\mathcal {G}^{2}\{\rho (a)-3p(a)\}}{\mathrm {\textit{T}}^2}-p(a)\bigg ]-\frac{16\dot{a}^{3}}{\mathrm {\textit{T}}}\bigg (\dot{\mathcal {G}}-\frac{\dot{\mathrm {\textit{T}}}}{\mathrm {\textit{T}}}\bigg ). \end{aligned}$$
(42)
Euler–Lagrangian equations here take the form
$$\begin{aligned}&3a^{2}\bigg [R-\frac{\mathcal {G}^{2}\{\rho (a)-3p(a)\}}{\mathrm {\textit{T}}^2}-p(a)\bigg ]\nonumber \\&\quad -a^{3}\bigg [ \frac{\{\rho (a)-3p(a)\}_{,a}\mathcal {G}^{2}}{\mathrm {\textit{T}}^2}+p_{,a}(a)\bigg ]\nonumber \\&\quad +\frac{48(\dot{a}^{2}\ddot{\mathcal {G}}-2\dot{a}\ddot{a}\dot{\mathcal {G}})}{\mathrm {\textit{T}}}-\frac{48\dot{\mathrm {\textit{T}}} \dot{a}^{2}\dot{\mathcal {G}}}{\mathrm {\textit{T}}^{2}}-\frac{48(\dot{a}^{2}\ddot{{\mathrm {\textit{T}}}}+2\dot{\textit{T}}\dot{a}\ddot{a})}{\mathrm {\textit{T}}^{2}}\nonumber \\&\quad +\frac{96{{\dot{{\mathrm {\textit{T}}}}}^2\dot{a}}^2}{\mathrm {\textit{T}}^{3}} =0,\end{aligned}$$
(43)
$$\begin{aligned}&\mathcal {G}\{\rho (a)-3p(a)\}-24\mathrm {\textit{T}}\dot{a}^{2}\ddot{a}+8\dot{a}^{3}\dot{\mathrm {\textit{T}}}=0,\end{aligned}$$
(44)
$$\begin{aligned}&{a}^{3}\mathcal {G}^{2}\{\rho (a)-3p(a)\}-8\mathrm {\textit{T}}\dot{a}^{3} \dot{\mathcal {G}}+24\mathrm {\textit{T}}\dot{a}^{2}\ddot{a}=0. \end{aligned}$$
(45)
Using Eq. (45) and by putting the corresponding values for \(\mathcal {G}\) and \(\mathrm {\textit{T}}\), we get
$$\begin{aligned} 40a{\ddot{a}}^2{\dot{a}}^4+8a{\dot{a}}^5{\dddot{a}}-24{\dot{a}}^6{\ddot{a}}-a^4{\ddot{a}}{\dot{a}}^2=0. \end{aligned}$$
(46)
This equation admits a solution of exponential form
$$\begin{aligned} a=e^{mt}, \end{aligned}$$
(47)
where m is an arbitrary constant. It is mentioned here that exponential solution is satisfied with the constraint equation
$$\begin{aligned} 24m^8-m^4=0 \end{aligned}$$
(48)
yielding the real solutions
$$\begin{aligned} m=0, ~~~m\approx 0.451801,~~~m\approx -0.451801. \end{aligned}$$
(49)
Also, using Eq. (44) the value of trace of energy momentum tensor turns out to be
$$\begin{aligned} T=c_5e^{\frac{3}{4}(4-a^{3})}, \end{aligned}$$
(50)
where \(c_5\) is constant of integration. Using Eqs. (43) and (44), we obtain
$$\begin{aligned} p(a)_{,a}+\frac{3}{a}p(a)=l(a), \end{aligned}$$
(51)
where
$$\begin{aligned} l(a)= & {} \frac{c_5e^{\frac{3}{2}(a^{3}-4)}}{a^{3}}\nonumber \\&\times \bigg [-3a^2{\mathcal {G}}^2\textit{T}+a^3\mathcal {G}^2{\textit{T}}_a+ 96\dot{a}{} \textit{T}(\ddot{a}\dot{\mathcal {G}}-\dot{a})\nonumber \\&+48\dot{a}^2(\dot{\mathcal {G}}\dot{\textit{T}}-\ddot{\mathcal {G}}{} \textit{T} +\ddot{\textit{T}})-\frac{96(\textit{T}\dot{a})^2}{\textit{T}}\bigg ]. \end{aligned}$$
(52)
It is evident that Eq. (51) is a non-homogeneous linear differential equation and one can solve it to find the pressure and consequently the energy density of the universe. Thus in this case the solution metric takes the form
$$\begin{aligned} \mathrm{d}s^{2}=\mathrm{d}{t}^{2}-e^{2mt}[\mathrm{d}x^{2}+\mathrm{d}{y}^{2}+\mathrm{d}{z}^{2}]. \end{aligned}$$
(53)
This corresponds to the well-known deSitter spacetime in GR. Here we have constructed a physical cosmological solution with a particular \(f(\mathcal {G},\textit{T})\) gravity model. Similarly, more solutions with some other cosmological models can be reconstructed.

