Interaction between Dark Matter and Dark Energy and the Cosmological Coincidence Problem

Nozari, Kourosh; Behrouz, Noushin; Rashidi, Narges

doi:https://doi.org/10.1155/2014/569702

Advances in High Energy Physics

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Abstract Introduction Preliminaries Conclusion Appendix References Copyright Related Articles

Research Article | Open Access

Volume 2014 | Article ID 569702 | https://doi.org/10.1155/2014/569702

Interaction between Dark Matter and Dark Energy and the Cosmological Coincidence Problem

Kourosh Nozari,¹Noushin Behrouz,¹and Narges Rashidi¹

Academic Editor: Frank Filthaut

Received27 May 2014

Revised27 Oct 2014

Accepted09 Nov 2014

Published02 Dec 2014

Abstract

We consider a quintessence model of dark energy inspired by scalar-tensor theories of gravity where the scalar field is nonminimally coupled to gravity and dark matter. By considering exponential potential as self-interaction potential, the stability and existence of the critical points are discussed in details. With nonminimally coupled dark sector with gravity, we obtain scaling solutions to address the coincidence problem by considering complex velocity for dark matter. The statefinder diagnostic shows that the equation of state reaches model in the future.

1. Introduction

Recent observational pieces of evidence [1–6] have revealed that today the energy density of the universe is dominated by a component with negative pressure that violates the strong energy condition (SEC). This yet unknown component is called “dark energy” (DE), which derives the positively accelerated phase of the universe expansion. Modification of gravity on vast scale may be another alternative to explain this accelerated phase of expansion [7, 8]. In the framework of dark energy proposal, the simplest model is a cosmological constant, whereas, the cosmological constant proposal suffers from serious difficulties such as a huge fine-tuning [9–12]. In fact, there is no convincing explanation for the very small value of the and also no concrete solution for coincidence problem and need for huge fine-tuning. Coincidence problem is that why are the energy densities of both dark components (dark energy and dark matter) the same order of magnitude today? The dynamical dark energy models such as light scalar fields, quintessence [13, 14], phantom fields [15], tachyon fields [16, 17], and other similar theories that are capable of explaining the late-time cosmic acceleration can alleviate the coincidence problem [18]. It is possible to construct a generalized model of quintessence field that the background and the dark energy evolve independently, but there is a nonminimal coupling between both dark components [19–26]. Because the nature of the dark matter (DM) is yet unknown, it is possible to consider additional interactions between the dark components, without tension with the observational facts. Nevertheless, solar system tests impose some restrictions on the nonminimal coupling between the dark matter and the dark energy [27]. Currently no specific coupling between the dark sectors has been known based on fundamental theories. Therefore, suggested coupling models will necessarily be phenomenological [28, 29], though some models seem to have more physical justification than others [19]. Here we are going to study an interacting model in which the dark sectors are coupled to each other in a background gravitational field nonminimally coupled to the dark energy. We seek scaling solutions to address the coincidence problem in a manner much similar to the chameleon mechanism.

The paper is organized as follows. In Section 2 we review some new details of two models of interaction between the dark sectors and scalar curvature with minimal and nonminimal coupling. We present existence and stability of the critical points in phase space. In Section 3, we present a model in which the scalar field is coupled nonminimally with both gravity and dark matter. The cosmological dynamics of the model is studied via dynamical system technique and also statefinder diagnostic. Scaling solutions are obtained in this section and the coincidence problem is addressed through a manner similar to the chameleon mechanism. This is done by relaxing the reality of sound velocity and allowing to have complex sound speed profile. The coincidence problem can be evaded in this case since, a constant ratio between the dark energy and dark matter density is a stable attractor. We suppose universal coupling of the quintessence field to all sorts of matter (radiation is excluded). We note also that actually there is no need to consider the coupling between quintessence field and baryonic matter. In fact, the quintessence field has coupling with dark matter. In Section 4, conclusions are presented.

