Research Article | Open Access

Supriya Pan, Subenoy Chakraborty, "Will There Be Future Deceleration? A Study of Particle Creation Mechanism in Nonequilibrium Thermodynamics", *Advances in High Energy Physics*, vol. 2015, Article ID 654025, 10 pages, 2015. https://doi.org/10.1155/2015/654025

# Will There Be Future Deceleration? A Study of Particle Creation Mechanism in Nonequilibrium Thermodynamics

**Academic Editor:**Juan José Sanz-Cillero

#### Abstract

The paper deals with nonequilibrium thermodynamics based on adiabatic particle creation mechanism with the motivation of considering it as an alternative choice to explain the recent observed accelerating phase of the universe. Using Friedmann’s equations, it is shown that the deceleration parameter () can be obtained from the knowledge of the particle production rate (). Motivated by thermodynamical point of view, cosmological solutions are evaluated for the particle creation rates in three cosmic phases, namely, inflation, matter dominated era, and present late time acceleration. The deceleration parameter () is expressed as a function of the redshift parameter (), and its variation is presented graphically. Also, statefinder analysis has been presented graphically in three different phases of the universe. Finally, two noninteracting fluids with different particle creation rates are considered as cosmic substratum, and deceleration parameter () is evaluated. Whether more than one transition of is possible or not is examined by graphical representations.

#### 1. Introduction

There was a dramatic change in our knowledge of the evolution history of the universe based on the standard cosmology at the end of the last century due to some observational predictions from type Ia Supernova [1, 2] and others [3, 4]. Riess et al. [1] and Perlmutter et al. [2] observed that distant Supernovae at redshift and mag are found to be about 25% fainter than the prediction from standard cosmology, and, hence, they concluded that the universe at present is undergoing an accelerated expansion rather than deceleration (as predicted by the standard cosmology). This present accelerating phase was also supported by the cosmic microwave background (CMB) [3] and the baryon acoustic oscillations (BAO) [4]. The explanation of this unexpected accelerating phase is a great challenge to the theoretical physics. Since the discovery of this accelerating universe, people are trying to explain this observational fact in two different ways—either by modifying the Einstein gravity itself or by introducing some unknown kind of matter in the framework of Einstein gravity. In the second option, cosmological constant is the common choice for this unknown matter. But it suffers from two serious problems—the measured value of the cosmological constant being far below the prediction from quantum field theory and, secondly, the coincidence problem [5]. So, people choose this unknown matter as some kind of dynamical fluid with negative and time dependent equation of state, which is termed dark energy (DE). Though a lot of works have been done with several models of DE (see references [6–9] for reviews) still its origin is totally mysterious to us.

Among other possibilities to explain the present accelerating stage, inclusion of back reaction in the Einstein field equations through (−ve) effective pressure is much relevant in the context of cosmology, and the gravitational production of particles (radiation or cold dark matter (CDM)) provides a mechanism for cosmic acceleration [10–16]. In particular, in comparison with dark energy models, the particle creation scenario has a strong physical basis: the nonequilibrium thermodynamics. Also, the particle creation mechanism not only unifies the dark sectors (DE + DM) [15, 16] but also contains only one free parameter as we need only a single dark component (DM). Further, statistical Bayesian analysis with one free parameter should be preferred along with the hierarchy of cosmological models [17]. So, the present particle creation model, which simultaneously fits the observational data and alleviates the coincidence and fine-tuning problems, is better compared to the known (one-parameter) models, namely, (i) the concordance CDM which, however, suffers from the coincidence and fine-tuning problems [18–23] and (ii) the brane world cosmology [24] which does not fit the SNIa + BAO + CMB (shift-parameter) data [25, 26]. Furthermore, it should be mentioned that the thermodynamics of dark energy has been studied in equilibrium and nonequilibrium situations in the literature [27–32].

