Dark Energy from Gauss-Bonnet and non-minimal couplings

Dark Energy from Gauss-Bonnet and non-minimal couplings

L. N. Granda luis.granda@correounivalle.edu.co    D. F. Jimenez jimenez.diego@correounivalle.edu.co Departamento de Fisica, Universidad del Valle
A.A. 25360, Cali, Colombia

We consider a scalar-tensor model of dark energy with Gauss-Bonnet and non-minimal couplings. Exact cosmological solutions were found in absence of potential, that give equations of state of dark energy consistent with current observational constraints, but with different asymptotic behaviors depending on the couplings of the model. A detailed reconstruction procedure is given for the scalar potential and the Gauss-Bonnet coupling for any given cosmological scenario. Particularly, we consider conditions for the existence of a variety of cosmological solutions with accelerated expansion, including quintessence, phantom, de Sitter, Little Rip. For the case of quintessence and phantom we have found a scalar potential of the Albrecht-Skordis type, where the potential is an exponential with a polynomial factor.

PACS numbers

98.80.-k, 95.36.+x, 04.50.Kd

preprint: APS/123-QED

I introduction

A significant number of extensions of general relativity modifying the behavior of Einstein gravity at cosmic scales, have been introduced lately in order to explain the observed accelerated expansion of the universe perlmutter -planck2 . These models range from modifications of the source terms that involve scalar fields of different nature like quintessence, phantom, tachyion, dilaton (see copeland -sergeiod for review), including different couplings of scalar field to curvature (scalar-tensor theories) chiba -granda3 , to modifications of the geometrical terms involving curvature, known as modified gravity theories capozziello1 -tsujikawa .
Among all possible explanations for the observed cosmic acceleration the scalar-tensor theories are widely considered since the couplings of scalar fields to curvature naturally appear in the process of quantization on curved space time ford ; birrel , from compactifications of higher dimensional gravity theories lamendola1 , in the next to leading order corrections in the expansion of the string theory metsaev ; cartier ; green . Perhaps the most studied and the simplest one of these couplings is the non-minimal coupling of the type . The role of this coupling in the dark energy (DE) problem has been studied in different works, including the constraint on by solar system experiments chiba , the existence and stability of cosmological scaling solutions uzan ; lamendola , perturbative aspects and incidence on CMB perrotta ; riazuelo , tracker solutions perrotta1 , observational constraints and reconstruction boisseau ; polarski ; capozziello3 , the coincidence problem tchiba , super acceleration and phantom behavior vfaraoni -polarski1 , and asymptotic de Sitter attractors vfaraoni1 . Another interesting interaction that gives good results in the study of the dark energy is the coupling between the scalar field and the Gauss-Bonnet (GB) invariant . Although the GB term is topologically invariant in four dimensions, nevertheless it affects the cosmological dynamics when it is coupled to a scalar field, contributing second order differential terms to the equations of motion. This coupling has been proposed to address the dark energy problem in sergei4 , showing attractive features like preventing the Big Rip singularity in phantom cosmology. Different aspects of accelerating cosmologies with GB correction have been discussed in sergei5 -capozziello5 . All these studies demonstrate that it is quite plausible that the scalar-tensor couplings predicted by fundamental theories may become important at current, low-curvature universe.
In this paper we consider a scalar-tensor model that contains the above mentioned two couplings: the non-minimal coupling to the curvature and to the Gauss-Bonnet invariant, and analyze the role of these couplings in the late time universe. The understanding of the effect of these non-minimal couplings could provide clues about how the fundamental theories at high energies manifest at cosmological scales. We consider two different approaches: first we find exact cosmological solutions in absence of potential, that give consistent description of different DE scenarios. It is shown that depending on values of the couplings, the universe can be currently undergoing a transition from quintessence to phantom phase or from phantom to quintessence phase. In the second approach we reconstruct the potential and the GB coupling for various interesting cosmological scenarios beginning with power-law expansion and considering also Big Rip and Little Rip solutions. For power-law solutions we found a potential that was considered before in connection with low energy limit of M-theory andreas ; skordis . The paper is organized as follows. In Sec. II we introduce the model of the scalar field with non-minimal and GB couplings and give a detailed reconstruction scheme for a given cosmological scenario. In section III we present exact solutions of the model with zero potential and study the behavior of the corresponding equations of state. In sec. IV we present some samples of late time cosmologies and make reconstruction of the scalar potential and GB coupling. Sec. V is dedicated to some summary and discussion.

Ii The scalar-tensor model and field equations

Let’s start with the action for the scalar field where in addition to the GB coupling we consider the non-minimal coupling of the scalar field to curvature. As will be seen below, the non-linear character of the cosmological equations makes the integration of the same ones very difficult for a given set of initial conditions. Nevertheless given that we know in advance some cosmological scenarios that represent probable states of expansion of the universe, we can deal with the inverse problem: for a given cosmological solution try the reconstruction of the model. Below we give a general approach to reconstruct the scalar-tensor model with non-minimal and GB couplings for any given cosmological scenario sergei5 . The action for the model with scalar field and matter is given by


where , is the GB invariant, and is the Lagrangian of perfect fluid with energy density and pressure . We will consider the spatially-flat Friedmann-Robertson-Walker (FRW) metric.


