Advances in High Energy Physics

Volume 2019, Article ID 9080218, 10 pages

https://doi.org/10.1155/2019/9080218

## Noncommutativity in Effective Loop Quantum Cosmology

^{1}Unidad Profesional Interdisciplinaria de Ingeniería Campus Guanajuato del Instituto Politécnico Nacional, Av. Mineral de Valenciana No. 200, Col. Fraccionamiento Industrial Puerto Interior, 36275 Silao de la Victoria, GTO, Mexico^{2}Departamento de Física, División de Ciencias e Ingenierías, Campus León, Universidad de Guanajuato, 37150 León, Mexico

Correspondence should be addressed to Abraham Espinoza-García; xm.npi@azonipsea

Received 6 September 2018; Revised 7 December 2018; Accepted 17 January 2019; Published 7 February 2019

Academic Editor: Edward Sarkisyan-Grinbaum

Copyright © 2019 Abraham Espinoza-García 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 construct a noncommutative extension of the Loop Quantum Cosmology effective scheme for the flat FLRW model with a free scalar field via a theta deformation. Firstly, a deformation is implemented in the configuration sector, among the holonomy variable and the matter degree of freedom. We show that this type of noncommutativity retains, to some degree, key features of the Loop Quantum Cosmology paradigm for a free field. Secondly, a deformation is implemented in the momentum sector, among the momentum associated with the holonomy variable and the momentum associated with the matter field. We show that in this latter case the scalar field energy density is the same as the one in standard Loop Quantum Cosmology.

#### 1. Introduction

The idea of noncommutativity in spacetime is not new (1947) [1]. It was proposed as an attempt to regularize Quantum Field Theory before the renormalization program was established. Due to its nonlocal behavior, noncommutativity was quickly forgotten after renormalization proved to be successful. In the 1970s M. Flato and coworkers proposed an alternative path to quantization [2–4], in which a deformation of the Poisson structure of classical phase space is performed and is encoded in the Moyal -product [5], and generalizations of it (for a review see [6]). In the early 1980s mathematicians led by A. Connes succeeded in formulating what they called Noncommutative Geometry [7], motivated by generalizing a classic theorem characterizing algebras.

At the end of the last century the noncommutative paradigm was resurrected, mainly due to results in String Theory [8, 9], in which Yang-Mills theories in a noncommutative space arise in different circumstances as effective theories when taking certain limits, for instance, the low energy limit. This renewed interest has led to a deeper understanding, from the physical and mathematical points of view, of noncommutative field theory (for a review see [10, 11]). Additionally, it is believed that in a full quantum theory of gravity the continuum picture of spacetime would no longer be consistent at distances comparable to the Planck length ; a quantization of spacetime itself could be in order.

A possible way to model these effects could be via an uncertainty relation for the spacetime coordinates of the formThis commutation relation is the starting point for noncommutative field theories. Attempts to implement this idea for the gravitational field have led to different proposals for a noncommutative theory of gravity (see, for example, [12–15]). In particular, a noncommutative generalization of Loop Quantum Gravity (LQG) was constructed in [15]. Different incarnations of noncommutative gravity have a common feature; they are highly nonlinear theories, which makes them very difficult to work with.

A possible way to study noncommutativity effects in the early universe was proposed by García-Compeán et al. [16]. They implemented noncommutativity in configuration space, in contrast to noncommutative spacetime, but only after a symmetry reduction of spacetime had been imposed and the Wheeler-DeWitt quantization had been carried, giving rise to a noncommutative quantum cosmology, mathematically similar to the noncommutative quantum mechanics constructed in [17–19]. Later, G. D. Barbosa and N. Pinto-Neto [20] introduced this minisuperspace noncommutativity already at the classical level. The idea is that, perhaps, this effective noncommutativity could incorporate novel effects and insights of a full quantum theory of the gravitational field, alongside with providing a simple framework for studying the implications of such possible noncommutative effects in the early universe through cosmological models. Since the publication of these two seminal investigations, some works along this line have been conducted. For instance, the noncommutativity of the FLRW cosmology has been studied, as well as some of the Bianchi Class A models [21, 22]. Quantum black holes have also been investigated within this framework [23].