The homogeneous and isotropic flat FLRW model of the universe is chosen as an open thermodynamics system which is adiabatic in nature. Although the entropy per particle is constant for this system, still there is entropy production due to expansion of the universe (i.e., enlargement of the phase space) [33, 34]. As a result, the dissipative pressure (i.e., bulk viscous pressure) is linearly related to the particle creation rate [33–35]. Further, using the Friedmann equations, one can relate to the evolution of the universe (see (8) below). Choosing as a function of the Hubble parameter from thermodynamical view point, it is possible to describe different phases of the evolution of the universe and can be obtained as a function of , the redshift parameter. Finally, we consider two components of matter which have different particle creation rate [36], and has been evaluated and plotted to examine whether more than one transition of is possible or not. In formulation of the general theory of relativity, in terms of the spin connection coefficients, it has been shown [37] that the cosmological evolution of the metrics is induced by the dilaton without the inflation hypothesis and the term. Further, it is found that the dilaton evolution yields the vacuum creation of matter, and the dilaton vacuum energy plays a role of the dark energy. On the other hand, in the Hamiltonian approach to the gravitational model with the aid of Dirac-ADM foliation, Pervushin et al. [38] showed a natural separation of the dilatonic and gravitational dynamics in terms of the Maurer-Carton forms. As a result, the dominance of the Casimir vacuum energy of physical fields provides a good description of the type Ia Supernovae luminosity distance-redshift relation. Furthermore, introducing the uncertainty principle at the Planck’s epoch, it is found that the hierarchy of the universe’s energy scales is supported by the observational data. Also, this Hamiltonian dynamics of the model describe the effect of an intensive vacuum creation of gravitons and the minimal coupling scalar (Higgs) bosons in the early universe.

Moreover, the motivation of the present work in the framework of the particle creation mechanism comes from some recent related works. It has been shown in [39, 40] that the entire cosmic evolution from inflationary stage can be described by particle creation mechanism with some specific choices of the particle creation rates. As these works show late-time acceleration without any concept of dark energy, so, it is very interesting to think of the particle creation mechanism as an alternative way of explaining the idea of dark energy. The present work is an extension of these works by considering two fluid systems as the cosmic fluid. The paper is organized as follows. Section 2 deals with nonequilibrium thermodynamics in the background of particle creation mechanics, while several choices of as a function of the Hubble parameter are shown in Section 3 and the deceleration parameter has been presented both analytically and graphically. A field theoretic analysis of the particle creation mechanism is presented in Section 4. Section 5 is related to interacting two dark fluids having different particle creation rates and it is examined whether two transitions for are possible or not. Finally, there is a summary of the work in Section 6.

#### 2. Nonequilibrium Thermodynamics: Mechanism of Particle Creation

Suppose the homogeneous and isotropic flat FLRW model of the universe is chosen as an open thermodynamical system. The metric ansatz takes the formThen the Friedmann equations arewhere , is the Hubble rate, is the scale factor of the universe, and are the total energy density and the thermodynamical pressure of the cosmic fluid, is related to some dissipative phenomena (bulk viscous pressure), and the overdot denotes the derivative with respect to the cosmic time . It should be noted that there are several choices of and corresponding solutions in the literature [41, 42]. The energy conservation relation reads

As the particle number is not conserved (i.e., ), so, the modified particle number conservation equation takes the form [36]where is the particle number density, is the total number of particles in a comoving volume , is the particle flow vector, is the particle velocity, stands for the fluid expansion, represents the particle creation rate, and, notationally, . The sign of indicates creation (for ) or annihilation (for ) of particles, and, due to which adds some dissipative effect to the cosmic fluid, nonequilibrium thermodynamics comes into picture.

Now, from the Gibb’s equation using Clausius relation, we have [36]where “” represents entropy per particle and is the fluid temperature. Using the conservation relations (3) and (4), the variation of entropy can be expressed as [33–35]

Further, for simplicity, if we assume the thermal process to be adiabatic (i.e., ), then from (6) we have [33–35]

Thus, the dissipative pressure is completely characterized by the particle creation rate for the above simple (isentropic) thermodynamical system. In other words, the cosmic substratum may be considered as a perfect fluid with barotropic equation of state, , (), together with dissipative phenomena which comes into picture through the particle creation mechanism. Furthermore, although the “entropy per particle” is constant, still there is entropy generation due to particle creation, that is, enlargement of the phase space through expansion of the universe. So, in some sense, the nonequilibrium configuration is not the conventional one due to the effective bulk pressure, rather a state with equilibrium properties as well (but not the equilibrium era with ). Now, eliminating , , and from the Friedmann equations (2), the isentropic condition (7), and, using barotropic equation of state, , we obtain

The above equation shows that in case of adiabatic process, the particle creation rate is related to the evolution of the universe.

#### 3. Particle Creation Rate as a Function of the Hubble Parameter and Evolution of the Universe

Introducing the deceleration parameterand using (8), we have

In the following subsections, we shall choose as different functions of the Hubble parameter to describe different stages of evolution of the universe and examine whether obtained from (10) has any transition (from deceleration to acceleration or vice versa) or not. Furthermore, it would be worthwhile to see the statefinder analysis for the particle creation rates in different stages of our universe. The statefinder parameters were introduced by Sahni et al. [43] as a geometrical concept to filter several observationally supported dark energy models from other phenomenological dark energy models existing in the literature. They introduced two new geometrical variables , as follows [43]:

##### 3.1. Early Epochs

In the very early universe (starting from a regular vacuum) most of the particle creation effectively takes place and from thermodynamic point of view we have the following [44].(i)At the beginning of the expansion, there should be maximal entropy production rate (i.e., maximal particle creation rate) so that universe evolves from nonequilibrium thermodynamical state to equilibrium era with the expansion of the universe.(ii)A regular (true) vacuum for radiation initially, that is, , as .(iii) in the very early universe so that the created radiation behaves as thermalized heat bath and, subsequently, the creation rate should fall slower than expansion rate and particle creation becomes dynamically insignificant.