The Friedman equations with Hubble parameter are


Deleting the potential from eqs. (3) and (4) one finds


which can be written in the form


If additionally we have in mind that


then, the eq. (5) can be written as


Let’s define the following function


which allows to rewrite the Eq. (8) in the compact form:


This equation can be solved with respect to as


From (3) one can write the potential as


where the function is defined as


and using the Eq. (11) one finds


The Eqs. (11) and (14) allow to reconstruct the model for a given scalar field and Hubble function . In order to express the potential and the Gauss-Bonnet coupling as functions of the scalar field, we can assume that


where y are given functions. Replacing (15) in (11) and (14) we find


These equations allow to reconstruct the model by given y . In order to have explicit solutions for and we need to take into account the conservation equation for the matter component with constant equation of state

From , follows

This way it is obtained that


The Eqs. (18) and (19) after being replaced in the Eqs. (16) and (17) give the reconstructed model by known functions and . Therefore any cosmological scenario for the model (1) encoded in the functions and with the GB coupling and potential given by (16) and (17) can be realized. In section IV we provide some important examples, including cosmologies with phase of super-acceleration. In the next section we consider the model without potential, find exact solutions and analyze possible late time cosmological scenarios.

Iii The dynamics without potential. Exact solutions

As we will show, the model contains interesting solutions even in absence of the scalar potential. To this end, we write down the equation of motion for the scalar field


Setting and turning to the e-folding variable we can write the Eqs. (3) and (20) in the form


In order to integrate these equations we consider the following expression for the GB coupling


By using this expression for the GB coupling, the Eqs. (21) and (22) reduce to the following




by restricting the constant to the value , the last term in (24) disappears, reducing it to


which gives the solution


Replacing this solution into the equation of motion (25) leads to the following equation for the Hubble parameter


After solving this equation we can find the dark energy equation of state (EOS) as


In order to integrate the equation (28) we can assume some simplifications. First we can note that at far future () if , the exponential terms will dominate over the constants and the solution of the equation reduces to


where is the integration constant. The EOS for this solution is the constant , which corresponds to the divide between the decelerated and accelerated expansion. This means that (provided ) even if currently the EOS is close to , then at far future the dark energy EOS tends to . On the other hand, if then at far future the exponential terms in the Eq. (28) become subdominant and the solution to the equation will depend on the constant terms and reduces to


which gives the constant EOS


Thus depending on the values of and , at far future the EOS tends asymptotically to the cosmological constant if , or can fall below the phantom divide if the second term in Eq. (32) is negative. It follows then that the model (1) can describe quintessence and phantom phases even without potential. To see this more clearly lets consider the following restriction


which simplifies the Eq. (28) and leads to the solution


where is the integration constant. This solution gives the following dark energy EOS


lets assume that in the current epoch () the DE EOS parameter takes the value . Then setting in (35) one finds the following relation


By replacing from (27) and from the restriction (33) one can rewrite the Eq. (36) as


The r.h.s. of this equation is positive whenever , i.e. when the current EOS parameter is in the quintessential phase. Corresponding to this, the l.h.s. of the equation is positive if or . If the current EOS is or , then the r.h.s. of eq. (37) is negative and the corresponding l.h.s. becomes negative for in the interval . We can see the behavior of the initial condition in the EOS parameter depending on the initial conditions on the scalar field in Fig. 1.

Figure 1: The initial conditions for the current value of the DE EOS parameter as function of for some values of . The horizontal lines correspond to at and the cosmological constant at , which are independent of the initial value . For in the interval the allowed values of are or .

In the interval , where the EOS parameter can take values below the phantom divide, the Hubble parameter is not well defined and therefore the solution (34) does not describe phantom DE. Note that at larger values of (positive or negative), becomes closer to . To agree with current observations on , the initial value of the scalar field () should be around 2 or larger. Thus, for and we find . In Fig. 2 we show the evolution of the EOS in terms of the redshift for initial conditions taken from Fig. 1

Figure 2: The evolution of the DE EOS parameter as function of for which give () and respectively, for . Though the current values are very similar, the DE evolves to different scenarios depending on (which defines the sign of ).

The EOS for remains very close to even for . In general for positive the EOS evolves from in the past up to in the far future, and for negative the EOS evolves from in the past up to de Sitter state () in the distant future. All curves present appropriate quintessence behavior in the ”near” past and the present. The behavior of the model depends on the initial value and the non-minimal coupling .
Let’s consider the general case of the Eq. (28) with the solution


where is the integration constant and

The EOS for this solution is given by


which depending on the sign of evolves between the values:


It is noted that these limits do not depend on the initial value of the scalar field . It can be seen from these equations that the solution can contain the phantom phase if one of the parameters or is negative. Let’s consider each case separately. If we assume and , then the first -dependent factor in (38) increases exponentially with but the power of the second factor becomes negative, which leads to divergence al some point where . So the solutions with give rise to Big Rip singularities. These singularities can be avoided if we consider the second case where and . In this case the second factor in (38) is always positive independently of the sign of the power, giving a solution that is always finite with the advantage that can describe a phantom universe. To illustrate the behavior of the solution (38), in Fig. 3 we plot the EOS as function of the redshift for some values of the parameters.

