Accelerated FRW solutions in Chern–Simons gravity

We consider a five-dimensional Einstein–Chern–Simons action which is composed of a gravitational sector and a sector of matter where the gravitational sector is given by a Chern–Simons gravity action instead of the Einstein–Hilbert action and where the matter sector is given by the so-called perfect fluid. It is shown that (i) the Einstein–Chern–Simons (EChS) field equations subject to suitable conditions can be written in a similar way to the Einstein–Maxwell field equations; (ii) these equations have solutions that describe an accelerated expansion for the three possible cosmological models of the universe, namely, spherical expansion, flat expansion, and hyperbolic expansion when α\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$\alpha $$\end{document}, a parameter of the theory, is greater than zero. This result allows us to conjecture that these solutions are compatible with the era of dark energy and that the energy–momentum tensor for the field ha\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$h^{a}$$\end{document}, a bosonic gauge field from the Chern–Simons gravity action, corresponds to a form of positive cosmological constant. It is also shown that the EChS field equations have solutions compatible with the era of matter: (i) In the case of an open universe, the solutions correspond to an accelerated expansion (α>0\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$\alpha >0$$\end{document}) with a minimum scale factor at initial time that, when time goes to infinity, the scale factor behaves as a hyperbolic sine function. (ii) In the case of a flat universe, the solutions describe an accelerated expansion whose scale factor behaves as an exponential function of time. (iii) In the case of a closed universe there is found only one solution for a universe in expansion, which behaves as a hyperbolic cosine function of time.


Introduction
Some time ago it was shown that standard, five-dimensional General Relativity can be obtained from Chern-Simons gravity theory for a certain Lie algebra B [1], whose generators { J ab , P a , Z ab , Z a } satisfy the commutation relationships This algebra was obtained from the anti-de Sitter (AdS) algebra and a particular semigroup S by means of the S-expansion procedure introduced in Refs. [2,3].
In order to write down a Chern-Simons Lagrangian for the B algebra, we start from the one-form gauge connection and the two-form curvature Consistency with the dual procedure of S-expansion in terms of the Maurer-Cartan forms [3] demands that h a inherits the unit of length from the fünfbein; that is why it is necessary to introduce the l parameter again, this time associated with h a .
It is interesting to observe that J ab are still Lorentz generators, but P a are no longer AdS boosts; in fact, [ P a , P b ] = Z ab . However, e a still transforms as a vector under Lorentz transformations, as it must, in order to recover gravity in this scheme.
A Chern-Simons Lagrangian in d = 5 dimensions is defined to be the following local function of a one-form gauge connection A: where · · · denotes an invariant tensor for the corresponding Lie algebra, F = d A + AA is the corresponding two-form curvature and k is a constant [4]. Using theorem VII.2 of Ref. [2], it is possible to show that the only non-vanishing components of an invariant tensor for the B algebra are given by J a 1 a 2 J a 3 a 4 P a 5 = α 1 4l 3 3 a 1 ···a 5 , J a 1 a 2 Z a 3 a 4 P a 5 = α 3 4l 3 3 where α 1 and α 3 are arbitrary independent constants of dimensions length −3 .
Using the extended Cartan homotopy formula as in Ref. [5], and integrating by parts, it is possible to write down the Chern-Simons Lagrangian in five dimensions for the B algebra as L (5) EChS = α 1 l 2 abcde e a R bc R de + α 3 abcde 2 3 R ab e c e d e e +2l 2 k ab R cd T e +l 2 R ab R cd h e + dB (4) EChS (5) where the surface term B (4) EChS is given by  (6) and where α 1 , α 3 are parameters of the theory, l is a coupling constant, R ab = dω ab +ω a c ω cb corresponds to the curvature two-form in the first-order formalism related to the one-form spin connection [4,6,7], and e a , h a , and k ab are the other gauge fields present in the theory [1].
From (5) we can see that the third term is a surface term and can be removed from this Lagrangian. Thus L (5) EChS = α 1 l 2 ε abcde R ab R cd e e + α 3 abcde 2 3 R ab e c e d e e +2l 2 k ab R cd T e +l 2 R ab R cd h e is the Einstein-Chern-Simons Lagrangian studied in Ref. [1]. The absence should be noted of kinetic terms for the fields h a and k ab in (7). The kinetic terms for the h a and k ab fields are present in the surface term of the Lagrangian (5) given by (6).
The Lagrangian (7) shows that standard, five-dimensional General Relativity emerges as the l → 0 limit of a CS theory for the generalized Poincaré algebra B. Here l is a length scale, a coupling constant that characterizes different regimes within the theory. The B algebra, on the other hand, is constructed from the AdS algebra and a particular semigroup S by means of the S-expansion procedure. The field content induced by the B algebra includes the vielbein e a , the spin connection ω ab , and two extra bosonic fields h a and k ab , which can be interpreted as boson fields coupled to the field curvature and the parameter l 2 can be interpreted as a kind of coupling constant.
Recently was found [8] that the standard five-dimensional FRW equations and some of their solutions can be obtained, in a certain limit, from the so-called Chern-Simons-FRW field equations, which are the cosmological field equations corresponding to a Chern-Simons gravity theory.
It is the purpose of this paper to show that the Einstein-Chern-Simons (EChS) field equations, subject to (i) the torsion-free condition (T a = 0), and (ii) the variation of the matter Lagrangian with respect to (w.r.t.) the spin connection is zero (δL M /δω ab = 0), can be written in a similar way to the Einstein-Maxwell field equations. The interpretation of the h a field as a perfect fluid allow us to show that the Einstein-Chern-Simons field equations have a universe in accelerated expansion as one of their solutions. This paper is organized as follows: In Sect. 2 we briefly review the Einstein-Chern-Simons field equations. In Sect. 3 we study the Einstein-Chern-Simons field equations in the range of validity of General Relativity. In Sect. 5 we consider accelerated solutions for the Einstein-Chern-Simons field equations. We try to find solutions that describe accelerated expansion for the cases of open universes, flat universes, and closed universes. In Sect. 6 we consider the consistency of the solutions with the "era of matter". A summary and an appendix conclude this work.