Now, according to Gunzig et al. [45], the simplest choice satisfying the above requirements is that particle creation rate is proportional to the energy density; that is, , where is a proportionality constant. For this choice of , can be solved from (8) aswhere is related to as . and are chosen to be the values of the Hubble parameter and the scale factor, respectively, at some instant. We note that as , constant, indicating an exponential expansion () in the inflationary era, while, for , indicates the standard FLRW cosmology (). So, if we identify “” at some intermediate value of “,” where, , that is, a transition from de Sitter accelerating phase to the standard decelerating radiation phase, then we have , and (8) gives .

Now, using (10), we obtainwhere the redshift parameter is defined as .

Figure 1 shows the transition of the deceleration parameter from early inflationary era to the decelerated radiation era. Figures 2 and 3 display the graphical behavior of the statefinder parameters showing that, in early stage of the universe, changes its sign from +ve ( inflationary era) to −ve ( decelerating phase), while stays positive throughout the transition.

##### 3.2. Intermediate Decelerating Phase

Here, the simple natural choice is . It should be noted that this choice of does not satisfy the third thermodynamical requirement (mentioned above) at the early universe. Also the solution will not satisfy the above condition (ii) of Section 3.1. In this case does not depend on the expansion rate, it only depends on . For radiation (i.e., ) era, , while for matter dominated era (i.e., ) . So, if , then we have deceleration in both the epochs as in standard cosmology, while there will be acceleration, if .

The solution for the Hubble parameter and the scale factor are given bywhere , which represents the usual power law expansion of the universe in standard cosmology with particle production rate decreasing as .

The statefinder parameters and in this case are constant with the valueswhich indicates that, for , and change their sign. becomes +ve, while becomes −ve.

##### 3.3. Late Time Evolution: Accelerated Expansion

In this case the thermodynamical requirements of Section 3.1 are modified as follows [45].(i)There should be minimum entropy production rate at the beginning of the late time accelerated expansion and the universe again becomes nonequilibrium thermodynamically.(ii)The late time false vacuum should have , as .(iii)The creation rate should be faster than the expansion rate.

We shall show that another simple choice of , namely, , that is, , where, is a proportionality constant, will satisfy these requirements. For this choice of , the Hubble parameter is related to the scale factor aswhere is some intermediate value of “,” such that

So, we have a transition from the standard cosmological era () to late time acceleration (), and ’s can be identified as the value of the scale factor at the instant of transition (). The deceleration parameter now has the expressionwhere the redshift parameter is defined as . Figure 4 displays the transition of the universe from matter dominated era to the present late time acceleration. Further, we have presented the statefinder analysis in Figures 5 and 6 for and parameters, respectively.

#### 4. Field Theoretic Analysis and Particle Creation

This section deals with particle creation from vacuum using quantum field theory [46]. In particular, the quantum effect of particle creation is considered in the context of thermodynamics of open systems and is interpreted as an additional negative pressure.

The energy-momentum tensor corresponding to the quantum vacuum energy is

So, the Friedmann equations and the corresponding energy conservation equation of a perfect fluid are now modified aswhich shows energy transfer from the decaying vacuum to matter. This modified energy conservation equation can be considered as the energy balance equation for an imperfect fluid with bulk viscous pressure:

Now, if the perfect fluid is considered as a scalar field with potential , that is,then the Einstein field equations (20) and (21) become, respectively (taking ),and the evolution equation (22) of the scalar field is given by

So, we havewhere “” stands for the differentiation with respect to the scale factor “.” Hence, for adiabatic process the particle creation rate can be written aswhere is the state finder parameter [43] and is the usual deceleration parameter.

It may be noted that, if we have only quantum energy and there is no other matter, then the energy conservation equation (22) demands “” should be a constant. Also, from (8), we have constant particle creation rate .

