Exact cosmological solutions for MOG

Open Access
Regular Article - Theoretical Physics


We find some new exact cosmological solutions for the covariant scalar–tensor–vector gravity theory, the so-called modified gravity (MOG). The exact solution of the vacuum field equations has been derived. Also, for non-vacuum cases we have found some exact solutions with the aid of the Noether symmetry approach. More specifically, the symmetry vector and also the Noether conserved quantity associated to the point-like Lagrangian of the theory have been found. Also we find the exact form of the generic vector field potential of this theory by considering the behavior of the relevant point-like Lagrangian under the infinitesimal generator of the Noether symmetry. Finally, we discuss the cosmological implications of the solutions.


Vector Field Scalar Field Cosmic Scale Factor Modify Friedmann Equation Exact Cosmological Solution 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

1 Introduction

We study a scalar–tensor–vector theory which has been introduced as an alternative to particle dark matter [1]. This theory is referred to as modified gravity (MOG) in the current literature. Mathematically, MOG is more complicated than GR in the sense that it postulates more gravitational fields than GR. In fact, MOG is a scalar–tensor–vector theory of gravity, while GR is a tensor theory. In other words, in MOG, in addition to the metric tensor, there are two scalar fields [\(\mu (x^{\alpha })\) and \(G(x^{\alpha })\)] and also a massive Proca vector field \(\phi ^{\alpha }\). In fact, the gravitational constant is variable as is in scalar–tensor theories of gravity. Therefore, the existence of these fields will provide some degrees of freedom, which may help to handle the dark matter problem without invoking dark matter particles. It is worth mentioning that adding non-minimal scalar fields to the effective Lagrangian of gravitational field dates back to Brans–Dicke theory [2]. In this theory the non-minimal scalar field was introduced in order to incorporate the Mach principle into GR. However, there are also other motivations for bringing into play the scalar fields. For example, non-minimally coupled terms between scalar fields and geometric quantities, such as the Ricci scalar R, have to be added to the gravitational action when quantum corrections are taken into account. Also scalar–tensor theories appear as the dimensionally reduced effective theories of higher dimensional theories, such as Kaluza–Klein theory. For a comprehensive review of the subject, we refer the reader to [3].

On the other hand, incorporating the vector fields in the gravitational action is based on different motivations. In vector–tensor theories, in the form of Einstein-aether theories [4], there is a Lorentz-violating vector field. The existence of this vector field can significantly affect the cosmology. For example, it may leave an imprint on cosmological perturbations in the early universe [5], and it can even affect the structure formation rate in the universe. Also, vector fields are simple and natural candidates to explain some certain anomalies in the Cosmic Microwave Background [6].

For another example of theories containing vector fields, one may refer to tensor–vector–scalar theory (TeVeS) [7]. TeVeS is a relativistic and covariant theory for modified Newtonian dynamics (MOND) [8]. This theory has both types of above mentioned fields, i.e. scalar and vector fields.

As we mentioned before, MOG is also another example of theories where scalar and vector fields participate in the gravitational sector. This theory has been applied to explain the rotation curves of spiral galaxies and the mass discrepancy in the galaxy clusters [9, 10, 11, 12, 13, 14]. Recently, it has been claimed that this theory is in excellent agreement with the rotation curve data for the Milky Way, while MOND does not fit the data [15]. In fact, the observed rotation curve data for the Milky Way extends as far as 200 kpc from the center of the galaxy. Data for such a large distances from the core of the galaxy may provide a critical test of modified theories of gravity [15].

There are some papers in the relevant literature which have studied the consequences of MOG at the cosmological scale, for example see [16, 17, 18, 19, 20]. However, to the best of our knowledge, the astrophysical aspects of this theory have been investigated more extensively than its cosmological consequences. For example, there is no exact cosmological solution for this theory in the literature. This point motivated us to study the cosmological behavior of this theory by looking for exact solutions for the modified Friedmann equations. To do so, we use the Noether symmetry approach [21]. In fact, as every conservation theorem, the Noether conservation theorem allows one to reduce dynamics of the cosmological model and gives insight into conserved quantities. This approach has been extensively used in various cosmological models and modified theories of gravity; for example see [22, 23, 24, 25, 26, 27, 28, 29, 30, 31, 32, 33, 34]. More specifically, in [23] the Noether symmetry approach is used in non-minimal scalar–tensor theories and in higher order theories of gravity. Also a general review of the Noether symmetry approach is presented in this paper. In the context of MOG, there is also a non-minimal scalar field. We shall see that there are some cosmological exact solutions in MOG which are similar to those presented in [23], for example see Sect. 6.4.

It is worth mentioning at this point that the Hojman’s conservation theorem [35] has also been used to study the dynamics of cosmological models and to find exact cosmological solutions for them [36].

The layout of the paper is the following. In Sect. 2, we briefly review MOG’s field equations and derive the corresponding modified Friedmann equations. In Sect. 4, we derive the point-like Lagrangian which is needed for applying the Noether symmetry approach. Section 5 is devoted to the application of the Noether conservation theorem to MOG. In this section we find the explicit form of the generic vector field potential by symmetry issues. In Sect. 6, for the first time in the literature, we find some new exact solutions for MOG and discuss their cosmological implications. Conclusions are drawn in Sect. 7.