Einstein-Chern-Simons field equations
In Ref. [8] it was found that in the presence of matter the Lagrangian is given by where L (5) ChS is the five-dimensional Chern-Simons Lagrangian given by (7), L M = L M (e a , h a , ω ab ) is the matter Lagrangian, and κ is a coupling constant related to the effective Newton constant. The variation of the Lagrangian (8) w.r.t. the dynamical fields vielbein e a , spin connection ω ab , h a , and k ab , leads to the following field equations: For simplicity, we will assume that the torsion vanishes (T a = 0) and k ab = 0. In this case (9)-(12) take the form This field equations system can be written in the form where we introduce κ 5 = κ/8α 3 and α = −α 1 /α 3 . The field equation (9) contains three terms. The first one is proportional to the Einstein tensor. The second one corresponds to a quadratic term in the curvature, and a third one, a term that describes the dynamics of the field k ab . Since we assume k ab = 0 the last term in left side of (9) vanishes.
In order to write this field equation manner analogous to Einstein's equations, one chooses to leave the term proportional to the Einstein tensor on the left side of (9), and using (14) we obtain (17). This result allows us to interpret δL M /δh a as the energymomentum tensor for a second type of matter, not ordinary.
Henceforth we will say that δL M /δh a corresponds to the energy-momentum tensor for the field h a .
The equation of motion for the h a -field is given by (19). The condition δL M /δω ab = 0 (usual in gravity theories), imposed for consistency with the condition T a = 0, leads to the equation of motion (22) for the h a -field. This means that h a -field is governed by the following field equations: This means that the Einstein-Chern-Simons field equations, subject to the conditions T a = 0, k ab = 0, and δL M /δω ab = 0, can be rewritten in a way similar to the Einstein-Maxwell field equations.
From (20) to (22) we can see that if L M = 0, then in five dimensions there is no solution of Schwarzschild type [1,9].
Introducing (23) into (20) we obtain the Einstein field equation ε abcde R ab e c e d ≈ 4κ 5 δL M δe e .
If R ab is not large then δL M /δe a is also not large. This means that General Relativity can be seen as a low energy limit of Einstein-Chern-Simons gravity. Thus, in the range of validity of General Relativity, (20)-(22) are given by On the another hand, if R ab is large enough, so that when it is multiplied by l 2 (which is very small) it will have nonnegligible results, then we will find that δL M /δh a is not negligible. This means that, in this case, we must consider the entire system of (20)-(22).