2. Preliminaries

2.1. Minimal Coupling of Quintessence Field with Dark Matter

The action for a quintessence field minimally coupled with the dark matter is given by where is the curvature scalar, is the quintessence scalar field, the quintessence self-interaction potential, which we consider as , where and are positive constants and is the Lagrangian density of matter (all sorts of matter except radiation and baryonic matter. Note that the only sort of matter here is the dark matter). The FRW line element is given by where is the cosmic time, (, , ) are the spatial (radial and angular) coordinates and is the spatial curvature where corresponding to the flat, closed and open universes, respectively. We consider the system of units in which . The field equations that are derived from the action (1) are where is the barotropic index which depends on the type of matter. The continuity equations are

The Friedmann equation (3) with is as follows: which and , (7) implies that

We study cosmological dynamics of the model by translating our equations in the language of the autonomous dynamical system. We define the following dimensionless quantities:

By rewriting the Friedmann equation (3) (with ) in terms of the new variables, we obtain a constraint on the parameters space of the model as follows: which allows to seek for evolution of just two variables since the third one can be obtained by this constraint. In what follows we choose and as our independent variables. Using these phase space variables, the evolution equations (4) and the equation of state parameter can be rewritten as follows:

In the next step, we introduce a new time variable that is related to the cosmic time through and obtain the following autonomous system of equations:

The stability around the fixed points is related to the form of the eigenvalues in each critical point. In Table 1 we exhibit the properties of the critical points such as the existence and stability. Furthermore, we present as the value of the total equation of state parameter at the critical points to see the possibility of accelerated expansion in this setup (). The eigenvalues can be obtained by using the above autonomous equations, the results of which are shown in Table 2. As we see in Table 1, among the five fixed points, only point exhibits scaling solution for late-time. Using (8), (9), (10), and (13), we find for this point According to Table 1, this point can be either stable node or stable spiral. In Figure 1, if we choose and parameters from the blue shaded region, point will be stable node, but if we select these parameters from the green shaded region, point will be stable spiral. The phase space of this critical point is illustrated in Figure 3(a). All the phase space trajectories diverge from the unstable point (radiation domination) and converge towards the attractor. As has been shown in Figure 4(a), this critical point cannot cross the phantom divide line and reaches to recent quantity of that tends to be less than [30]. To have such an observationally supported crossing, we add a further ingredient to the theory: the nonminimal coupling between the dark energy and scalar curvature [31]. Furthermore, it is important to keep in mind that if we consider negative values of for to have , then the critical point will be also a stable attractor point, which is not acceptable since it should be a transient matter dominated epoch.

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2.2. Nonminimal Coupling of Dark Energy with Ricci Scalar

We consider the following action in the spirit of the scalar-tensor theories: where is the nonminimal coupling between the quintessence field as dark energy and scalar curvature. The energy density and pressure of the scalar field nonminimally coupled to gravity are defined as follows [32]: The field equations derived from action (16) are given as where is the barotropic index of ordinary matter. The continuity equations are given as Similar to the previous subsection, (7) and (8) are valid for this case too. The dimensionless quantities for this case are , , and defined in the previous subsection, plus the additional one defined as follows: From Friedmann equation (18) with zero spatial curvature , we have the following constraint: In terms of these new variables, the acceleration equation (19), the scalar field’s equation of motion (20), and equation of state parameter are given by the following expressions: We differentiate the phase space dimensionless variables with respect to to find

The critical points and their stability around the fixed points are shown in Table 3 (for ) and eigenvalues of the Jacobian matrix are presented in Table 4. As Table 3 shows, there is no critical point for late-time. Attractor critical points and belong to the future. Fixed point can be either a stable node or a stable spiral depending on the values of and from blue shaded region or green shaded region in Figure 2. However, critical point is stable spiral. The 2-dimensional phase space of this critical point is depicted in the right panel of Figure 3. So, we see that the nonminimal model allows to reach a stable phase in the future with equation of state that tends to the one in the future. The behavior of is shown in Figure 4(b). There is no crossing of the phantom divide even in this nonminimal model. So, similar to the minimal model, this nonminimal model is not a suitable framework for late time cosmic dynamics and it is not capable of addressing the coincidence problem.

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Figure 3

(a) The phase plane for critical (for minimal case) with and . The critical points are stable nodes (sinks) so that the quintessence dominated solution is the late time attractor. The critical points and are saddle points, but , fixed points are repeller nodes. All the phase space trajectories diverge from the unstable point and converge towards the attractor. (b) The phase plane for the critical point (for nonminimal case) with , and . The critical point is a stable node (a sink) so that the quintessence dominated solution is a future attractor.

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3. Dark Energy Coupled Nonminimally with Gravity and Dark Matter

We consider a scalar field, as dark energy component, which is nonminimally coupled to gravity and dark matter in the spirit of scalar-tensor theories: where is the quintessence-matter coupling function, ( is constant). The energy density and pressure of the nonminimally coupled scalar field in this case are given by (17) but now with redefined (see (32) and (35) below).