#### 5. Two Noninteracting Fluids as Cosmic Substratum and Particle Creations

In this section, we suppose that the present open thermodynamical system contains two noninteracting dark fluids which have different particle creation rates. Let, () and () be the energy density and thermodynamic pressure of the fluids, respectively. Suppose that () denote the number density of the two fluids having balance equations [36]:where and . The above equations imply that there is creation of particles of fluid-1, while particles of fluid-2 decay. Now, combining equations in (29), the total number of particles, , will have the balance equation

So, the total number of particles will remain conserve, if , that is, .

Again from the isentropic condition in (7), the dissipative (bulk) pressures of the matter components are given by

As a consequence, the energy conservation relations arewhich imply an exchange of energy between the two fluids. In this connection, it should be mentioned that Barrow and Clifton [47] found cosmological solutions with energy exchange. Now, if and are the equations of state of the two fluid components, respectively, then, from the above two conservation relations, the effective equations of state parameters are

Thus, from the Einstein equations we have

Then, the deceleration parameter can be written as [48]

In particular, if (say), then the above form of the deceleration parameter () reads

Figures 7–12 describe how the deceleration parameter behaves with the Hubble parameter for different choices of the particle creation rate (equal or unequal), and it also matches with the present day observations. It should be mentioned that the choice for and in Figure 9 is not fixed; rather the cosmic evolution can be obtained for any and (where , , and are constants). Similarly, for any PCR of the form (for Figure 12) (where , , and are constants) we can have the same evolution of the universe.

#### 6. Discussions and Future Prospects

The present work deals with nonequilibrium thermodynamics based on particle creation formalism. In the context of universal thermodynamics, flat FLRW model of the universe is considered as the open thermodynamical system. Although, cosmic fluid is chosen in the form of a perfect fluid, dissipative effect in the form of bulk viscous pressure arises due to the particle production mechanism. For simplicity of calculations, we are restricted to the adiabatic process where the dissipative pressure is linearly related to the particle production rate (). From thermodynamic point of view, is chosen as a function of the Hubble parameter (), and the deceleration parameter is shown to be a function of the redshift parameter. In particular, by proper choices of , cosmological solutions are evaluated, and the deceleration parameter is presented graphically in Figures 1 and 4. The graphs show a transition from early inflationary stage to the radiation dominated era (Figure 1) and also the transition from matter dominated era to the present late time acceleration (Figure 4). Further, we have presented the statefinder analysis in early (Figures 2 and 3), intermediate ( and are constant in this stage), and late phases (Figures 5 and 6), respectively. Then a field theoretic analysis has been shown for the particle creation mechanism in Section 4. Finally, in Section 5, a combination of noninteracting two perfect fluids having different particle creation rate is considered as a cosmic substratum, and the deceleration parameter is evaluated. The behavior of the deceleration parameter is examined graphically in Figures 7–12. Figures 7, 8, 10, and 11 show two transitions of —one in the early epoch from acceleration to deceleration and the other one corresponding to the transition in the recent past from deceleration to present accelerating stage. Figures 7 and 8 correspond to two different choices of unequal particle creation parameters, while, for two distinct equal particle creation rates, the variations of are presented in Figures 10 and 11. There are three distinct transitions of for unequal and equal particle creation parameters in Figures 9 and 12, respectively. Both the figures show that there is a chance of our universe to decelerate again in future from the present accelerating stage. Thus, theoretically, considering noninteracting two-fluid system as cosmic substratum, it is possible to have again a decelerating phase of the universe in future. Therefore, we may conclude that the present observed accelerating phase is due to nonequilibrium thermodynamics having particle creation processes, or, in other words, in addition to the presently known two possibilities (namely, modification of Einstein gravity or introduction of some unknown exotic fluid, i.e., DE) for explaining the recent observations, nonequilibrium thermodynamics through particle creation mechanism may not only explain the late time acceleration but also exhibit early inflationary scenario and predict future transition to decelerating era again, and this transient phenomenon is supported by the works in [39, 49, 50]. Finally, we remark that only future evolution of the universe can test whether our prediction from particle creation mechanism is correct or wrong.

#### Conflict of Interests

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

#### Acknowledgments

Supriya Pan acknowledges CSIR, Government of India for financial support through SRF scheme (File no. 09/096 (0749)/2012-EMR-I). Subenoy Chakraborty thanks UGC-DRS programme at the Department of Mathematics, Jadavpur University. Both the authors thank Inter University Centre for Astronomy and Astrophysics (IUCAA), Pune, India, for their warm hospitality as a part of the work was done during a visit there. The authors thank Prof. J.D. Barrow for introducing some references which were useful for the present work, and their other works. Finally, they are thankful to the anonymous referees for their valuable comments on the earlier version of the paper which helped us to improve the paper considerably.

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#### Copyright

Copyright © 2015 Supriya Pan and Subenoy Chakraborty. 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}.