Einstein-Chern-Simons field equations for a Friedmann-Robertson-Walker-like spacetime
The shape of the field e a is obtained from of the application of the cosmological principle to the metric tensor of spacetime: it is considered a splitting of the 5D-manifold in a maximally symmetric four-dimensional manifold and one temporal dimension (M = R × 4 ). This leads to a fivedimensional Friedmann-Robertson-Walker (FRW) metric. Thus the vielbein can be chosen like in [8]: The application of the cosmological principle to the metric tensor of the spacetime also constrains the shape of the field h a (see for example [8]). A detailed discussion can be also found in Ref. [10]. The bosonic field h a is given by where h(0) is a constant and h(t) is a function of time t, which must be determined. Substituting (28) into (22) we obtain the explicit form of the equations of motion for the h a -field, which will be displayed in (39).
In accordance with (20), we will consider a fluid composed of two perfect fluids, the first one related to ordinary energymomentum tensor (T μν ∼ δL M δe a ) and the second one related to the field h a (T The energy-momentum tensors in the comoving frame are given by where ρ is the matter density and p is the pressure of fluid. Then the energy-momentum tensor for the composed fluid is = diag(ρ,p,p,p,p).
In the torsion-free case, the energy-momentum tensor of ordinary matter satisfies a conservation equation and the Einstein tensor has also a zero divergence. In this case the energy-momentum tensor for the non-ordinary matter must also satisfy a conservation equation. In fact, from (20) we find Introducing (27)-(33) into (20)-(22) we find the following field equations (see Ref. [8] and Appendix A): We should note that (35) was studied in Ref. [11] in the context of inflationary cosmology.
Equations (35) and (36) are very similar to the Friedmann equations in five dimensions. However, now ρ and p are subject to restrictions imposed by the remaining equations.

Accelerated solution for Einstein-Chern-Simons field equations
In order to recover the known results of the standard cosmology in the context of accelerated expansion we use the approach This approach is analogous to the case when, in the era of dark energy, the energy-momentum tensor is neglected compared to the cosmological constant. This means that the contribution from the ordinary matter is negligible compared to the contribution from the field h a . In this case, the energymomentum tensorT μν of the fluid is given bỹ and (35)-(39) take the form 5.1 Case T μν = 0 and k = −1 which can be rewritten Consider the solutionä = 0, i.e., a solution without accelerated expansion. For the first term in the left side of (47) we havė The solution is In this case a(t) increases linearly, i.e., there is no accelerated expansion. Substituting this solution into (41)-(44) we find and (45) is satisfied for h(t) arbitrary.
Consider the case where the constant α is positive. Using the following ansatz 1 where t is a constant of integration, we obtain and therefore the initial condition a 0 = a(t = t 0 ) leads to This result shows that if α > 0, then there is an accelerated expansion (see Fig. 1). On the another hand, from (56) and (57) we can see thaẗ substituting (56), (57), and (58) into (41)-(44) we obtain 1 This ansatz can be obtained froṁ using a hyperbolic substitution i.e., we have an accelerated expansion when the energy density is positive and pressure is negative (like a positive cosmological constant). From Integrating, we find where C is a constant of integration. The initial condition Consider now the case when the constant α is negative. The ansatz with t a constant of integration, leads to therefore The initial condition a 0 = a(t = t 0 ) leads to Therefore if a(t) > 0 thenä(t) < 0, which shows that if α < 0, then there is a decelerated expansion (see Fig. 2).
On the another hand, substituting (65) and (66) into (41)-(44) we obtain Since the energy-momentum tensor is given bỹ we find that the corresponding energy density and pressure are (α < 0) i.e., the energy density is negative and the pressure is positive (like a negative cosmological constant).
Integrating, we find where C is a constant of integration. The initial condition 5.2 Case T μν = 0 and k = 0 Introducing (43) into (41) and considering k = 0, we obtain which can be rewritten as The solution for an static universe is given by which leads to and (45) is satisfied for all h(t).
In this case we have an expanding universe, The initial condition a 0 = a(t 0 ) leads to and Substituting (80) into (45), solving for h(t) and using the initial condition h 0 = h(t 0 ), we find In this case it is not possible to find a solution.
In this case it is not possible to find a solution.
From (84) we can see two cases.
If α > 0 we can postulate a solution given by where t is a constant of integration, which leads to The initial condition a 0 = a(t = t 0 ) leads to which shows an accelerated expansion (see Fig. 3). Substituting (87) and (88) into (41)-(44) we obtain i.e., we have an accelerated expansion when the energy density is positive and the pressure is negative (like a positive cosmological constant).
From (45) we find so that where C is a constant of integration. The initial condition from which we can see that h(t) → h(0) when t → ∞.  Table 3 Solutions for scale factor of a closed space, k = 1 If α < 0 (84) has no solution.

