Advances in Mathematical Physics

Volume 2018, Article ID 3468381, 9 pages

https://doi.org/10.1155/2018/3468381

## Classical and Quantum Exact Solutions for a FRW Multiscalar Field Cosmology with an Exponential Potential Driven Inflation

^{1}Departamento de Física, DCeI, Universidad de Guanajuato-Campus León, 37150 León, GTO, Mexico^{2}School of Physics and Astronomy, University of Edinburgh, Edinburgh EH9 3FD, UK

Correspondence should be addressed to J. Socorro; xm.otgu.acisif@orrocos

Received 28 September 2018; Accepted 26 November 2018; Published 4 December 2018

Academic Editor: Eugen Radu

Copyright © 2018 J. Socorro 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.

#### Abstract

A flat Friedmann-Robertson-Walker (FRW) multiscalar field cosmology is studied with a particular potential of the form , which emerges as a relation between the time derivatives of the scalars field momenta. Classically, by employing the Hamiltonian formalism of two scalar fields with standard kinetic energy, exact solutions are found for the Einstein-Klein-Gordon (EKG) system for different scenarios specified by the parameter , as well as the e-folding function which is also computed. For the quantum scheme of this model, the corresponding Wheeler-DeWitt (WDW) equation is solved by applying an appropriate change of variables.

#### 1. Introduction

The inflation paradigm is considered the most accepted mechanism to explain many of the fundamental problems of the early stages in the evolution of our universe [1–4], such as the flatness, homogeneity, and isotropy observed in the present universe. Another important aspect of inflation is its ability to correlate cosmological scales that would otherwise be disconnected. Fluctuations generated during this early phase of inflation yield a primordial spectrum of density perturbation [5–8], which is nearly scale invariant, adiabatic, and Gaussian, which is in agreement with cosmological observations [9].

The single-field scalar models have been broadly used to describe the primordial expansion, the most phenomenological successful are those with a quintessence scalar field and slow-roll inflation [10–19]. However, if another component is included, i.e., a multiscalar field theory, it is also possible to produce an inflationary scenario [20, 21], even if the fields are noninteracting [16]. Even more the dynamical possibilities in multifield inflationary scenarios are considerably richer than in single-field models, such as in the primordial inflation perturbations analysis [22, 23] or the assisted inflation as discussed in [24], furthermore, the general assisted inflation as in [21]. In this sense the multiscalar fields’ cosmology is an attractive candidate to explain such phenomenon.

Recent works have shown that multiscalar field models are very fruitful when studying the early stages of the universe, such as the case in [25], where the authors perform a semianalytic study of preheating in inflationary models comprised of multiple scalar fields coupled nonminimally to gravity. In [26] the authors show the sensitivity of the cosmological observables to the reheating phase following inflation driven by many scalar fields, where they find that, for certain decay rate, reheating following multifield inflation can have a significant impact on the prediction of cosmological observables.

Indeed the multiscalar field models for inflation are of interest even on most recent studies, such as the above-mentioned cases; however, one of the most important features in such models is the potential associated with the scalar fields, and in many cases, the employed potentials are simple polynomial powers of the scalar fields or in other cases the employed potential is a series of lineally summed exponentials; however, it has been shown that a potential of the form is a good candidate to model the inflation phenomenon for multiscalar field theory, as discussed in previous work [27], and might provide a richer postinflation scenario.

Generally, in the studies of inflationary cosmology one employs the usual slow-roll approximation with the objective to extract simple expression for basics observable, such as the scalar and tensor spectral indices, the running of the scalar spectral index, and the tensor-to-scalar ratio. Moreover, in the slow-roll regime the set of EKG equations reduces in such a way that one can quickly obtain the solution of the scale factor. Nevertheless, there is an alternative approach which allows for an easy derivation of many inflation results. It is called Hamilton’s formulation, widely used in analytical mechanics. Using this method we obtain the exact solutions of the complete set of EKG equations without using the aforementioned approximation.

On the other hand, we implement a basic formulation in quantum cosmology by means of the Wheeler-DeWitt (WDW) equation. The WDW equation has been analyzed with different approaches in order to solve it, and there are several papers on the subject, such is the case in [28], where they debate what a typical wave function for the universe is. Reference [29] has a review on quantum cosmology where the problem of how the universe emerged from big bang singularity can no longer be neglected in the GUT epoch. Moreover, the best candidates for quantum solutions are those that have a damping behavior with respect to the scale factor, since only such wave functions allow for good classical solutions when using a Wentzel-Kramers-Brillouin (WKB) approximation for any scenario in the evolution of our universe [30, 31]. Furthermore, in the context of a single scalar field a family of scalar potentials is obtained in the Bohmian formalism [27, 32], where among others a general potential of the form is examined. Given this insight, for a two scalar field scenario we consider a potential of the form in order to solve the WDW equation.

