Parameterizing Dark Energy Models and Study of Finite Time Future Singularities

Bandyopadhyay, Tanwi; Debnath, Ujjal

doi:https://doi.org/10.1155/2019/5393491

Advances in High Energy Physics

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Research Article | Open Access

Volume 2019 | Article ID 5393491 | https://doi.org/10.1155/2019/5393491

Parameterizing Dark Energy Models and Study of Finite Time Future Singularities

Tanwi Bandyopadhyay¹and Ujjal Debnath²

Academic Editor: Antonio J. Accioly

Received01 Nov 2018

Revised01 Mar 2019

Accepted21 Mar 2019

Published09 Apr 2019

Abstract

A review on spatially flat D-dimensional Friedmann-Robertson-Walker (FRW) model of the universe has been performed. Some standard parameterizations of the equation of state parameter of the dark energy models are proposed and the possibilities of finite time future singularities are investigated. It is found that certain types of these singularities may appear by tuning some parameters appropriately. Moreover, for a scalar field theoretic description of the model, it was found that the model undergoes bouncing solutions in some favorable cases.

1. Introduction

In order to avoid the initial singularity problem [1], a competitive alternative structure is proposed to the standard inflationary description. This is called the big bounce scenario ([2–10]). In this framework, the universe initially contracts continuously up to an initial narrow state with a nonzero minimal radius and then transforms to an expanding phase [11]. This means that the initial singularity is replaced by a bounce and consequently the cosmic equation of state (EoS) parameter crosses the phantom divide line (from to ).

On the other hand, various cosmological observations indicate the current cosmic acceleration ([12–21]). To explain this phenomenon in the homogeneous and isotropic universe, it is necessary to assume a component of matter with large negative pressure, called dark energy. Since the inception of this concept, a wide variety of phenomenological models have been proposed as the most suitable candidate of dark energy. Among them, the cosmological constant provides plausible answers but suffers from the fine-tuning problem. This issue has forced researchers to probe models having time-dependent equation of state parameter for the dark energy component. A simple classification of these models could be as follows:

Cosmological constant ()

Dark energy with constant [cosmic strings (), domain walls ()].

Dynamical dark energy ( constant) (i.e., quintessence, Chaplygin gas, k-essence, braneworld) ([22–30])

Dark energy with [scalar-tensor theory, phantom models] ([31, 32])

The reconstruction problem for dark energy is reviewed in [33] in much detail (see also the references therein). Recently, in the literature [34], the possibilities of future singularities have been studied in the framework of Modified Chaplygin Gas filled universe and conditions of bounce were investigated. In this work, we provide more general results in terms of the possibilities of finite time future singularities in the context of a D-dimensional Friedmann-Robertson-Walker universe by imposing five standard parameterizations of the dark energy equation of state parameter. Different aspects of dark energy models have been studied so far to reconcile standard cosmological scenario with observations but no work has been done to the parameterization of these models in view of investigating the finite time future singularities.

The paper is organized as follows. In Section 2, we state the governing equations of the metric in the D-dimensional universe. In Section 3, the descriptions for the major physical quantities are provided in the backdrop of five different parameterization models both analytically and graphically. In Section 4, the possibilities of future singularities are examined for these five models and the possible restrictions for certain type of singularity are shown in tabular form. In Section 5, the bouncing universe is described in the five parameterization models and, finally, we end with a short discussion in Section 6.

2. D-Dimensional Friedmann-Robertson-Walker Universe

We consider the D-dimensional spatially flat Friedmann-Robertson-Walker universe, given by [34]

where is the scale factor and is the metric for the -dimensional space. The field equations together with the energy conservation equation can be obtained as (assuming )and

Here denotes the Hubble parameter. In the following section and subsequent subsections, we will examine different parameterizations of dark energy models and attain analytical as well as graphical expressions of some physical entities involved in the process.

3. Dark Energy as Scalar Field for Various Parameterization Models

By considering scalar field with the potential , the effective Lagrangian [34] is given bySo the energy density and pressure take the formThe kinetic energy for the field is given by

where . One can always write , where the prime denotes differentiation with respect to redshift . With the help of (2), we have

The scalar potential associated with the field is given by

In the next subsections, we will investigate the scalar field and its potential in different well-known parameterization models. A detailed review of different dark energy models can be found in [35].

