Advances in High Energy Physics

Volume 2018, Article ID 2958605, 9 pages

https://doi.org/10.1155/2018/2958605

## On Chaplygin Gas Braneworld Inflation with Monomial Potential

^{1}Equipe Physique Quantique et Applications, Laboratoire de Physique de la Matière Condensée, Faculté des Sciences Ben M’sik, Université Hassan II, Casablanca, Morocco^{2}Equipe de Recherche Subatomique et Applications, Laboratoire de Physique de la Matière Condensée, Faculté des Sciences Ben M’sik, Université Hassan II, Casablanca, Morocco^{3}Groupement National de Physique des Hautes Energies, Focal Point, LabUFR-PHE, Rabat, Morocco

Correspondence should be addressed to A. Safsafi; rf.oohay@lida_ifasfas

Received 26 July 2017; Revised 1 October 2017; Accepted 4 October 2017; Published 25 June 2018

Academic Editor: Orlando Luongo

Copyright © 2018 A. Safsafi 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 SCOAP^{3}.

#### Abstract

We study the Chaplygin gas model as a candidate for inflation in the framework of the Randall-Sundrum type II braneworld model. We consider the original and generalized Chaplygin gas model in the presence of monomial potential. The inflationary spectrum perturbation parameters are reformulated and evaluated in the high-energy limit and we found that they depend on several parameters. We also showed that these perturbation parameters are widely compatible with the recent Planck data for a particular choice of the parameters space of the model. A suitable observational central value of is also obtained in the case of original and generalized Chaplygin gas.

#### 1. Introduction

It is widely believed that the early universe underwent a period of accelerated expansion called inflation [1], which has become the standard paradigm of modern cosmology. Inflation model has been proposed as an attempt to solve the shortcoming of the standard Big-Bang model of cosmology, known usually as the flatness and the horizon problem [2]. Inflation is the candidate for understanding the physics of the very early universe, typing the evolution of the universe to the properties of one or more scalar inflaton fields, responsible for creating an accelerating expanding universe [3]. Recently, a great amount of work has been invested in studying the inflationary model with several candidates. Among these candidates is the Chaplygin gas model [4]. This model was also used to describe a mysterious dark sector, so-called dark energy and dark matter [5, 6], and the early universe [7]. In cosmology, dark energy is a form of unknown energy dominating the universe with a hugely negative pressure [8]. It is demonstrated by various astrophysical observations, including the accelerating universe [9]. Recall that the dark energy is defined by an exotic equation of state of the form , where and are the pressure and energy density of dark energy, while is the equation of state parameter of the dark energy [10]. There are several candidates to describe the dark matter and dark energy in the cosmology [11]. Among them are -essence model [12], the CDM model [13], cosmological constant [14], tachyon model [15], and quintessence model [16]. There are different kinds of the Chaplygin gas model which have been proposed in the literature, for example, the general model named extended Chaplygin gas which is defined by an exotic equation of state of the form [17, 18] where , , are universal positive constants and . In recent years the extended Chaplygin gas was the subject of several cosmological and phenomenological studies [19, 20]. Note that when , we obtain the case of modified Chaplygin gas [21, 22]. The original Chaplygin gas corresponds to the case of and ; this type was studied in [23]. In the case of and it is known as the generalized Chaplygin gas (GCG) [24, 25] and finally for and it corresponds to the CDM model [13]. Further, the Chaplygin gas models have been studied in different paper. In [26] the authors have studied the interaction of the dark energy with some fluids specially Chaplygin gas in the context of theory. In [27], the authors have proposed an attempt for emergent universe scenario with modified Chaplygin gas and have shown that it is not possible to have emergent scenario with model. In another work [20], Pourhassan and Kahya have examined extended model of Chaplygin gas equation of state for which it recovers barotropic fluid with quadratic equation of state and have found that extended Chaplygin gas may be a more appropriate model than generalized and modified Chaplygin gas and give a best fit with the observational data.

On the other hand, the Chaplygin gas inspired inflation model [28] was the subject of several cosmological and phenomenological studies. In this context, the scalar field is usually the standard inflaton field, where the energy density can be extrapolated to obtain a successful inflationary period with a Chaplygin gas model. In the same context, a work has been done by Herrera [29] where the brane-Chaplygin inflationary model was studied in great detail and considered as a viable alternative model that can provide an accelerated expansion of the early universe. In extension of [29], similar work was performed for the case of the tachyon-Chaplygin inflationary model by using an exponential potential in the high-energy regime [30].