2 Modified gravity (MOG)

We start with the generic action of MOG,
$$\begin{aligned} S= & {} \frac{1}{16\pi }\int \sqrt{-g}d^4x \left[ \frac{\chi ^2}{2}(R-2\varLambda )+\frac{1}{2}g^{\mu \nu }\nabla _{\mu }\chi \nabla _{\nu }\chi \right. \\ \nonumber&\left. + \frac{\chi ^2}{4}g^{\mu \nu }\nabla _{\mu }\psi \nabla _{\nu }\psi +\omega _0\left[ \frac{1}{4}B_{\mu \nu }B^{\mu \nu }+V_{\phi }\right] \right] +S_M \end{aligned}$$
where R is the Ricci scalar, \(S_M\) is the matter action, \(\varLambda \) is the cosmological constant, \(\omega _0\) is a positive coupling constant, \(B_{\mu \nu }=\nabla _{\mu }\phi _{\nu }-\nabla _{\nu }\phi _{\mu }\), and the scalar fields \(\chi \) and \(\psi \) are related to those of the original paper [1] as \(\chi ^2=2/G\) and \(\psi =\ln \mu \). Also \(V_{\phi }\) is the self-interaction potential for the vector field \(\phi ^{\mu }\) and they can be a function of \(\phi _{\mu }\phi ^{\mu }\) and \(\psi \). Variation of (1) with respect to \(g^{\mu \nu }\), \(\phi _{\alpha }\), \(\chi \), \(\psi \) leads to the following field equations, respectively [37]:
$$\begin{aligned} G_{\mu \nu }+\varLambda g_{\mu \nu }=\frac{1}{\chi ^2}(\nabla _{\mu }\nabla _{\nu }-g_{\mu \nu }\square )\chi ^2+\frac{16\pi }{\chi ^2} T^\mathrm{total}_{\mu \nu }, \end{aligned}$$
$$\begin{aligned} \nabla _{\mu }B^{\alpha \mu }+ \frac{\partial V_{\phi }}{\partial \phi _{\alpha }}=-\frac{16\pi }{\omega _0} J^{\alpha }, \end{aligned}$$
$$\begin{aligned} \square \chi =\chi R+\frac{\chi }{2}g^{\mu \nu }\nabla _{\mu }\psi \nabla _{\nu }\psi , \end{aligned}$$
$$\begin{aligned} \square \psi =-\frac{2}{\chi }\nabla _{\gamma }\chi \nabla ^{\gamma }\psi +\frac{2\omega _0}{\chi ^2}\frac{\partial V_{\phi }}{\partial \psi } \end{aligned}$$
where \(G_{\mu \nu }\) is the Einstein tensor and \(J^{\alpha }\) is a “fifth force” matter current defined as
$$\begin{aligned} J^{\alpha }=-\frac{1}{\sqrt{-g}}\frac{ \delta S_M}{\delta \phi _{\alpha }}; \end{aligned}$$
a nonzero \(J^{\alpha }\) means that there is a coupling between matter and the Proca vector field \(\phi ^{\mu }\). Consequently, one can verify that the matter energy-momentum tensor is not conserved and the Einstein equivalence principle is violated [38]. Also, the total energy-momentum tensor is defined as
$$\begin{aligned} T^\mathrm{total}_{\mu \nu }=T_{\mu \nu }+T^{\phi }_{\mu \nu }+T^{\chi }_{\mu \nu }+T^{\psi }_{\mu \nu } \end{aligned}$$
where \(T_{\mu \nu }\) is the energy-momentum tensor for the ordinary matter, and
$$\begin{aligned} T^{\phi }_{\mu \nu }= & {} -\frac{\omega _0}{16\pi }\left( B_{\mu }^{~\alpha }B_{\nu \alpha }{-}g_{\mu \nu }\left( \frac{1}{4}B^{\rho \sigma }B_{\rho \sigma }{+}V_{\phi }\right) {+}2\frac{\partial V_{\phi }}{\partial g^{\mu \nu }}\right) \\ T^{\chi }_{\mu \nu }= & {} -\frac{1}{16\pi }\left( \nabla _{\mu }\chi \nabla _{\nu }\chi -\frac{1}{2} g_{\mu \nu }\nabla _{\alpha }\chi \nabla ^{\alpha }\chi \right) \\ T^{\psi }_{\mu \nu }= & {} -\frac{\chi ^2}{32 \pi }\left( \nabla _{\mu }\psi \nabla _{\nu }\psi -\frac{1}{2} g_{\mu \nu }\nabla _{\alpha }\psi \nabla ^{\alpha }\psi \right) . \end{aligned}$$
Furthermore, we assume a perfect fluid energy-momentum tensor for the ordinary matter. Also we consider the cosmological behavior of MOG in a flat Friedmann–Robertson–Walker (FRW) universe for which the line element is given by
$$\begin{aligned} \hbox {d}s^2=-\hbox {d}t^2+a(t)^2\left( \hbox {d}x^2+\hbox {d}y^2+\hbox {d}z^2\right) \end{aligned}$$
where a(t) is the cosmic scale factor. Now, by inserting this metric to the field Eqs. (2)–(5), and also noting the relation between \(\chi \), \(\psi \), and G, \(\mu \), we find the modified version of the Friedmann equations. The 00 component of (2) gives
$$\begin{aligned} \frac{\dot{a}^2}{a^2}= & {} \frac{8\pi G}{3}\rho +\frac{\varLambda }{3} \nonumber \\&+\left[ \frac{\dot{G}}{G}\frac{\dot{a}}{a}-\frac{1}{12}\frac{\dot{\mu }^2}{\mu ^2} -\frac{1}{24}\frac{\dot{G}^2}{G^2}+\frac{8\pi G}{3}\kappa \phi _0 \rho \right] \end{aligned}$$
where \(\phi _0(t)=-\phi ^0(t)\) is the zeroth covariant component of the vector field and \(\rho \) is the total energy density of the matter/radiation. Also a dot denotes the derivative with respect to time. The terms inside the bracket can be considered as corrections to the corresponding standard Friedmann equation. Using the equation of motion of the test particles in MOG (the generalized version of the geodesic equation in metric theories), one can find the action for pressure-less dust. Therefore, it can be shown that \(J^0=\kappa \rho \) (see [38] for more details). Here \(\kappa \) is another coupling constant. Although it seems that there are two independent coupling constants, \(\omega _0\) and \(\kappa \), they almost always appear as the combination \(\kappa ^2/\omega _0\) through the calculations of the physical quantities. Also it should be mentioned that because of the cosmological principle, the spatial components of \(J^{\alpha }\) and all components of antisymmetric tensor \(B_{\mu \nu }\) are zero. Furthermore the ii components of (2) take the following form:
$$\begin{aligned} \frac{\ddot{a}}{a}= & {} -\frac{4\pi G}{3}(\rho +3 p)+\frac{\varLambda }{3} \nonumber \\&+\left[ \frac{1}{2}\frac{\dot{G}}{G}\frac{\dot{a}}{a}+\frac{1}{6}\frac{\dot{\mu }^2}{\mu ^2}+\frac{1}{2}\frac{\ddot{G}}{G}\right. \nonumber \\&\left. -\frac{11}{12}\frac{\dot{G}^2}{G^2}-\frac{4\pi G}{3}\kappa \phi _0\rho -\frac{G\omega _0}{6} V_{\phi }\right] \end{aligned}$$
where p is the pressure of the cosmic fluid, and we have used Eq. (9) for terms including \(\dot{a}^2\). Equation (3), i.e. the field equation of the vector field, takes the following form:
$$\begin{aligned} \frac{\partial V_{\phi }}{\partial \phi _0}=\frac{16\pi \kappa }{\omega _0}\rho . \end{aligned}$$
Therefore the potential \(V_{\phi }\) should satisfy the following general criterion for all values of \(\mu (t)\) and \(\phi _0(t)\):
$$\begin{aligned} \frac{\omega _0}{\kappa }\frac{\partial V_{\phi }}{\partial \phi _0}\ge 0. \end{aligned}$$
Furthermore, Eq. (4) can be written as
$$\begin{aligned} \frac{\ddot{G}}{G}= & {} 32\pi G(1+\kappa \phi _0)\rho +12\frac{\ddot{a}}{a}+9\frac{\dot{G}}{G}\frac{\dot{a}}{a} \nonumber \\&-2\frac{\dot{\mu }^2}{\mu }+\frac{\dot{G}^2}{G^2}-2G\omega _0 V_{\phi }, \end{aligned}$$
and finally Eq. (5) reads
$$\begin{aligned} \frac{\ddot{\mu }}{\mu }=\frac{\dot{\mu }^2}{\mu ^2}-3\frac{\dot{\mu }}{\mu }\frac{\dot{a}}{a}+\frac{\dot{G}}{G}\frac{\dot{\mu }}{\mu }-G\omega _0\mu \frac{\partial V_{\phi }}{\partial \mu }. \end{aligned}$$
If the generic potential \(V_{\phi }\) and the equation of state \(p=p(\rho )\) are known, then Eqs. (9), (10), (11), (13), and (14) are five non-linear partial differential equations for five unknown functions a(t), \(\phi _0(t)\), \(\mu (t)\), G(t), and \(\rho (t)\). It is interesting to remark that the vector field is not “dynamical” in the sense that its field equation does not contain any time derivative. In other words, the vector field is algebraically related to the energy density \(\rho \).