Figure 3: The behavior of the DE EOS as function of the redshift. The initial value of the scalar field is and the current value is . For the corresponding coupling parameters take the values and for all cases.

We can see that these curves fit very well to the observed behavior of the DE EOS. According to the curves for , the expansion due to DE is currently undergoing the transition from phantom to quintessence phase, and the curves for describe un expansion currently going through the transition from quintessence to phantom phase. There is also possible to have adequate behavior of DE for small values of the coupling as is shown in Figs. 4 and 5, where we show solutions with ”almost constant” EOS or with almost constant slope in a wide interval of .

Figure 4: The DE EOS as function of the redshift for small parameters. In all cases and the initial value of the scalar field is . The curves show different current EOS parameters , but all of them are close to , and present transitions from phantom to quintessence phase in the past (), the present () and the future ().

The EOS shows very little evolution for a wide interval of , and the deviation from almost constant value happens near the present epoch. In fact the model can mimic a behavior very close to the cosmological constant up to recent epochs.

Figure 5: Fig. 5 The DE EOS as function of the redshift for . In all cases the initial value of the scalar field is . The curves cover different behaviors of the EOS, but all of them in an acceptable range of values according to the data. Note the transitions from quintessence to phantom phase in the past (), the present () and the future (). The horizontal line corresponds to the cosmological constant.

Iv Reconstructing quintessence and phantom scenarios

In an scenario with dominance of DE we assume the scalar field with non-minimal and GB couplings as the responsible for the energy content of the universe, which is achieved in the model (1) by setting or in the subsequent equations, by making . In this section we will discuss some important solutions that give appropriate description of late-time universe. We give explicit examples of reconstructed scalar potential and GB coupling for an accelerated universe in quintessence and phantom phases, with Big Rip and Little Rip singularities. The phantom cosmology can be realized in the present model without resorting to ghost scalar fields.

iv.1 Quintessential power-law

In the FRW background the power-law solutions are of special interest because they represent asymptotic or intermediate states among all possible cosmological evolutions. Let’s consider the following functions


which according to (15) lead to


Replacing (40) in (16) one finds the GB coupling as



and the expression for the potential (17) becomes



The power-law solution can also be realized by the following functions


which lead to the following Gauss-Bonnet coupling


and the scalar potential


It can be seen that for large this potential has similar behavior as the potential (45).

iv.2 Phantom power-law

Another interesting solution is the phantom power-law, that gives an EoS below the cosmological constant which is not ruled out by current astrophysical observations, but leads to future Big Rip singularity. Assuming the following functions


which give


Replacing in the GB coupling (16) we find



and the potential from (17) takes the form



According to (48), at and the scalar potential (50) becomes infinity giving rise to the Big Rip singularity. This phantom behavior can also be obtained with the following functions


which give the Gauss-Bonnet coupling


and the scalar potential


This potential also grows toward infinity since at . The expressions for the potentials (45) and (49) show a run-away behavior (i.e. at ) which is important in the phenomenology of dark energy since it reflects the scaling behavior of the model. The potentials like (43) and (50) which contain combination of exponential and power-law terms can be present in the low energy limit of M-theory as proposed in andreas ; skordis where it was shown that simple corrections to pure exponential potential produce interesting quintessence accelerating solutions. In the present model (1) these corrections allow not only quintessence but also phantom scenarios (at least of the power-law type). Note that from (42), (43), (49), and (50) follows that when the non-minimal coupling disappears, then only the free term , , and survive in the corresponding expressions, and the GB coupling and potential become pure exponentials for quintessence and phantom power-law.

iv.3 The de Sitter solution

The model (1) (with ) contains de Sitter solution with varying scalar field as we show in the following two examples. Taking the functions


that lead to


we find the Gauss-Bonnet coupling and the potential as


The following functions also give the de Sitter solution


from where , which lead to the Gauss-Bonnet coupling


and the expression for the potential (17) becomes


Note that in absence of potential and for the asymptotic case of constant there is not de Sitter solution.

iv.4 Little Rip solution

This type of solutions represent an alternative to Big Rip frampton ; brevik where the dark energy density increases with time but without facing a finite time future singularity. In Little Rip solutions the equation of state parameter (or ) and causes the same effect of dissociation of matter in the future as the Big Rip solutions, but the scale factor, the density and pressure remain finite at finite time. Let’s consider the following scenario


From where it is seen that y . If we replace these functions in (16) and (17) in absence of matter one obtains



iv.5 Solutions with quintessence and phantom phases

Another interesting scenario that allows the integration in Eqs. (16) and (17) presents quintessence and phantom phases and comes from the functions and , which give


Note that for times the universe is in the quintessence phase, and enters the phantom phase for times . The Big Rip singularity occurs at . The general expressions for and for arbitrary depend on hypergeometric functions and are too large. Here we limit ourselves to the special case where the expressions for the GB coupling and potential take the form