Era of dark energy from Einstein-Chern-Simons gravity
The results in the previous section are summarized in Tables 1, 2, and 3. Thus we have found solutions that describe accelerated expansion for the three possible cosmological models of the universe. Namely, spherical expansion (k = 1), flat expansion (k = 0), and hyperbolic expansion (k = −1) when the constant α is greater than zero. This means that the Einstein-Chern-Simons field equations have as one of their solutions a universe in accelerated expansion. This result allows us to conjecture that these solutions are compatible with the era of dark energy and that the energy-momentum tensor for the field h a corresponds to a form of positive cosmological constant.
From these solutions we can see that as time passes, the h(t) decreases rapidly to h(0), a constant value, keeping a constant matter density.
We have also shown that the EChS field equations have solutions that allow us to identify the energy-momentum tensor for the field h a with a negative cosmological constant.

Consistency of the solutions with the "era of matter"
In the previous section, we find that the solutions of the EChS field equations, with T μν = 0, can be useful as models of the era of dark energy. In this section we review the consistency of these equations with the era of matter.
We will consider the ordinary matter as dust (ρ = 0, p = 0), such as occurs in standard cosmology. The nonordinary matter will be modeled as a perfect fluid (ρ (h) = 0 y p (h) = 0). In this case the field equations (35)-(39) take the form and the conservation (34) (divergence-free energy-momentum tensor) for each of the fluids are given bẏ Equation (96) has as solution where the initial conditions a 0 = a(t 0 ) and ρ 0 = ρ(t 0 ) have been set. Substituting (98) and (93) into (91) we have where we defined 6.1 Case k = −1 In this case, (99) can be rewritten where we finḋ In this case From (102) we can see thatȧ is well defined if where On the other hand a 0 must satisfy so that and therefore These results allow us to analyze the radicand in (102) i.e., which is satisfied for all a.

a. Plus or minus sign?
The choice of the sign in the radicand has information as regards the allowed values ofȧ. Let us considerȧ > 0 (the analysis of the caseȧ < 0 is very similar) The functionȧ(a) is monotonically increasing (decreasing) if we consider the plus (minus) sign in front of the square root.
From (110) we can see that there existsȧ cri a cri :=ȧ(a 4 min ) = If we consider the plus (minus) sign in front of the square root,ȧ cri is the minimum (maximum) value ofȧ.
If there is a limit to a a min , theṅ where k = −1.
b. Case where the sign is "+".
In this casė whose approximate solution is where we use A = 1 αl 2 and k = −1.
b. Case where the sign is "−".
In this casė whose approximate solution is where we use k = −1.

Case α < 0
In this case From (102) we can see thatȧ is well defined if but this condition is satisfied for all a.
a. Case where the sign is "+".
In this case so that The left side of the last equation must be positive, i.e., From (119) we obtain and again, the left side of the last equation must be positive, i.e., and from (121) we find Since i.e., a max is a local maximum. It is straightforward to prove thatȧ = 0 for a = a max . If a has a maximum value a max then (see (98)) This means that ρ has a minimum value ρ min given by Consider the case whereȧ > 0. We just considerȧ > 0 because the analysis of the caseȧ < 0 looks very similar. In this casė is a decreasing function. We can see that the minimum value ofȧ is given bẏ a min =ȧ(a max ) = 0 (130) and the maximum value ofȧ is given bẏ b. Case where the sign is "−".
In this case we obtain the following condition: where A = − 1 αl 2 and k = −1. This condition is trivially satisfied for all a.
This result implies thatȧ = 0. This means that a has no local maxima/minima, so a is monotonically increasing or monotonically decreasing.
If there is a limit to a 4 − B A a 0 , theṅ whose approximate solution is where we use k = −1.
In this casė is a decreasing function. The maximum value ofȧ is given bẏ and we can see thatȧ tends to a minimum value given bẏ 6.2 Case k = 0 In this case, (99) takes the form

Case α > 0
In this case From (139) we can see thatȧ is well defined if and therefore a minimum value for a is given by On the other hand a 0 ≥ a min , so that These results lead to i.e., a has no local maxima/minima, 2 so that a is monotonically increasing or monotonically decreasing.