In the present paper, we are going to use the Randall-Sundrum II braneworld model to study the original and generalized Chaplygin gas as a candidate for the primordial inflation by assuming that the matter source on the brane consists of a Chaplygin gas. The Chaplygin gas emerges as an effective fluid of a generalized -brane in a (, ) spacetime, where the action can be written as a generalized Born–Infeld action [25]. These models have been extensively studied in the literature [7]. The motivation for introducing Chaplygin-brane scenarios is the increasing interest in higher-dimensional cosmological models, motivated by superstring theory, where the matter fields are confined to a lower-dimensional brane while gravity can propagate in the bulk. On the other hand, the Chaplygin gas model seems to be a viable alternative to models that provide an accelerated expansion of the early universe. Our aim is to quantify the modifications of the Chaplygin inspired inflation in the braneworld scenario. We use the monomial potential to study various perturbation spectrum parameters such as the scalar spectral index and the ratio and the running of the scalar spectral index in the high-energy limit, particularly for a suitable choice of the different parameters. We show that the inflation parameters are in good agreement with recent Planck 2015 data [31].

An outline of the remainder of this paper is as follows: We first begin in Section 2, by recalling the standard inflation and Chaplygin gas braneworld inflation formalism, in particular the modified Friedmann equation. In Section 3, we study different perturbation spectrum concerning monomial potential in the high-energy limit, and we present our results for original and generalized Chaplygin gas on the brane. The last section is devoted to conclusion.

#### 2. Generalized Chaplygin Gas Braneworld Inflation

##### 2.1. Inflationary Universe

In this section we propose a short description on standard inflation formalism to enable readers to understand the meanings of terms here involved. Inflation is the period of the early universe that undergoes an accelerating phase [1]. This period is equivalent to . The candidate that can yield this acceleration phase and is responsible for driving inflation is a scalar field named inflaton field. The pressure and energy of the inflaton field are given by and , where is the scalar potential. The Friedmann equation reads During inflation, the potential depends only on the inflaton field . It is supposed that the field equation is well-approximated by The condition for acceleration requires that . This is called the slow-roll approximation. With very small , the Friedmann equation is approximately , and the flatness conditions and , where and The amount of inflation can be measured in terms of the -folding number given by equation , where and are the values of the scalar field at the epoch when the cosmological scales exit the horizon and at the end of inflation, respectively.

The small quantum fluctuations in the scalar field lead to fluctuations in the energy density which was studied in a perturbative theory [32]. As discussed in [33] quantum fluctuations effects of the inflaton are generally negligible, since the coupling of the scalar field to bulk gravitational fluctuations only modifies the usual 4D predictions at the next order in the slow-roll expansion. So, one can define the power spectrum of the curvature perturbations as . On the other hand, the quantum fluctuations in the scalar field lead also to fluctuations in the metric [34]. In this way, one can define the amplitude of tensor perturbations as . These results lead to the ratio of tensor-to-scalar perturbations . In relation to , the scalar spectral index is defined as . Reference [3] is recommended for further reading on inflation.

##### 2.2. Generalized Chaplygin Gas on the Brane

Braneworld inflation [35] is a particular kind of inflation models. It is based primarily on the cosmological model Randall-Sundrum type II which describes the universe in five dimensions with the presence of a brane that includes all ordinary matter. The generalized Chaplygin gas is a perfect fluid characterized by the following equation of state [36]:where and are the energy density and pressure of the generalized Chaplygin gas, respectively, is a constant satisfying , and is a positive constant.

Inserting (2) in the equation of conservation of energy , we obtain the following expression for the energy density:where and are the current values of the scale factor and the generalized Chaplygin gas energy density, respectively.

The modification of (5) is realized from an extrapolation of (3), where the density matter is replaced by the scalar field as .

In this section, we will recall briefly some basic facts of Randall-Sundrum type II braneworld model [37, 38]. We suppose that the universe is filled with a perfect fluid with energy density and pressure in which the Friedmann equation is modified from its usual form [29]where defines the Hubble parameter, represents the matter confined to the brane, , is the current cosmological constant, and is an integration constant and thus transmitting bulk graviton influence onto the brane. This term appears as a form of “dark radiation” and may be fixed by observation [39]. However, during inflation this term is rapidly diluted, so we will neglect it, where is the brane tension and is the four-dimensional Planck mass, which is related to the five-dimensional by . Note that the crucial correction to standard inflation is given by the density quadratic term . Note also that, in the limit , we recover standard four-dimensional general relativistic results.