3 Vacuum exact solution

Before starting the Noether symmetry approach, we consider the vacuum exact solution (\(\rho =0\) and \(\varLambda =0\)). In this case the modified Friedman equations can be analytically integrated for a wide range of generic potential \(V_{\phi }\). Let us rewrite Eqs. (9), (10), (11), (13), and (14), respectively, as
$$\begin{aligned} \frac{1}{12}\left( \frac{\mu '^2}{\mu ^2}+\frac{G'^2}{2G^2}\right) =\frac{G'}{G}-1, \end{aligned}$$
$$\begin{aligned} \frac{H'}{H}=\frac{G'}{G}-3, \end{aligned}$$
$$\begin{aligned} \mu ''=\frac{\mu '^2}{\mu }, \end{aligned}$$
$$\begin{aligned} G''=\frac{G'^2}{G} \end{aligned}$$
where \(H=\dot{a}/a\) and a prime denotes the derivative with respect to \(\ln a\). Also it should be mentioned that we have assumed that the Proca potential has the general form \(V_{\phi }=f_1(\mu )f_2(\phi _{\alpha }\phi ^{\alpha })\) where \(f_1\) and \(f_2\) are arbitrary functions. \(f_2\) satisfies \(f_2(0)=0\) and \(\frac{\hbox {d}f_2(0)}{\hbox {d}\phi _0}=0\). Note that in the absence of matter/radiation the vector field freezes out at a finite value. We have assumed models for which the vector field freezes at \(\phi _0=0\). This is the case for the original potential of MOG, i.e. \(V_{\phi }=-\frac{1}{2} \mu ^2 \phi ^{\alpha }\phi _{\alpha }\).
The exact solutions to Eqs. (15)–(18) are
$$\begin{aligned} G(t)=G_0\,a(t)^{\epsilon }, \end{aligned}$$
$$\begin{aligned} \mu (t)=\mu _0\,a(t)^{\frac{\pm \sqrt{24\epsilon -24-\epsilon ^2}}{\sqrt{2}}}, \end{aligned}$$
$$\begin{aligned} a(t)=(\epsilon _1\, t+\epsilon _2)^{\frac{1}{3-\epsilon }} \end{aligned}$$
where \(G_0\), \(\mu _0\), \(\epsilon \), \(\epsilon _1\), and \(\epsilon _2\) are constants of integration. One may consider this solution as a late time solution where the energy density of matter and radiation is zero. If \(2<\epsilon <3\) then we have an accelerated expansion, i.e. \(\ddot{a}>0\). In this case G(t) is an increasing function of time and \(\mu (t)\) can be decreasing or increasing. It is important to mention that this late time acceleration is not a de Sitter universe where the cosmic scale factor grows as \(a(t)\sim e^{\sqrt{\varLambda } t}\).

4 Canonical point-like Lagrangian for MOG

Equations (9), (10), (11), (13), and (14) can also be deduced from a canonical point-like Lagrangian \(\mathscr {L}(a,\dot{a},\chi ,\dot{\chi },\phi _0,\dot{\phi _0},\psi ,\dot{\psi })\). For notational simplicity, in this section we use \(\psi \) and \(\chi \) instead of \(\mu \) and G. The point-like Lagrangian \(\mathscr {L}\) is derived from the action (1). We denote the configuration space by \(\mathscr {Q}\equiv \lbrace a,\chi ,\psi ,\phi _0\rbrace \). Then \(\mathscr {TQ}\equiv \lbrace a,\dot{a},\chi ,\dot{\chi },\phi _0,\dot{\phi _0},\psi ,\dot{\psi }\rbrace \) is the corresponding tangent space where the Lagrangian \(\mathscr {L}\) is defined. On the other hand, the Euler–Lagrange equation of \(\mathscr {L}\) is
$$\begin{aligned}&\frac{\hbox {d}}{\hbox {d}t}\frac{\partial \mathscr {L}}{\partial \dot{q}}-\frac{\partial \mathscr {L}}{\partial q}=0,~~~ \frac{\hbox {d}}{\hbox {d}t}\frac{\partial \mathscr {L}}{\partial \dot{\phi _0}}-\frac{\partial \mathscr {L}}{\partial \phi _0}=16\pi a^3 \kappa \rho \end{aligned}$$
where q can be a, \(\chi \) or \(\psi \). Also the energy equation is
$$\begin{aligned} E_{\mathscr {L}}= \dot{a}\frac{\partial \mathscr {L}}{\partial \dot{a}}+\dot{\chi }\frac{\partial \mathscr {L}}{\partial \dot{\chi }}+\dot{\psi }\frac{\partial \mathscr {L}}{\partial \dot{\psi }}+\dot{\phi _0}\frac{\partial \mathscr {L}}{\partial \dot{\phi _0}}-\mathscr {L}=0; \end{aligned}$$
therefore, combining Eqs. (22) and (23), we have five equations which make a complete set of partial differential equations for five unknown functions.
In order to find \(\mathscr {L}\) one must insert the flat FRW metric into the action (1) and simplify the result using an integration by parts. Note that the Ricci scalar curvature takes the form \(R =6(\dot{a}^2/a^2+\ddot{a}/a)\). As a result, one can easily verify that, in a FRW manifold, the Lagrangian related to the action (1) takes the point-like form
$$\begin{aligned} \mathscr {L}= & {} 6\chi \dot{\chi }\dot{a}a^2+3a\dot{a}^2\chi ^2+\varLambda a^3\chi ^2+\frac{1}{2}a^3\dot{\chi }^2\nonumber \\&+\frac{1}{4}a^3\chi ^2\dot{\psi }^2-\omega _0 a^3 V_{\phi }+16\pi \rho a^3 \end{aligned}$$
where \(\rho =\rho _{m}+ \rho _r\) is the proper energy density. Here \(\rho _m\) is the matter energy density, and \(\rho _{r}\) is the radiation energy density. It is worth mentioning that, in general, the matter energy-momentum tensor in MOG is not conserved (see Eq. (A31) in [38]). However, in the case of FRW universe we have \(\nabla _{\mu }T^{\mu \nu }=0\) and consequently one can write \(\rho _m=\rho _{m0} \,a^{-3}\) and \(\rho _{r}=\rho _{r0}\,a^{-4}\), where \(\rho _{m0}\) and \(\rho _{r0}\) are the current values of the corresponding energy densities. The current magnitude of the cosmic scale factor has been normalized to unity. It is interesting that although there is a coupling between matter and the vector field, the energy-momentum tensor of the ordinary matter is conserved. This is an enormous simplification brought about by the cosmological principle.