5 Outlook

In this paper, we have discussed in detail about the Noether symmetries of the flat FRW universe model in \(f(\mathcal {G},\mathrm {T})\) gravity. Noether symmetries are not just a tool to deal with the solution of the dynamics, but also their existence provides favorable conditions so that we can choose physically and analytically the universe models according to our calculated observations. Lagrangian multipliers perform a big part to shape the Lagrangian into its canonical form and so as to reduce the dynamics to determine the exact solutions. We have worked out the Lagrangian for FRW universe model in \(f(\mathcal {G},\mathrm {T})\) theory. The existence of Noether charges is considered important in the literature and equation for conservation of charge plays an important role to investigate the Noether symmetries. The conservation equation for Noether charge has been developed. The exact solutions of Noether equations have been discussed for two cases of \(f(\mathcal {G},\mathrm {T})\) gravity models. The first case when \(f_{\mathcal {G}\mathcal {G}}=0\) yields trivial symmettries while we obtain non-trivial symmetries for the second case when \(f_{\mathcal {G}\mathrm {\textit{T}}}=0\) and \(f_{\mathcal {G}\mathcal {G}}\ne 0\). Thus we have also worked out the corresponding \(f(\mathcal {G},\mathrm {T})\) gravity model and the solution metric. It is concluded that the second case provides \(f(\mathcal {G},\textit{T})=a_{0}\mathcal {G}^{2}+b_{0}{} \textit{T}^{2}\) gravity model, where \(a_{0}\) and \(b_{0}\) are arbitrary constants. Furthermore, solutions in both cases satisfy the conservation equation for Noether charge.

We have also reconstructed an important cosmological solution by considering \(f(\mathcal {G},\textit{T})=\mathcal {G}^{k}{} \textit{T}^{1-k}\), where k is an arbitrary real number. This model yields the well-known deSitter solution already available in GR. It is mentioned here that many other cosmologically physical solutions may be reconstructed for some other choice of \(f(\mathcal {G},\textit{T})\) gravity models. We have discussed the exact solutions with only three cases. Many other solutions can be explored by assuming some other forms of \(f(\mathcal {G},\mathrm {T})\).

Notes

Acknowledgements

Many thanks to the anonymous reviewer for valuable comments and suggestions to improve the paper. This work was supported by National University of Computer and Emerging Sciences (NUCES).