This work is arranged as follows. In Section 2 we present the model with the action and the corresponding EKG equations for our cosmological model and the associated Hamiltonian density. In Section 3 general equations for the classical solutions of scale factor, scalar fields, and their associated momenta are derived in terms of the free parameters of the model. In Sections 3.1, 3.2, 3.3, and 3.4 the particular solutions and their number of e-folds are computed for different cases of the parameter. in Section 4 we use the Hamiltonian density to compute the corresponding WDW equation, which is solved by using a change of variables; an ansatz for the wave function is employed in terms of a generic function and parameters which are to be determined. In Sections 4.1 and 4.2 the corresponding wave function and their constants relations are presented for different cases of the parameter, which in turn is related to the parameter of the classical solutions. Finally, in Section 5 we present our conclusions for this work.

#### 2. The Model

We begin with the construction of two scalar fields cosmological paradigm, which requires canonical scalar fields . The action of a universe with the constitution of such fields iswhere is the Ricci scalar, is the corresponding scalar field potential, and the reduced Planck mass . The corresponding variations of (1), with respect to the metric and the scalar fields give the Einstein-Klein-Gordon field equationsThe line element to be considered in this work is the flat FRWwhere is the lapse function, which in a special gauge one can directly recover the cosmic time (), the scale factor is in the Misner’s parametrization, and the scalar function has an interval, . Consequently the field equations are

By building the corresponding Lagrangian and Hamiltonian densities for this cosmological model, classical solutions to Einstein-Klein-Gordon equations ((2)-(4)) can be found using the Hamilton’s approach, and the quantum formalism can be determined and solved. In that sense, we use the metric equation (5) into (1) havingwhere upper “" represents the first time derivative and the corresponding momenta are defined in the usual way . We obtainBy performing the variation of the canonical Lagrangian with respect to , i.e., , where , it implies the constraint . Hence the Hamiltonian density isIn the gauge and using the Hamilton equations and , we have the following set of equations:where . Given a particular form of the potential one can derive a relation between the time derivative of the momenta such as , provided that , where is a constant. Such connection can be obtained considering two different configurations of the potential: or , where and are constants, and is an arbitrary function. We select the simplest form of the potential :where is a constants and and are distinguishing parameters. This class of potential has been obtained by other methods; see, for instance, [27, 32–35]. Therefore the time derivative of the momenta is simply and , of which solutions arewhere and are integration constants. Henceforth we will employ this scheme in order to find analytic classic and quantum solutions.

#### 3. Classical Solutions

We start from the Hamilton equations (13) in order to find relations between the scale factor and the scalar fields, such as of which solutions arewhere and are integration constants, and they can be determined by suitable conditions. These expressions are indeed general relations, since they satisfy the Einstein-Klein-Gordon equations ((6)-(9)). Then by taking into account the constraint , we obtain the temporal dependence for which allows us to construct a master equation:where the parameters , , areSubsequently by analyzing the parameter we will obtain three different solutions.

##### 3.1. Solution for

Having implies that , so the integral to solve becomes then we parameterize such as , where measures the corresponding weight for each scalar field during inflation; so the constants (21) becomeThus becomeswhere is an integration constant. Using the relations from (13) and after some algebra, the solutions of the set of variables and arewhere () are all integration constants. In order to make the above results fulfill the EKG equations ((6)-(9)), all constants must satisfy that . Finally the scale factor for this case iswhere . Given that the scale factor is an exponential of an exponential function, it might exhibit a highly substantial growth.

##### 3.2. Solution for

For this case , so the integral to solve becomeswhere we include the minus sign in this equation, such the constant . Then we define , so we change variable as in order to integrate (31). Thus the solution to the momenta becomesUsing the relations from (13) and after some algebra, the solutions of the set of variables and arewhere () are all integration constants. In order to make the above results fulfill the EKG equations ((6)-(9)), all constants must satisfy that . Finally the scale factor becomeswhere . For this case, given that , one would expect that the scale factor grows slower than the previous case .

##### 3.3. Solution When

For this case we modify the relation between the momenta equation (15), by changing the sign in the constants, , and ; therefore the integral to solve becomes Thus iswhere . Using the relations from (13) and after some algebra, the solutions of the set of variables and arewhere () are integration constants. In order to fulfill the EKG equations ((6)-(9)), all constants must satisfy that . Finally the scale factor becomeswhere . For this case, given that , one would expect the scale factor to grow in a similar way as the previous case .

##### 3.4. Number of e-Folds

Inflation is characterised by the number of e-folds it expands during such period that corresponds to , where the primes represent the derivatives with respect to the cosmic time . The e-folding function is described by : computing the integral from to , where represents the time when the relevant cosmic microwave background (CMB) modes become superhorizon at 50-60 e-folds before inflation ends at ; and is the Hubble parameter. Although, in our prescription we use a proper time , we can evaluate the Hubble function in the corresponding gauge as .

At the end of inflation the expansion rate of the scale factor must be null which translates to or . From here we can compute the time when inflation ends () given each particular case. Table 1 shows the computation of the e-folding function and for each case given by the parameter.