Now by writing the Euler–Lagrange equations (22) for the Lagrangian (24), one can straightforwardly derive Eqs. (10)–(14). On the other hand, the energy condition (23) will give Eq. (9).

5 Noether symmetry approach

Now let us introduce the lift vector field \(\mathbf {X}\) [39]. \(\mathbf {X}\) is an infinitesimal generator of the Noether symmetry in the tangent space \(\mathscr {TQ}\), and it is defined as
$$\begin{aligned} X= & {} \alpha \frac{\partial }{\partial a}+\beta \frac{\partial }{\partial \chi }+\gamma \frac{\partial }{\partial \psi }+\xi \frac{\partial }{\partial \phi _0}+\dot{\alpha }\frac{\partial }{\partial \dot{a}}\nonumber \\&+\dot{\beta }\frac{\partial }{\partial \dot{\chi }}+\dot{\gamma }\frac{\partial }{\partial \dot{\psi }}+\dot{\xi }\frac{\partial }{\partial \dot{\phi _0}} \end{aligned}$$
where the functions \(\alpha \), \(\beta \), \(\gamma \), and \(\xi \) depend on the configuration space variables a, \(\chi \), \(\psi \), and \(\phi _0\). One can straightforwardly show that
$$\begin{aligned} \frac{\hbox {d}\Sigma }{\hbox {d}t}=L_{\mathbf {X}}\mathscr {L}+16\pi \xi a^3\kappa \rho \end{aligned}$$
where \(L_{\mathbf {X}}\mathscr {L}\) is the Lie derivative of the Lagrangian along the lift vector \(\mathbf {X}\), and \(\Sigma \) is defined as
$$\begin{aligned} \Sigma =\alpha \frac{\partial \mathscr {L}}{\partial \dot{a}}+\beta \frac{\partial \mathscr {L}}{\partial \dot{\chi }}+\gamma \frac{\partial \mathscr {L}}{\partial \dot{\psi }}. \end{aligned}$$
Therefore one may conclude that \(\Sigma \) is a conserved quantity if \(L_{\mathbf {X}}\mathscr {L}=-16\pi \xi a^3\kappa \rho \) (this is the Noether theorem). One needs to recall that in theories in which there is no coupling between matter and the gravitational fields, the right hand side of this criterion is zero. By applying this condition to the Lagrangian, the analytic form of the functions \(\alpha \), \(\beta \), \(\gamma \), and \(\xi \) will be specified. In fact, one may simply equate to zero the coefficients of terms like \(\dot{\psi }^2\), \(\dot{\chi }^2\), \(\dot{\psi }\dot{\chi }\), and so on in order to find some differential equations for the lift vector’s components. This is a common procedure in the relevant literature of the Noether symmetry approach; for example see [21, 22, 23, 24, 25, 26, 27, 28, 29, 30, 31, 32, 33, 34, 35]. Applying this procedure to the Lagrangian (24), we find the following differential equations:
$$\begin{aligned}&12\chi \frac{\partial \alpha }{\partial \psi }+12a\frac{\partial \beta }{\partial \psi }+\chi a^2\frac{\partial \gamma }{\partial a}=0,\nonumber \\&\beta a+\frac{a^2}{6}\frac{\partial \beta }{\partial a}+\chi ^2\frac{\partial \alpha }{\partial \chi }+a\chi \frac{\partial \beta }{\partial \chi }+a\chi \frac{\partial \alpha }{\partial a}+2\alpha \chi =0,\nonumber \\&\frac{3}{2}\alpha +6\chi \frac{\partial \alpha }{\partial \chi }+a\frac{\partial \beta }{\partial \chi }=0,\nonumber \\&\chi \alpha +2 a \chi \frac{\partial \alpha }{\partial a}+2 a \beta +2a^2\frac{\partial \beta }{\partial a}=0,\nonumber \\&3\alpha \chi +2a\chi \frac{\partial \gamma }{\partial \psi }+2a\beta =0,\nonumber \\&12\chi \frac{\partial \alpha }{\partial \psi }+2a\frac{\partial \beta }{\partial \psi }+a\chi ^2\frac{\partial \gamma }{\partial \chi }=0,\nonumber \\&\frac{\partial \gamma }{\partial \phi _0}=\frac{\partial \alpha }{\partial \phi _0}=\frac{\partial \beta }{\partial \phi _0}=\frac{\partial \xi }{\partial \phi _0}=0. \end{aligned}$$
Furthermore, there are some terms in \(L_{\mathbf {X}}\mathscr {L}\) which do not contain any time derivatives of configuration space variables. The summation of these terms should be separately zero:
$$\begin{aligned}&\left( 3\omega _0 V_{\phi }+16\pi \rho _r\right) \alpha -2\varLambda \chi a\left( \beta +\frac{3}{2}\frac{\chi }{a}\alpha \right) \nonumber \\&\quad +\omega _0 a \frac{\partial V_{\phi }}{\partial \psi }\gamma =0. \end{aligned}$$
It is obvious from Eq. (28) that the function \(\xi \) can be an arbitrary function of a, \(\chi \), and \(\psi \). In other words, the existence of the Noether symmetry does not restrict the functional form of \(\xi \). Therefore, one can construct an infinite number of symmetry generators for this cosmological model. It is also worth mentioning that there are nine differential equations in (28) which is enough for finding the exact form of \(\alpha (a,\chi ,\psi )\), \(\beta (a,\chi ,\psi )\), \(\gamma (a,\chi ,\psi )\). After finding these functions and inserting them into (29), we shall find the form of the generic potentials \(V_{\phi }\) for which the Noether symmetry exists. After some straightforward algebraic calculations, one can verify that the general solutions to Eq. (28) are
$$\begin{aligned} \alpha= & {} (\alpha _1\psi +\alpha _2)a\nonumber \\ \beta= & {} -\frac{3}{2}\frac{\chi }{a}\alpha ,\\ \gamma= & {} 6\alpha _1\ln \left( a\chi ^{-3/2}\right) +\alpha _3 \nonumber \end{aligned}$$
where \(\alpha _1\), \(\alpha _2\), and \(\alpha _3\) are integration constants. Although the Lagrangian (24) seems complicated, it possesses simple Noether symmetry generators. Furthermore, using the second equation in (30), the term containing the cosmological constant \(\varLambda \) vanishes in (29). Therefore, Eq. (29) can be rewritten as
$$\begin{aligned} V_{\phi }+\frac{16\pi \rho _{r}}{3\omega _0}+\frac{6\alpha _1\ln \left( a\chi ^{-3/2}\right) +\alpha _3}{3(\alpha _1\psi +\alpha _2)}\frac{\partial V_{\phi }}{\partial \psi }=0. \end{aligned}$$
In order to find the exact form of the potential \(V_{\phi }\) one needs to find the scale factor a(t) and the scalar field \(\chi \) with respect to \(\psi \) and \(\phi _0\). To do so, let us first derive the conserved quantity \(\Sigma \) associated to the Noether symmetry generator \(\mathbf {X}\). We recall that Noether’s theorem states that every symmetry of the Lagrangian implies the existence of a conservation law, and therefore a conserved quantity. Using the Lagrangian (24) and Eq. (27), we find
$$\begin{aligned} \Sigma =(9 a^2\chi \dot{\chi }-6\chi ^2\dot{a}a)\alpha +a^3\chi ^2\dot{\psi }\gamma . \end{aligned}$$
For the sake of simplicity we assume that \(\Sigma =0\). Thus one can easily verify that, when \(\alpha _1\ne 0\), we have
$$\begin{aligned} \ln (a\chi ^{-\frac{3}{2}})=\alpha _4\alpha _2-\frac{\alpha _3}{6\alpha _1}+\alpha _4\alpha _1\psi \end{aligned}$$
where \(\alpha _4\) is a new integration constant. When \(\alpha _1\) is zero (i.e. when \(\gamma \) is constant), it is easy to show that
$$\begin{aligned} \ln (a\chi ^{-\frac{3}{2}})=\alpha _4+\frac{\alpha _3}{6\alpha _2}\psi . \end{aligned}$$
Substituting these results into Eq. (31), we find
$$\begin{aligned} V_{\phi }+\frac{16\pi \rho _{r}}{3\omega _0}+A^{-1}\frac{\partial V_{\phi }}{\partial \psi }=0, \end{aligned}$$
where A is a constant and is equal to \(\frac{1}{2\alpha _1\alpha _4}\) when \(\alpha _1\ne 0\) and \(A=(3\alpha _2)/\alpha _3\) when \(\alpha _1\) is zero. It is important to note that, in principle, one may find the cosmic scale factor as a function of \(\frac{\partial V_{\phi }}{\partial \phi _0}\) from the field equation of the vector field (i.e. Eq. (11)). Therefore, Eq. (35) is a partial differential equation for the potential \(V_{\phi }(\phi _0,\psi )\). This equation will determine the general form of \(V_{\phi }\) for which the Noether symmetry exists.