References

  1. 1.
    M. Sharif, A. Ikram, Eur. Phys. J. C 76, 640 (2016)ADSCrossRefGoogle Scholar
  2. 2.
    A.G. Riess et al. (Supernova Search Team), Astron. J. 116, 1009 (1998)Google Scholar
  3. 3.
    C.L. Bennett et al., Astrophys. J. Suppl. 148, 1 (2003)ADSCrossRefGoogle Scholar
  4. 4.
    D.N. Spergel et al., Astrophys. J. Suppl. 148, 175 (2003)ADSCrossRefGoogle Scholar
  5. 5.
    A.G. Riess et al., Astrophys. J. 607, 665 (2004)ADSCrossRefGoogle Scholar
  6. 6.
    M. Tegmartk et al., Phys. Rev. D 69, 103501 (2004)ADSCrossRefGoogle Scholar
  7. 7.
    J. Hogan, Nature 448, 240 (2007)ADSCrossRefGoogle Scholar
  8. 8.
    P.S. Corasaniti et al., Phys. Rev. D 70, 083006 (2004)ADSCrossRefGoogle Scholar
  9. 9.
    J. Weller, A.M. Lewis, Mon. Not. Astron. Soc. 346, 987 (2003)ADSCrossRefGoogle Scholar
  10. 10.
    S. Nojiri, S.D. Odintsov, Phy. Lett. 599, 137 (2004)ADSCrossRefGoogle Scholar
  11. 11.
    A.D. Felice, S. Tsujikaswa, Living Rev. Rel. 13, 3 (2010)Google Scholar
  12. 12.
    S. Nojiri, S.D. Odintsov, Phys. Rept. 505, 59 (2011)ADSCrossRefGoogle Scholar
  13. 13.
    K. Bamba, S. Capozziella, S. Nojiri, S.D. Odintsov, Astrophys. Space Sci. 342, 155 (2012)ADSCrossRefGoogle Scholar
  14. 14.
    A.A. Starobinsky, J. Exp. Theor. Phy. Lett. 86, 157 (2009)CrossRefGoogle Scholar
  15. 15.
    S. Capozziello, F. Darabi, D. Vernieri, Mod. Phys. Lett. A 26, 65 (2011)ADSCrossRefGoogle Scholar
  16. 16.
    T. Harko, F.S.N. Lobo, S. Nojiri, S.D. Odinttsov, Phys. Rev. D 84, 024020 (2011)ADSCrossRefGoogle Scholar
  17. 17.
    M. Sharif, M. Zubair, J. Phys. Soc. Jpn. 82, 014002 (2013)ADSCrossRefGoogle Scholar
  18. 18.
    M. Sharif, M. Zubair, J. Cosmol. Astropart. Phys. 03, 028 (2012)ADSCrossRefGoogle Scholar
  19. 19.
    G. Cognola, E. Elizalde, S. Nojiri, S.D. Odintsov, S. Zerbini, Phys. Rev. D 75, 086002 (2007)ADSMathSciNetCrossRefGoogle Scholar
  20. 20.
    G. Cognola, E. Elizalde, S. Nojiri, S.D. Odintsov, S. Zerbini, Phys. Rev. D 73, 084007 (2006)ADSCrossRefGoogle Scholar
  21. 21.
    M.F. Shamir, Astrophys. Space Sci. 361, 147 (2016)ADSCrossRefGoogle Scholar
  22. 22.
    M.F. Shamir, J. Exp. Theor. Phys. 123, 607 (2016)ADSCrossRefGoogle Scholar
  23. 23.
    S. Nojiri, S.D. Odintsov, Phys. Lett. B 631, 1 (2005)ADSMathSciNetCrossRefGoogle Scholar
  24. 24.
    T. Chiba, J. Cosmol. Astropart. Phys. 03, 008 (2005)ADSMathSciNetCrossRefGoogle Scholar
  25. 25.
    S. Nojiri, S.D. Odintsov, P.V. Tretyakov, Prog. Theor. Phys. Suppl. 172, 81 (2008)ADSCrossRefGoogle Scholar
  26. 26.
    M. Sharif, H.I. Fatima, Mod. Phys. Lett. A 30, 1550142 (2015)ADSCrossRefGoogle Scholar
  27. 27.
    M. Sharif, H.I. Fatima, JETP 149, 121 (2016)Google Scholar
  28. 28.
    M. Sharif, H.I. Fatima, Int. J. Mod. Phys. D 25, 1650011 (2016)ADSCrossRefGoogle Scholar