3.1. Model I: Linear Parameterization

Here we assume the linear equation of state [36] . Here and are constants. Using (4), the energy density of the model then gives rise to

Here is the present value of the energy density. The pressure of the fluid then becomes

Then (9) reduces to

which on further integration gives rise to the scalar field as

where . Also (10) changes to

We draw the variations of energy density , pressure , EoS parameter , Hubble parameter , potential , and the scalar field with the variation in in Figures 1(a)–1(f), respectively. Figure 1(g) shows the variation of with . We observe that , , and decrease as decreases. and decrease from positive level to negative level as decreases. first increases up to certain value of and then decreases as decreases. Also decreases as increases.

(a)

(b)

(c)

(d)

(e)

(f)

(g)

3.2. Model II: Chevallier-Polarski-Linder (CPL) Parameterization

In the Chevallier-Polarski-Linder (CPL) parameterization model, the equation of state is given by [37, 38] . Here again and are constants. With these, the expressions of energy density, pressure, scalar field, and the potential becomeand

We draw the variations of energy density , pressure , EoS parameter , Hubble parameter , potential , and the scalar field with the variation in in Figures 2(a)–2(f), respectively. Figure 2(g) shows the variation of with . We observe that , , and first decrease up to as decreases and then sharply increase as decreases. But first increases up to as decreases and then sharply decreases as decreases but keeps the negative level. decreases as decreases and always keeps negative sign. increases as decreases. Also decreases as increases.

(a)

(b)

(c)

(d)

(e)

(f)

(g)

3.3. Model III: Jassal-Bagla-Padmanabhan (JBP) Parameterization

For the Jassal-Bagla-Padmanabhan (JBP) parameterization model, the equation of state changes to [39] , where and are constants. The following expressions are subsequently obtained as

We draw the variations of energy density , pressure , EoS parameter , Hubble parameter , potential , and the scalar field with the variation in in Figures 3(a)–3(f), respectively. Figure 3(g) shows the variation of with . We observe that , , and first decrease up to as decreases and then sharply increase as decreases. But first increases up to as decreases and then sharply decreases as decreases but keeps the negative level. first increases up to certain value of and then sharply decreases but keeps negative sign. decreases as decreases. Also increases as increases.

(a)

(b)

(c)

(d)

(e)

(f)

(g)

3.4. Model IV: Alam-Sahni-Saini-Starobinsky (ASSS) Parameterization

In the Alam-Sahni-Saini-Starobinsky (ASSS) parameterization model, the equation of state parameter has the expression [40, 41]

where, , and are constants. In this case, the physical parameters , and become

We draw the variations of energy density , pressure , EoS parameter , Hubble parameter , potential , and the scalar field with the variation in in Figures 4(a)–4(f), respectively. Figure 4(g) shows the variation of with . We observe that , , , and decrease as decreases. increases as decreases but keeps negative sign. first decreases up to certain value of and then increases as decreases. Also increases as increases.

(a)

(b)

(c)

(d)

(e)

(f)

(g)

3.5. Model V: Efstathiou Parametrization

Here, in Efstathiou parametrization model, the equation of state takes the form [42, 43] , where again and are constants. This gives rise to the following terms:

We draw the variations of energy density , pressure , EoS parameter , Hubble parameter , potential , and the scalar field with the variation in in Figures 5(a)–5(f), respectively. Figure 5(g) shows the variation of with . We observe that , , and first decrease up to certain value of as decreases and then sharply increase as decreases. But first decreases from positive level to negative level and then slightly increases and then sharply decreases as decreases but keeps the negative sign. decreases from positive level to negative level as decreases. decreases as decreases. Also increases as increases.

(a)

(b)

(c)

(d)

(e)

(f)

(g)

4. Analysis of Future Singularities

The future singularities can be classified in the following ways [44, 45]:(i)Type I (big rip): for , , , and (ii)Type II (sudden): for , , , and (iii)Type III: , , , and (iv)Type IV: for , , , and

where , , and are constants with .

Table 1 shows the restrictions on the parameters involved in the five parameterization models for the occurrence of the future singularities.

5. Bouncing Universe

The initial singularity in the cosmological models can be avoided by introducing the nonsingular bouncing models. In these models, a universe undergoing a “bounce” stage attains a minimum after a collapsing phase and then subsequently expands. During the collapse, the scale factor decreases [] and, during the expanding phase, it increases []. At the bounce point, , the minimal necessary condition (may not be sufficient) is and for for small . For a nonsingular bounce .