5.1 The case \(\rho _r=0\) and \(\rho _m\), \(\varLambda \ne 0\)

In this case the energy budget consists of the cosmological constant \(\varLambda \), non-relativistic matter, the scalar fields G and \(\mu \), and the vector field \(\phi ^{\mu }\). Equation (35) takes a simple form and can easily be integrated. The result is
$$\begin{aligned} V_{\phi }(\mu ,\phi _0)=f(\phi _0)\mu ^{-A} \end{aligned}$$
where \(f(\phi _0)\) is an arbitrary function of \(\phi _0\), and we have used \(\psi (t)=\ln (\mu (t))\). This potential covers a wide range of potentials. For example the original potential of MOG, i.e. \(V_{\phi }=-\frac{1}{2}\mu ^2 \phi _{\nu }\phi ^{\nu }\) [1], lies in this subclass. Another, straightforward example is
$$\begin{aligned} V_{\phi }(\mu ,\phi ^{\alpha })=V_0 \mu ^n\left( -\phi _{\nu }\phi ^{\nu }\right) ^{m/2}, \end{aligned}$$
which in an isotropic and homogeneous space-time takes the form \(V_{\phi }=V_0 \mu ^n\phi _0^m\). Also, it is obvious that if \(\alpha _2\)=0 (or equivalently \(A=0\)) then \(V_{\phi }\) is a function of the vector field and does not depend on the scalar field \(\mu \). More importantly, every function of \(\phi _{\mu }\phi ^{\mu }\) is a solution.

5.2 The case \(\rho _m=0\) and \(\rho _r\), \(\varLambda \ne 0\)

In this case, we rewrite Eq. (35) as follows:
$$\begin{aligned} V_{\phi }+\frac{1}{3\kappa }\frac{\partial V_{\phi }}{\partial \phi _0}+A^{-1}\frac{\partial V_{\phi }}{\partial \psi }=0, \end{aligned}$$
and the general form of the solution is
$$\begin{aligned} V_{\phi }=f(y)\mu ^{-A}, \end{aligned}$$
in which \(y=\exp (\phi _0)\mu ^{-A/3\kappa }\), and f is an arbitrary function of y. Simple examples of this class of potentials are \(V_{\phi }=V_0 \mu ^{\lambda _1}\) and \(V_{\phi }=V_0 \exp (\lambda _1 \sqrt{-\phi _{\alpha }\phi ^{\alpha }})\mu ^{\lambda _2}\).