Plus or minus sign?
The choice of the sign into the radicand has information as regards the allowed values ofȧ. Let us considerȧ > 0 (the analysis of the caseȧ < 0 is very similar): The functionȧ(a) is monotonically increasing (decreasing) if we consider the plus (minus) sign in front of the square root.
If we consider the plus (minus) sign in front of the square root,ȧ cri is the minimum (maximum) value ofȧ.
If there is a limit to a a min theṅ a. Case where the sign is "+".
In this casė whose approximate solution is In this casė whose approximate solution is where we use A = 1 αl 2 > 0 and a min = 4 κ 5 αl 2 ρ 0 3 a 0 .

Case α < 0
In this case From (139) we can see thatȧ is well defined if This condition is only satisfied if we use the minus sign "−" for all a, i.e., and therefore a has no local maxima/minima, so a is monotonically increasing or monotonically decreasing. Thus,ȧ has a maximum value in a = 0, i.e., andȧ tends to a minimum value given bẏ If there exists a limit for a whose approximate solution is where we use B = κ 5 ρ 0 3 .

Case k = 1
In this case, (99) can be rewritten as from whicḣ with k = 1.

Case α > 0
In this case From (159) we can see thatȧ is well defined if so that With these considerations we can analyze if the radicand is positive in (159):

a. Plus or minus sign?
Let us considerȧ > 0 (the analysis of the caseȧ < 0 is very similar): The functionȧ(a) is monotonically increasing (decreasing) if we consider the plus (minus) sign in front of the square root.
If we consider the plus (minus) sign in front of the square root,ȧ cri is the minimum (maximum) value ofȧ.
b. Case where the sign is "+".
In this case so that but (see (98)) It is straightforward to prove thatȧ = 0 for a > a min , then a has no local maxima/minima, and therefore a is monotonically increasing or monotonically decreasing.
If there is a limit to a a min , theṅ whose approximate solution is where we use A = 1 αl 2 and k = 1.
c. Case where the sign is "−".
In this case therefore This condition must also be satisfied by a min so that but (see (98)) and therefore From (171) we obtain i.e.,

Case α < 0
In this case From (159) we can see thatȧ is well defined if This constraint excludes the case with the plus sign "+" in front of the square root. This condition leads to where k = 1 and A = 1 αl 2 < 0. There is a maximum value for a: this maximum leads to but (see (98)) If there is a maximum a max then there must exist a minimum for ρ There is no a limit to a −→ ∞ and therefore it is impossible to find an approximate solution foṙ

Solutions for era of matter
We have found a family of solutions for the era of matter. If we consider an open space (k = −1), the solutions found include (i) an accelerated expansion (α > 0) with a minimum scale factor at initial time such that, when time goes to infinity, the scale factor behaves as a hyperbolic sine function (Fig. 4), (ii) a decelerated expansion (α < 0), with a Big Crunch in a finite time t max (Fig. 5), and (iii) a couple of solutions without accelerated expansion, whose scale factor tends to a constant value: α > 0 (Fig. 6) and α < 0 (Fig. 7). See Tables 4 and 5.
From models found in Sect. 6.1 we can see that there are solutions with α > 0 for an accelerated contracting universe and no accelerated contracting universe (see Fig. 8,ȧ < 0). These solutions were not studied.
Solutions found for a flat universe (k = 0) in expansion are (i) an accelerated expansion whose scale factor behaves as an exponential function when time grows and starts from a minimum value (Fig. 9), and (ii) a couple of solutions with decelerated expansion whose scale factor tends to a square root function: α > 0 (Fig. 10) and α < 0 (Fig. 11). See Tables 6 and 7.
In this case there are also solutions of a contraction universe (ȧ < 0): (i) one ends with a minimum value a min when α is positive (Fig. 12), and (ii) the other ends with a Big Crunch when α is negative (Fig. 13). Finally, we only found one solution for a closed universe (k = 1) in expansion. This solution is found when α is greater than zero. It behaves as a hyperbolic cosine function when time grows and starts from a minimum value (Fig. 14). See Table 8.
Furthermore, there are two contracting universe solutions, both ends in a finite time: (i) one ends with a minimum value a min , when α is positive (Fig. 15), and (ii) the other ends with a Big Crunch, when α is negative (see Table 9; Fig. 16).