The field equations that are derived from the action (28) with redefined are as follows:

A general coupling between a quintessence field and the dark matter may be described by the continuity equations as Here is the rate of energy density exchange in the dark sector with the following properties: After integration of (32) we find where is a constant of integration. By defining now the following equation is valid: Like the previous subsection, (7), (8) are valid for this case too. Now we study cosmological dynamics of this interacting model as a dynamical system in phase space. Our dimensionless parameters and the Friedmann constraint are similar to (9), (22), and (23). We rewrite other important equations of the setup in terms of the new variables. The acceleration equation (30) and the equation of motion (31) in terms of the new variables take the following form, respectively: With , the following autonomous system of equations is obtained: The critical points and stability around these points are presented in Table 5 and their eigenvalues of the Jacobian matrix are shown in Table 6.

(i) Critical Point . The critical point behaves like a saddle point in the phase space and in this case we have no late-time acceleration. For this point the universe is radiation dominated.

(ii) Critical Point . Points represent a cosmological constant dominated accelerating phase. In this case, either a scalar field’s kinetic energy term or a potential energy term plays the role of a cosmological constant. So, with a quintessence scalar field nonminimally coupled with dark matter and curvature, it is possible to realize a stable, de Sitter, future accelerating phase. The complicated stability conditions for the critical point were confirmed numerically, and the results are shown in Figure 2. As we see from Figure 2(a), if we choose and quantities from the blue shaded region, then we have a stable node, but if we select these two quantities from the green region, we will have a stable spiral. For critical point there is only a stable spiral solution that is illustrated in Figure 2(b). The phase portrait for this case is shown in Figure 7(a). The behavior of is drawn in Figure 8(a). This figure shows that we will reach a stable phase in the future with equation of state parameter that tends to model.

(iii) Critical Point . For this case, there is no contribution of the scalar field and the universe is dominated by matter fields other than the quintessence scalar field. These two critical points behave like saddle points in the phase space if we consider . For , one can obtain an accelerating phase of expansion, but this phase is not stable. However, if we consider , we will have two kinds of stable attractors. It will be a stable node if we choose and from the Figure 5(a), and a stable spiral if we choose and from Figure 5(b).

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(b)

(iv) Critical Point . The stability conditions for critical points are very complicated and therefore we do not present their functional form here. However, for completeness the results are illustrated in Figure 6. There are two situations depending on the values of . If we consider , there is a saddle point. On the other hand for , we can consider the possibility of having complex sound speed for nonordinary matter fields. In this situation there is a stable node for values of and that belong to the shaded region in Figure 6(a), and a stable spiral for values of and belonging to the shaded region in Figure 6(b). This point is an accelerated scaling solution. Now, by considering (8), (9), (22), (23), and (26), the coincidence problem can be addressed naturally. In fact, with and , our analysis confirms that and . The phase portrait for this case is shown in Figure 7(b). It has been shown that if we select and from Figure 6, the critical points (matter dominated phase) will be a saddle point and all the trajectories converge to the attractor points . By adopting suitable values of quantities , , and , the current value of the dark matter density, , can be in agreement with recent data from [30], . The behavior of is shown in Figure 8(b). Now the total equation of state parameter crosses the phantom divide line and the universe reaches a stable phase. From Figure 8, we see that if we choose suitable values for , , and , the value of the equation of state parameter can be in agreement with recent observational data; according to the Planck + WP + highL + BAO results [30].

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4. Statefinder Diagnostic

The dark energy properties are model-dependent. In order to distinguish between different types of dark energy models, in 2003 Sahni et al. [33] have suggested a diagnostic proposal by introducing a new pair of parameters , called statefinder parameters. These parameters can be constructed by using both the second and third derivatives of the expansion factor. The second derivative gives the deceleration parameter which has the following form in a spatially flat universe: The statefinder pair, , are defined as The statefinder diagnostic tool depends on the scale factor. This shows that the statefinder parameters are geometrical in essence. Nowadays, the various dark energy models have been considered from the statefinder diagnostic point of view. The different dark energy models have various evolutionary trajectories in plane. So, the statefinder tool can distinguish between alternative models. Furthermore, by using the statefinder parameters, we can study the expansion history of the universe by using higher derivatives of the scale factor. The scenario corresponds to a critical point in the phase diagram with . By drawing the trajectories in the - phase plane, the discrepancy of the model from can be investigated [34]. We can rewrite (41) as In a minimally coupled quintessence field with the dark matter, by substituting (11) into (43), is obtained to be as follows where a prime denotes derivative with respect to .