In the current study, the bouncing universe can be viewed in different parameterizing models from Figures 6(a)–6(j), where the evolution of the scale factor and the EoS parameter are shown with respect to time for each model. For the bouncing phase, the scale factor first decreases and then increases in order that the universe enters into the hot Big Bang era immediately after the bounce. The nature of the equation of state parameters has been presented in the figures. The figures clearly show bouncing solutions for linear, CPL, JBP, ASSS, and Efstathiou models with a minimal nonzero scale factor .

(a)

(b)

(c)

(d)

(e)

(f)

(g)

(h)

(i)

(j)

6. Discussion

In this work, we have considered the D-dimensional flat FRW model of the universe in the background of some well-known parametrization of dark energy models like linear, CPL, JBP, ASSS, and Efstathiou. By considering the scalar field model as these parametrizations of dark energy, we found the energy density, pressure, scalar field, and corresponding potential in terms of the redshift . In model I (linear), we have drawn the variations of energy density , pressure , EoS parameter , Hubble parameter , potential , and the scalar field with the variation in in Figures 1(a)–1(f), respectively. Figure 1(g) shows the variation of with . We have seen that , , and decrease as decreases. and decrease from positive level to negative level as decreases. first increases up to certain value of and then decreases as decreases. Also decreases as increases.

In model II (CPL), we have drawn the variations of energy density , pressure , EoS parameter , Hubble parameter , potential , and the scalar field with the variation in in Figures 2(a)–2(f), respectively. Figure 2(g) shows the variation of with . We have seen that , , and first decrease up to as decreases and then sharply increase as decreases. But first increases up to as decreases and then sharply decreases as decreases but keeps the negative level. decreases as decreases and always keeps negative sign. increases as decreases. Also decreases as increases.

In model III (JBP), we have drawn the variations of energy density , pressure , EoS parameter , Hubble parameter , potential , and the scalar field with the variation in in Figures 3(a)–3(f), respectively. Figure 3(g) shows the variation of with . We have seen that , , and first decrease up to as decreases and then sharply increase as decreases. But first increases up to as decreases and then sharply decreases as decreases but keeps the negative level. first increases up to certain value of and then sharply decreases but keeps negative sign. decreases as decreases. Also increases as increases.

In model IV (ASSS), we have drawn the variations of energy density , pressure , EoS parameter , Hubble parameter , potential , and the scalar field with the variation in in Figures 4(a)–4(f), respectively. Figure 4(g) shows the variation of with . We have seen that , , , and decrease as decreases. increases as decreases but keeps negative sign. first decreases up to certain value of and then increases as decreases. Also increases as increases.

In model V (Efstathiou), we have drawn the variations of energy density , pressure , EoS parameter , Hubble parameter , potential , and the scalar field with the variation in in Figures 5(a)–5(f), respectively. Figure 5(g) shows the variation of with . We have seen that , , and first decrease up to certain value of as decreases and then sharply increase as decreases. But first decreases from positive level to negative level and then slightly increases and then sharply decreases as decreases but keeps the negative sign. decreases from positive level to negative level as decreases. decreases as decreases. Also increases as increases.

Also the present work is designed to investigate the possibilities of finite time future singularities, that is, types I (big rip), II (sudden), III, and IV singularities. From Table 1, we observe that, for linear parametrization model, the type I (big rip) singularity occurs provided , but types II-IV singularities cannot occur. For CPL parametrization model, the type I (big rip) singularity occurs provided , but types II-IV singularities cannot occur. For JBP parametrization model, the type I (big rip) singularity occurs provided , but types II-IV singularities cannot occur. For ASSS parametrization model, the types I-III singularities cannot occur; only type IV singularity occurs provided . For Efstathiou parametrization model, the type I (big rip) singularity occurs provided , but types II-IV singularities cannot occur.

Data Availability

The data used to support the findings of this study are included within the article in the references and therein.

Conflicts of Interest

The authors declare that there are no conflicts of interest regarding the publication of this paper.

Acknowledgments

The authors are thankful to IUCAA, Pune, for their warm hospitality where most of the work has been done during a visit under the Associateship Programme.

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Copyright

Copyright © 2019 Tanwi Bandyopadhyay and Ujjal Debnath. 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.

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