The Friedmann equation will become [30]In four-dimensional general relativity, the condition for inflation is , that is, , where and , is the scalar potential, and is the inflaton field; the scalar field satisfies the Klein-Gordon equation: Note that , , and . During inflation, the relation between the energy density and the scalar potential is ; we consider the slow-roll approximations and ; the Friedmann equation reduces toThe term in square brackets is the brane-modification to the standard slow-roll expression for the Hubble rate.

We consider the slow-roll parameters, in the Randall-Sundrum type II braneworld model [33]. The two first parameters are given for generalized Chaplygin gas model by The inflationary phase ends when or is equal to one; during inflation, the conditions and are satisfied. Note that, at low energies, , the slow-roll parameters reduce to the standard inflation.

In addition, the number of -foldings is given bywhere and are the values of the potentials at the horizon exit and the end of inflation, respectively.

The inflationary spectrum perturbation is produced by quantum fluctuations of fields around their homogeneous background values. The small quantum fluctuations in the scalar field lead to fluctuations in the energy density and in the metric; for that, we define the power spectrum of the curvature perturbations by [33]By using (7) and (10), we find the expression for power spectrum of the curvature perturbations: Another important inflationary spectrum parameter is the amplitude of the tensorial perturbations , describing the primordial gravitational wave perturbations produced by a period of extreme slow-roll inflation, which is defined by [34] where and . Note that, in the low-energy limit , we have and, in the high-energy limit , .

We define the tensor-to-scalar ratio as Here corresponds to the case , the value when the universe scale crosses the Hubble horizon during inflation. From (11) and (12), the tensor-to-scalar ratio is given by The scalar spectral index is presented by [32]The running of the scalar index is also defined as Note that, in the limit , the perturbation spectrum parameters coincide with brane inflation [33], in particular for . Also, in the low-energy limit, , the slow-parameters reduce to the standard form [28].

In what follows, we shall apply the above braneworld formalism with a monomial potential in the high-energy limit; that is, , in relation to recent Planck data.

#### 3. Chaplygin Gas with Monomial Potential

##### 3.1. Original Chaplygin Gas

In the following, we will concentrate on the original Chaplygin gas; it is reached as a special case of the general Chaplygin gas and is proposed as possible explanation of the acceleration of the current universe. The original Chaplygin gas model has been extensively studied. For example, [40] studied the behaviour of density perturbations in a universe dominated by the Chaplygin gas and found that, in spite of presenting negative pressure of Chaplygin gas, it is stable at small scale, opposite to in general what happens with perfect fluids with negative pressure. In [23], the authors have focused on studying a Chaplygin gas model in braneworld inflation with an exponential potential and have obtained that, for negligible and small running of the scalar spectral index, the inflationary parameters are in good agreement with observation data. In another example [41], the authors have analysed a phase space of the evolution for a Friedmann Robertson Walker universe driven by an interaction of Chaplygin gas and dark matter; their results are derived from continuity equations, which means that they are independent of any theories of gravity. The original Chaplygin gas model is characterized by an exotic equation of state of the form where is a positive constant.

In this section we will propose to investigate monomial potential in braneworld context with generalized Chaplygin gas. This potential was used in a very recent model in different work. In the paper [42] the authors study the attractors solutions of the dynamical system of a scalar field endowed with monomial potentials and show that the behaviour found for monomial potentials is typical in realistic inflationary models. Furthermore, Zarrouki et al. have studied various inflationary spectrum perturbation parameters with three types of potentials; they have shown that the monomial potential provides the best fit results to observations data [43]. This potential is given by where is a positive integer and is a parameter of dimension . In order to derive the inflationary parameters , , and , let us consider the monomial potential. In this case, the scalar spectral index , the ratio , and the running of the scalar index become Note that, in the limit , the scalar spectral index , the ratio , and coincide with those in [43].

Although we have analytic results for slow-roll parameters and the number of -foldings, it is not easy to solve them to obtain at which the observables , , and should be evaluated. For this, we proceed numerically by finding and using (9) to obtain while making sure that the slow-roll parameters remain small in this range of .

To complete our study with original Chaplygin gas, we analyse the variations of the perturbation spectrum parameters with respect to for various values of . We can see that these observables depend on several parameters. For this purpose, we take the inflationary scale , the brane tension value (, and [29], in order to obtain consistent perturbation spectrum parameters with recent Planck data.

Figure 1 presents the variations of scalar spectral index as a function of -folding number . The scalar spectral index has an increasing behaviour as we increase the -folding number . We also note that the values of are found to be consistent with the Planck data for large domain of and the central value of . is obtained in particular for .