Also parameter can be derived by substituting (44), (40), and (11) into (42). Due to its lengthy form, we avoid presenting this quantity explicitly. Now, we examine the numerical analysis of the statefinder diagnostic. Figure 9 for the late time stable scaling solutions , shows the trajectories of , , and phase plane for two different and parameters. If and , the initial values will be and with for blue, dashed line. For and , the initial values will be and for purple solid line and this is in agreement with Planck data [30]. As the figure illustrates with various and parameters, the trajectories evolve differently. One can choose small values of and in order to approach the model in this framework. We note also that in this platform one can choose the suitable values of and in order to find more viable values of in comparison with recent observations.

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After studying statefinder diagnostic for the case with minimal coupling between the quintessence field and dark matter, now we extend our analysis to the nonminimal coupling between the dark energy component and the scalar curvature. The parameter can be obtained by replacing (24) into (43) As we have mentioned previously, parameter can be obtained by replacing (45), (40), and (24) in (42). Now we present the numerical analysis of the statefinder diagnostic. Figure 10 for the stable node shows the trajectories of , , and phase planes for two different initial values with , , and . As this figure indicates, the model with ordinary dark mater () and a nonminimally coupled quintessence field, the trajectories of , , and in phase plane reach a stable point in the future, that is, corresponding to the model ().

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Now we study statefinder diagnostic for a general model with dark energy nonminimally coupled to both dark matter and scalar curvature. Similar to our previous treatment, the parameter can be derived by replacing (37) into (43) The parameter can be calculated by replacing (46), (40), and (37) into (42). For this model we analyze numerically the statefinder diagnostic for critical points , and . If we consider , then the critical points for the late time scaling solution will be saddle points (see Table 5). In addition, by considering the attractor points , the model reaches the model in the future. For stable node , the trajectories of , , and in phase plane with two initial conditions are drawn in Figure 11. In these figures we considered two different sets of initial values for , , and as have been shown in figures and we have set also , , , and (for ordinary dark matter). These two different initial values lead to the trajectories that evolve to the same fixed point in the future. For stable nodes , with (corresponding to nonordinary dark matter) we have late time scaling solutions. The trajectories of , , and in phase plane with two different values of the parameter, but with the same initial conditions, , , and , have been shown in Figure 12. As this figure illustrates, with different values of the parameter the trajectories evolve differently. With both adopted values of the parameter, the model approaches the model in the late time and also the future. However, it is possible to choose the values of so that the model tends to the model at late time or future.

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5. Summary and Conclusion

In this paper we have studied an interacting model in which the dark sectors (dark matter and dark energy) are coupled to each other in a background gravitational field which is nonminimally coupled to the dark energy. We have shown the possibility of having scaling solutions in this setup. These solutions are capable of addressing the coincidence problem in a manner much similar to the chameleon mechanism. In fact, we have introduced the idea that , as the barotropic index, is capable of getting negative values for nonordinary dark matter (or in some nonstandard situations). This assumption opens new windows in the issue of dark energy interacting with dark matter. With this assumption, it is possible to have complex sound velocity in the medium much similar to the complex index of refraction in optical media.

In summary, in the first part of the paper we have considered a minimal model with no interaction between the dark sectors. In this case there is no crossing of the phantom divide. In the next step we considered nonminimal coupling between dark energy and gravitational sector but without any interaction between the dark sectors. In this case, there is no attractor solution for late time. There is also no possibility for transition to phantom phase. In the last step we supposed a general model with interaction between the dark sectors and also between dark energy and scalar curvature. This general model in the spirit of scalar-tensor theories provides a lot of interesting facilities: there is a possiblity to cross the phantom divide line by the equation of state parameter in some subspaces of the model parameter space, it is possible to address the coincidence problem in a natural manner and finally there is a late time attractor which goes to in the future via statefinder diagnostic analysis. In each step we have compared our results with observational data from joint data set.

Appendix

The values of the parameters introduced in Tables 4 and 6 are as follows:

Conflict of Interests

The authors declare that there is no conflict of interests regarding the publication of this paper.

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Copyright

Copyright © 2014 Kourosh Nozari et al. This is an open access article distributed under the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. The publication of this article was funded by SCOAP³.

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