6 Cosmological exact solutions for MOG

Now we present some new exact cosmological solutions to MOG’s modified Friedmann equations. Also we restrict ourselves to solutions with zero radiation density. We recall that by setting the Noether constant of motion \(\Sigma \) to zero, we found Eqs. (33) and (34). Let us rewrite these equations as
$$\begin{aligned} a(t)=c G(t)^{-3/4}\mu (t)^{1/2A} \end{aligned}$$
where c is a constant. This is a key equation to derive exact solutions. Using this equation we find some solutions for specific potentials introduced in the previous sections as potentials for which the Noether symmetry exists.

6.1 Model \(V_{\phi }=\lambda _0 \mu (t)^{2q}\), \(\rho _m=\rho _r=\varLambda =0\)

Here \(\lambda _0\) is a constant. We have used a new parameter q instead of A as \(A=-2q\). This model corresponds to a scalar–tensor theory with two scalar fields \(\mu (t)\) and G(t). In fact, since the matter and radiation are absent in the model, there is no source for producing the vector field. With the aid of Eq. (40) and assuming a power-law type solutions for the scalar fields as \(\mu (t)=\mu _0 t^n\) and \(G(t)=G_0 t^m\), we find the following exact solution:
$$\begin{aligned}&a(t)= a0\,{t}^{ \frac{1}{4-20\,{q}^{2}}},\nonumber \\&G(t)=G0\,{t}^{ \frac{2}{5\,{q}^{2}-1}},\\ \nonumber&\mu (t)=\mu _0\,{t}^{{\frac{5q}{1-5\,{q}^{2}}}} \end{aligned}$$
where \(G_0\) is related to other constants as
$$\begin{aligned} G_0=-\frac{5}{8}\,{\frac{20\,{q}^{2}+7}{\omega _0\,\lambda _0\,{ \mu _0}^{2q} \left( 25\,{q}^{4}-10\,{q}^{2}+1 \right) }}. \end{aligned}$$
One can easily show that this solution corresponds to an accelerated expansion (i.e. \(\ddot{a}>0\) and \(\dot{a}>0\)) if \(\sqrt{3/20}<q<1/\sqrt{5}\) or \(-1/\sqrt{5}<q<-\sqrt{3/20}\). In this case, the magnitude of the scalar G(t) decreases with time and for \(\mu (t)\) increases.

This solution has an interesting feature: the model can be contracting (i.e. \(\dot{a}<0\)) while \(\ddot{a}>0\). This situation happens when \(q>1/\sqrt{5}\) or \(q<-1/\sqrt{5}\). In this case \(\mu (t)\) is a decreasing function of time and G(t) is increasing. In fact, the existence of the scalar fields \(\mu (t)\) and G(t) can lead to a repulsive gravitational force in the early universe.

6.2 Model \(V_{\phi }=-\frac{1}{2}\mu ^2 \phi _{\alpha }\phi ^{\alpha }\), \(\rho _r=\varLambda =0\), and \(\rho _m\ne 0\)

As we have already mentioned, this potential is the original potential postulated in MOG [1]. For this model we use Eq. (40) and also assume a power-law type solution for G(t) and \(\mu (t)\). One can easily verify the following exact solution:
$$\begin{aligned} a(t)= & {} \root 3 \of {{\frac{544}{9}}\,{\frac{\pi \,\alpha _0 G_N{ \rho _{m0}}}{{{ \mu _0}}^{2}{}}}}{t}^{{\frac{12}{23}}},\nonumber \\ G(t)= & {} {\frac{2312}{207}}\,\frac{\alpha _0 G_N}{{{ \mu _0}}^{2}}{ t}^{-{\frac{10}{23}}}, \nonumber \\ \mu (t)= & {} { \mu _0}{t}^{-{\frac{18}{23}}},\nonumber \\ \kappa \phi _0(t)= & {} {\frac{9}{34}},\\ \nonumber \rho _m(t)= & {} {\frac{9}{544}}\,\frac{\mu _0^{2}}{\pi \,\alpha _0 G_N}{t}^{-{\frac{36}{23}}} \end{aligned}$$
where \(\alpha _0=\kappa ^2/\omega _0 G_N\) is one of the free parameters of MOG, and \(G_N\) is the gravitational constant. Its observational value is \(\alpha _0=8.89\pm 0.34\) [12]. One can easily verify that the condition (12) is satisfied. It is obvious that the “velocity” of the vector field is zero and the field’s value remains constant in this matter dominated phase. Also this solution corresponds to a decelerating universe. If we compare this solution with the matter dominated universe in GR (flat FRW space-time with \(\varLambda =0\)) where \(a(t)\sim t^{2/3}\), then we see that the scale factor increases more slowly than the standard Friedman model. Thus the matter density also decreases with a slower rate.

6.3 Model \(V_{\phi }=V_0\,\mu \, \phi _{\alpha }\phi ^{\alpha }\), \(\rho _r=\varLambda =0\), and \(\rho _m\ne 0\)

Here \(V_0\) is a constant. With the aid of Eq. (40), one may easily verify the following solution:
$$\begin{aligned} a(t)= & {} { a_0}\,{t}^{-\frac{1}{3}\,m},\nonumber \\ G(t)= & {} { G_0}\,{t}^{-2-m},\nonumber \\ \mu (t)= & {} {\frac{{\kappa }^{2} \left( 3\,\pi \,m+10\,\pi \right) ^{2}}{{ 4 G_0}\,{\pi }^{2}{ V_0}\,m{ \omega _0}}}{t}^{m},\\ \nonumber \kappa \phi _0(t)= & {} -\,{\frac{2\,\pi \,m}{ \left( 3\,\pi \,m+10\,\pi \right) }},\\ \nonumber \rho _m(t)= & {} {\frac{3\,\pi \,m+10\,\pi }{{16\, G_0}\,{\pi }^{2} }} {t}^{m} \end{aligned}$$
where m can have two values: \(m=-18/7\) and \(m=-3\), and \(G_0\) is related to the other constants as
$$\begin{aligned} G_0={\frac{ \left( 3\,\pi \,m+10\,\pi \right) {{a_0}}^{3}}{{16\,\rho _{m0}}\,{\pi }^{2}}}>0; \end{aligned}$$
it is worth mentioning that the condition (12) holds if \(G_0>0\). As we see the vector field is again constant. Also, the existence of two different values for m shows that our power-law type solutions are not the complete and unique solutions to the cosmological field equations. For \(m=-3\) the cosmic scale factor increases linearly with time and so is without deceleration, i.e. \(\ddot{a}=0\). Therefore the scale factor increases faster than the standard matter dominated Friedmann model. Also we recall that in GR, for a matter dominated universe with flat spatial curvature and zero cosmological constant, \(\ddot{a}\) cannot vanish.