  29. 29.
    M. Sharif, A. Ikram, J. Exp. Theor. Phys. 123, 40 (2016)ADSCrossRefGoogle Scholar
  30. 30.
    M.J.S. Houndjo, M.E. Rodrigues, D. Momeni, R. Myrzakulov, Can. J. Phys. 92, 1528 (2014)ADSCrossRefGoogle Scholar
  31. 31.
    M.E. Rodrigues, M.J.S. Houndjo, D. Momeni, R. Myrzakulov, Can. J. Phys. 92, 173 (2014)CrossRefGoogle Scholar
  32. 32.
    B. Wu, B. Ma, Phys. Rev. D 92, 044012 (2015)ADSMathSciNetCrossRefGoogle Scholar
  33. 33.
    M. Laurentis, M. Paolella, S. Capozziello, Phys. Rev. D 91, 083531 (2015)ADSMathSciNetCrossRefGoogle Scholar
  34. 34.
    A.D. Felice, T. Suyama, T. Tanaka, Phys. Rev. D 83, 104035 (2011)ADSCrossRefGoogle Scholar
  35. 35.
    L. Sebastiani, Springer Proc. Phys. 137, 261 (2011)CrossRefGoogle Scholar
  36. 36.
    M. Sharif, S. Waheed, Can. J. Phys. 88, 833 (2010)ADSCrossRefGoogle Scholar
  37. 37.
    Y. Kucukakca, U. Camci, I. Semiz, Gen. Relat. Gravit. 44, 1893 (2012)ADSCrossRefGoogle Scholar
  38. 38.
    M. Jamil, D. Momeni, R. Myrzakulov, Eur. Phys. J. C 72, 2137 (2012)ADSCrossRefGoogle Scholar
  39. 39.
    M. Sharif, I. Shafique, Phys. Rev. D 90, 084033 (2014)ADSCrossRefGoogle Scholar
  40. 40.
    M. Sharif, I. Fatima, J. Exp. Theor. Phys. 122, 104 (2016)ADSCrossRefGoogle Scholar
  41. 41.
    P. Pani, T.P. Sotiriou, D. Vernieri, Phys. Rev. D 88, 121502 (2013)ADSCrossRefGoogle Scholar
  42. 42.
    S. Capozziello, A. Stabile, A. Troisi, Class. Quant. Grav. 24, 2153 (2007)ADSCrossRefGoogle Scholar
  43. 43.
    M. Jamil, F.M. Mahomed, D. Momeni, Phys. Lett. B 702, 315 (2011)ADSCrossRefGoogle Scholar
  44. 44.
    I. Hussain, M. Jamil, F.M. Mahomed, Astrophys. Space Sci. 337, 373 (2012)ADSCrossRefGoogle Scholar
  45. 45.
    U. Camci, Eur. Phys. J. C 74, 3201 (2014)ADSCrossRefGoogle Scholar
  46. 46.
    U. Camci, JCAP 07, 002 (2014)ADSCrossRefGoogle Scholar
  47. 47.
    M. Sharif, S. Waheed, Phys. Scr. 83, 015014 (2011)ADSCrossRefGoogle Scholar
  48. 48.
    M. Sharif, S. Waheed, J. Cosmol. Astropart. Phys. 02, 043 (2013)ADSCrossRefGoogle Scholar
  49. 49.
    M.F. Shamir, A. Jhangeer, A.A. Bhatti, Chin. Phys. Lett. 29(8), 080402 (2012)CrossRefGoogle Scholar
  50. 50.
    D. Momeni, H. Gholizade, Int. J. Mod. Phys. D 18, 1 (2009)CrossRefGoogle Scholar
  51. 51.
    S. Capozziello, S.J.G. Gionti, D. Vernieri, JCAP 1601, 015 (2016)ADSCrossRefGoogle Scholar
  52. 52.
    P.J. Olver, Applications of Lie Groups to Differential Equations (Springer, New York, 2000)MATHGoogle Scholar
  53. 53.
    S. Capozziello, N. Frusciante, D. Vernieri, Gen. Relat. Gravit. 44, 1881 (2012)ADSCrossRefGoogle Scholar

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Authors and Affiliations

  1. 1.National University of Computer and Emerging SciencesLahore CampusPakistan

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