Summary
We have considered a five-dimensional Einstein-Chern-Simons action S = S g + S M , which is composed of a gravitational sector and a sector of matter, where the gravitational sector is given by a Chern-Simons gravity action instead of    No accelerated the Einstein-Hilbert action and where the matter sector is given by a so-called perfect fluid. We have shown that: i The Einstein-Chern-Simons field equations (9) Table 6 Expanding universe solutions for scale factor of a flat space Table 7 Expanding universe solutions for scale factor of a flat space satisfy the cosmological principle and the ordinary matter is negligible compared to the dark energy, we find that (20)-(22) take the form (41)-(45). When ordinary matter is modeled as dust (era of matter), we find that (20)-(22) take the form (91)-(95). ii The field equations (41)-(45) were completely resolved for the age of dark energy (Sect. 5, accelerated expansion). We find that the field h a has a similar behavior to that of a cosmological constant.  iii The field equations (91)-(95) were solved for the era of matter (Sect. 6). We find several models that are consistent with standard cosmology. The dynamics of the field h a (95) was not analyzed because the focus was placed on the dynamics of the scale factor a(t).
In fact, in Sect. 5 we have found solutions that describe accelerated expansion for the three possible cosmological models of the universe. Namely, spherical expansion (k = 1), flat expansion (k = 0) and hyperbolic expansion (k = −1) when the constant α is greater than zero. This means that the Einstein-Chern-Simons field equations have as one of their solutions an universe in accelerated expansion. This result allows us to conjecture that these solutions are compatible with the era of dark energy and that the energy-momentum tensor for the field h a corresponds to a form of positive cosmological constant. We have also shown that the EChS field equations have solutions, which allows us to identify the − k with A > 0, k = 1, andȧ 0 >ȧ cri Table 8 Expanding universe solutions for scale factor of a closed space 3αl 2 a 2 0 − k. A decelerated solution describes an expanding universe, which then stops the expansion and contracts until the scale factor reaches a minimum a min > 0, in a finite time t max Accelerated Decelerated − k with A > 0, k = 1, andȧ 0 <ȧ cri  On the other hand, in Sect. 6 we have found a family of solutions for the era of matter. In the case k = −1 (open universe), the solutions correspond to (i) an accelerated expansion (α > 0) with a minimum scale factor at initial time that, when time goes to infinity, the scale factor behaves as a hyperbolic sine function; (ii) a decelerated expansion (α < 0), with a Big Crunch in a finite time t max , and (iii) a couple of solutions without accelerated expansion, whose scale factor tends to a constant value. In the case k = 0 (flat universe), the solutions describe (i) an accelerated expansion whose scale factor behaves as an exponential function when time grows and starts from a minimum value, and (ii) a couple of solutions with decelerated expansion whose scale factor tends to square root function. In the case k = 1 there is found only one solution for a closed universe in expansion, which behaves as a hyperbolic cosine function when time grows and starts from a minimum value. However, there are two     In summary, we have found some solutions for the field equations, which were obtained from a Lagrangian for the Chern-Simons gravity theory, studied in Ref. [1]. One problem with these solutions is that they are valid only in a fivedimensional space.
A connection between five-dimensional spacetimes and the four-dimensional universe could be accomplished by using a procedure, based on the Kaluza-Klein theory, known as dynamic compactification [12,13]. The method consists in considering a spacetime metric in which the scale factor of the compact space evolves as an inverse power of the radius of the observable universe. In fact the metric can be written in a convenient way so that it can achieve the compactness of the fifth dimension. Following Refs. [12,13] we could consider the five-dimensional metric ds 2 = −dt 2 + a 2 (t) dx 1 2 + dx 2 2 + dx 3 2 and then consider the case when the scale factor b(t) is given by b(t) = 1 a n , n > 0, where the parameter n must be positive for dynamical compactification to take place. Substituting (189) into the metric (188) we have ds 2 = −dt 2 + a 2 (t) dx 1 2 + dx 2 2 + dx 3 2 + dx 2 a 2n (t) .
Therefore b gets smaller as the radius of our universe a becomes bigger. It is possible to conjecture that the dynamic compactification procedure could lead, in a certain limit, to the usual results of the four-dimensional General Relativity (work in progress).
It should be noted that this compactification procedure (dynamic compactification) cannot be directly implemented in the theory, because this gravity theory is based on a Chern-Simons Lagrangian.
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