For \(m=-18/7\) the scale factor increases as \(a(t)\sim t^{6/7}\). Therefore the scale factor increases faster than the standard case. However, unlike the case \(m=-3\), we have a negative acceleration (\(\ddot{a}<0\)). As a final remark for this solution, we mention that the repulsive nature of the theory is again evident. In other words, the combination of the scalar fields and the vector field MOG can yield a repulsive gravitational force at the cosmological scale.

6.4 Model \(V_{\phi }=V_0\root m \of {-\phi _{\alpha }\phi ^{\alpha }}\mu ^n \), \(\rho _r=\varLambda =0\), and \(\rho _m\ne 0\)

Here m and n are real constants, and \(m\ne 0,1,2\). Therefore this model is different from those presented in the previous subsections. Again, by using Eq. (40) which was obtained from the conserved quantity of the Noether symmetry, we find the following solution:
$$\begin{aligned} a(t)= & {} a_0\,t^2,\nonumber \\ G(t)= & {} G_0\,t^4,\nonumber \\ \mu (t)= & {} \mu _0\,t^K, \\ \kappa \phi _0(t)= & {} \kappa \varPhi _0=\frac{m}{(2-m)},\nonumber \\ \rho _{m}(t)= & {} \frac{5\,(2-m)}{8\pi G_0}\frac{1}{t^6}\nonumber \end{aligned}$$
where \(K=\pm 2\sqrt{15}\) corresponding to \(n=\mp \sqrt{15}/5\) and the relations between constants are
$$\begin{aligned} V_0=\frac{10\,\mu _0^{K/10}\,\varPhi _0^{-m}}{\omega _0\, G_0},~G_0=\frac{5\,(2-m)\,a_0^3}{8\,\pi \,\rho _{m0}}. \end{aligned}$$
The criterion (12) leads to \((2-m)/G_0>0\). If we assume that \(G_0>0\) (note that G(t) is related to the gravitational constant), then everything is well defined provided that \(m<2\). It is interesting that this solution represents a constant acceleration for the cosmic expansion. We mention again that such a behavior is not achievable in the corresponding standard Friedmann model. As is clear from Eq. (46), the scalar field G(t) is an increasing function of time, and the scalar field \(\mu (t)\) depending on the value of parameter K can be an increasing function of time or a decreasing one. However, the rate of the expansion is independent of the behavior of \(\mu (t)\).

It is worth mentioning that G is a non-minimal scalar field. As we have already mentioned, non-minimal scalar–tensor theories have already been investigated using the Noether symmetry approach; for example see [23]. Although there is an extra vector field in MOG, which is coupled to the matter distribution, there are some similarities between the exact solutions of these theories. For example the exact solution presented in this subsection is reminiscent of the exact solution obtained in Eq. (6.42) of [23].

6.5 Model \(V_{\phi }=-\frac{1}{2}\mu ^2\,\phi ^{\alpha }\phi _{\alpha }+\frac{\mu ^2}{\kappa }\sqrt{-\phi ^{\alpha }\phi _{\alpha }}+\frac{\mu ^2}{2\kappa } \), \(\rho _r=\varLambda =0\), and \(\rho _m\ne 0\)

In this case, we found the exact solution:
$$\begin{aligned} a(t)= & {} a_0\,{t}^{-{\frac{11}{30}}\,m+\frac{1}{3}},\nonumber \\ G(t)= & {} G_0\,t^{-\frac{m}{5}},\nonumber \\ \mu (t)= & {} \mu _0\,t^{m}, \\ \kappa \phi _0(t)= & {} -1-{\frac{3\,m \sqrt{\alpha _0 G_N}}{\sqrt{10\,{G_0}\,{{\mu _0}}^{2}}}}\,{t}^{-{\frac{9}{10}}\,m-1},\nonumber \\ \rho _m(t)= & {} \frac{\rho _{m0}}{a_0^3}\,t^{\frac{11}{10}\,m-1},\nonumber \end{aligned}$$
where \(m=5/4\) or \(-20/11\) and
$$\begin{aligned} a_0=\frac{2}{3}\sqrt{2}\,3^{2/3}\,5^{1/6}\,\root 6 \of {\,{\frac{{G_0}\,\alpha _0 G_N{\pi }^{2}{{\rho _{m0}}}^{2}}{{m}^{2}{\mu _0}}}}. \end{aligned}$$
The condition (12) is satisfied if \(\mu _0>0\) and \(G_0>0\). For \(m=5/4\) the scale factor decreases as \(a(t)\sim t^{-9/8}\), and so \(\dot{a}<0\) and \(\ddot{a}>0\). However, for \(m=-20/11\) the scale factor grows as \(a(t)\sim t\).

7 Conclusion

In this paper we have studied the cosmology of a specific scalar–vector–tensor theory of gravity known as MOG using a well-known approach. We have found the Noether symmetry generators and also the conserved quantity associated to the symmetry. More specifically, this approach helped us to find the explicit form of the vector field potential \(V_{\phi }\) [see Eqs. (36) and (39)]. We showed that the original potential postulated in this theory is one of the potentials for which the Noether symmetry exists. Also, using the conserved quantity associated to the Noether symmetry, we have found some exact solutions for the modified Friedmann equations of MOG. We have found five sets of exact solutions and, except for one of them, we have not neglected the ordinary matter contribution. More specifically, our solutions correspond to matter dominated universes. As we mentioned before, power-law type exact solutions are not necessarily unique. However, these solutions are very often used in cosmological theories in order to gain insight into the physical content of them. In the context of MOG, there are some interesting features in the exact solutions which may help to understand the cosmological behavior of this theory. For example, the existence of the scalar and vector fields in MOG can lead to a contracting universe with positive acceleration. In other words, these fields can behave like a repulsive gravitational force at the cosmological scales. Also, there exist some solutions for which the “gravitational constant” [the scalar field G(t)] increases with time as well as solutions where G(t) is decreasing.



This work is supported by Ferdowsi University of Mashhad under Grant No. 2/32649 (21/11/1393). The author thanks Sarah Jamali for pointing out an error in a previous version of this paper.


  1. 1.
    J.W. Moffat, JCAP 0603, 004 (2006)MathSciNetCrossRefADSGoogle Scholar
  2. 2.
    C.H. Brans, R.H. Dicke, Phys. Rev. 124, 925 (1961)MathSciNetCrossRefADSGoogle Scholar
  3. 3.
    S. Capozziello, M. De Laurentis, Phys. Rep. 509, 167 (2011)MathSciNetCrossRefADSGoogle Scholar
  4. 4.
    T. Jacobson, D. Mattingly, Phys. Rev. D 64, 024028 (2001)MathSciNetCrossRefADSGoogle Scholar
  5. 5.
    E.A. Lim, Phys. Rev. D 71, 063504 (2005)CrossRefADSGoogle Scholar
  6. 6.
    P. Fleury, J.P.B. Almeida, C. Pitrou, J.P. Uzan, JCAP 1411(11), 043 (2014)CrossRefADSGoogle Scholar
  7. 7.
    J.D. Bekenstein, Phys. Rev. D 70, 083509 (2004)CrossRefADSGoogle Scholar
  8. 8.
    M. Milgrom, Astrophys. J. 270, 365 (1983)CrossRefADSGoogle Scholar
  9. 9.
    J.R. Brownstein, J.W. Moffat, Astrophys. J. 636, 721 (2006)CrossRefADSGoogle Scholar
  10. 10.
    J.R. Brownstein, J.W. Moffat, Mon. Not. R. Astron. Soc. 382, 29 (2007)CrossRefADSGoogle Scholar
  11. 11.
    J.R. Brownstein, J.W. Moffat, Mon. Not. R. Astron. Soc. 367, 527 (2006)CrossRefADSGoogle Scholar
  12. 12.
    J.W. Moffat, S. Rahvar, Mon. Not. R. Astron. Soc. 436, 1439 (2013)CrossRefADSGoogle Scholar
  13. 13.
    J.W. Moffat, S. Rahvar, Mon. Not. R. Astron. Soc. 441, 3724 (2014)CrossRefADSGoogle Scholar
  14. 14.
    J.W. Moffat, V.T. Toth, Astrophys. J. 680, 1158 (2008)CrossRefADSGoogle Scholar
  15. 15.
    J.W. Moffat, V.T. Toth, Phys. Rev. D 91, 043004 (2015)CrossRefADSGoogle Scholar
  16. 16.
    J.W. Moffat, V.T. Toth. arXiv:0710.0364
  17. 17.
    J.W. Moffat, Int. J. Mod. Phys. D 16, 2075 (2008)CrossRefADSGoogle Scholar
  18. 18.
    J.W. Moffat, V.T. Toth, Class. Quantum Grav. 26, 085002 (2009)MathSciNetCrossRefADSGoogle Scholar
  19. 19.
    J.W. Moffat, V.T. Toth, Galaxies 1, 65 (2013)CrossRefADSGoogle Scholar
  20. 20.
    J.W. Moffat. arXiv:1409.0853
  21. 21.
    R. de Ritis, G. Marmo, G. Platania, C. Rubano, P. Scudellaro, C. Stornaiolo, Phys. Rev. D 42, 1091 (1990)MathSciNetCrossRefADSGoogle Scholar
  22. 22.
    S. Capozziello, R. de Ritis, Class. Quantum Grav. 11, 107 (1994)Google Scholar
  23. 23.
    S. Capozziello, R. De Ritis, C. Rubano and P. Scudellaro, Riv. Nuovo Cim. 19N4, 1 (1996)Google Scholar
  24. 24.
    S. Capozziello, M. Laurentis, S.D. Odintsov, Eur. Phys. J. C 72, 2068 (2012)CrossRefADSGoogle Scholar
  25. 25.
    Yusuf Kucukakca, Eur. Phys. J. C 74, 3086 (2014)CrossRefADSGoogle Scholar
  26. 26.
    F. Darabi, K. Atazadeh, A. Rezaei-Aghdam, Eur. Phys. J. C 73, 2657 (2013)CrossRefADSGoogle Scholar
  27. 27.
    U. Camci, Eur. Phys. J. C 74, 3201 (2014)CrossRefADSGoogle Scholar
  28. 28.
    K. Atazadeh, F. Darabi, Eur. Phys. J. C 72, 2016 (2012)CrossRefADSGoogle Scholar
  29. 29.
    H. Motavali, S. Capozziello, M. Rowshan Almeh Jog, Phys. Lett. B 666, 10 (2008)Google Scholar
  30. 30.
    A. Paliathanasis, M. Tsamparlis, S. Basilakos, S. Capozziello, Phys. Rev. D 89(6), 063532 (2014)CrossRefADSGoogle Scholar
  31. 31.
    S. Basilakos, S. Capozziello, M. De Laurentis, A. Paliathanasis, M. Tsamparlis, Phys. Rev. D 88, 103526 (2013)CrossRefADSGoogle Scholar
  32. 32.
    B. Vakili, Phys. Lett. B 738, 488 (2014)MathSciNetCrossRefADSGoogle Scholar
  33. 33.
    B. Vakili, Phys. Lett. B 664, 16 (2008)MathSciNetCrossRefADSGoogle Scholar
  34. 34.
    M. Roshan, F. Shojai, Phys. Lett. B 668, 238 (2008)MathSciNetCrossRefADSGoogle Scholar
  35. 35.
    S.A. Hojman, J. Phys. A. Math. Gen. 25, L291 (1992)Google Scholar
  36. 36.
    S. Capozziello, M. Roshan, Phys. Lett. B 726, 471 (2013)MathSciNetCrossRefADSGoogle Scholar
  37. 37.
    M. Roshan, S. Abbassi, Phys. Rev. D 90, 044010 (2014)CrossRefADSGoogle Scholar
  38. 38.
    M. Roshan, Phys. Rev. D 87(4), 044005 (2013)CrossRefADSGoogle Scholar
  39. 39.
    G. Marmo, E.J. Saletan, A. Simoni, B. Vitale, Dynamical Systems. A Differential Geometric Approach to Symmetry and Reduction (Wiley, New York, 1985)MATHGoogle Scholar

Copyright information

© The Author(s) 2015

Open AccessThis article is distributed under the terms of the Creative Commons Attribution 4.0 International License (, which permits unrestricted use, distribution, and reproduction in any medium, provided you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons license, and indicate if changes were made.

Funded by SCOAP3

Authors and Affiliations

  1. 1.Department of PhysicsFerdowsi University of MashhadMashhadIran

Personalised recommendations