On the other hand, LQG [24, 25] is an attempt to quantize the gravitational field taking seriously the lessons from General Relativity; that is, it aims at a full nonperturbative background independent quantization of General Relativity. It could be said that LQG is an improvement of the canonical Weeler-DeWitt quantization programme. On the other hand, Loop Quantum Cosmology (LQC) [26, 27] is the quantization of cosmological, symmetry reduced, models following closely the ideas and methods of LQG. In this way, the LQC of the FLRW and some of the Bianchi Class A models in the presence of a massless scalar field, employed as internal time, have been constructed [28–35]. In particular, as a result of the underlying quantum geometry, it has been shown that the loop quantization of the FLRW models features a bounce which enables the resolution of the cosmological singularity [36]. The LQC of the inhomogeneous Gowdy model has also been constructed [37].

As a consequence of loop quantization, the Wheeler-DeWitt equation is no longer a differential equation, but a difference equation, which is difficult to work with even in the simplest models. In order to extract physics, effective equations based on a geometrical formulation of quantum mechanics have been employed to study the outcome of loop quantum corrections in cosmological models [38]. The relevance for using the effective equations in LQC lies in the fact that this effective scheme is an excellent approximation to the underlying quantum theory. This conclusion can be drawn from [39, 40]. In both works, numerical simulations for the effective dynamics in LQC are employed. In the first one, the flat FRW with a free scalar field is studied; and the second one, the anisotropic vacuum Bianchi-I model, is address.

Recently, works that focus on the possible relation, at different physical/mathematical levels, among noncommutativity and LQG have been conducted. For instance, an emergent noncommutativity in LQG is found in [41] when constructing position operators for spin-networks; a relation between LQG-inspired deformations of spacetime and -Minkowski noncommutative spacetime is established in [42, 43].

The present investigation aims at constructing a noncommutative effective scheme for the flat FLRW model in the presence of a free scalar field, and establishing whether such noncommutative scheme could be compatible with the LQC paradigm, in the sense of retaining key features of the LQC of the flat FLRW model. Along this lines, our work could be related to a minisuperspace approximation of a more fundamental noncommutative construction based on the LQG approach, such as the one in [15], signaling possible restrictions on the way noncommutativity is to be incorporated in such general frameworks. While being related, our philosophy is different from the class of works cited in the above paragraph since we implement a simple type of noncommutativity in an LQG-related model, rather than trying to obtain noncommutativity from LQG or LQG-inspired models.

The manuscript is organized as follows: In Section 2 we introduce the loop variables for the flat FLRW model with a free standard scalar field and the corresponding effective scheme. In Section 3 we recall a way in which noncommutativity can be implemented in Classical Mechanics through a deformation of the product. Section 4 is devoted to construct a noncommutative model for the Effective Loop Quantum Cosmology of the flat FLRW model with the help of the method introduced in Section 3, along the lines of [20]. In the remaining part of this section we recall the canonical formulation of the flat FLRW model in metric variables, in the presence of a free scalar field.

##### 1.1. FLRW Model in the Metric Variables

The line element of a spatially homogeneous and isotropic universe iswhere is the scale factor, is the lapse function, and is the curvature constant, which can take values 0, 1, and , which corresponds to a flat, closed, and open universe, respectively. The corresponding Ricci scalar isWorking with the Einstein-Hilbert actionthe Lagrangian for a flat universe takes the formwhere is Newton’s constant. The spatial slice is topologically ; since this space is noncompact the spatial integral in the Lagrangian diverges. Restricting the integration to a fiducial cell (which we can safely do due to homogeneity), taking a homogeneous scalar field we havewhere is the coordinate volume of the auxiliary cell . The momenta arewhere we have set the fiducial volume equal to one. In the LQC paradigm a great deal of care has been taken in order to ensure that the physical content of the theory does not take into account this fiducial structure. Taking the Legendre transform, , where acts as a Lagrange multiplier which imposes the Hamiltonian constraint , we haveWith the canonical relations and the Hamiltonian at hand, Hamilton equationsreadwhere has been set. Taking into account the field equations and the Hamiltonian constraint one arrives at the Friedmann equation is called the Hubble parameter, and, in this particular case of a free standard homogeneous scalar field, () is the energy density.

#### 2. Connection Variables and Effective Dynamics

##### 2.1. The FLRW Model in the Ashtekar-Barbero Variables

In this section, we recall the formulation of the flat FLRW model in the Ashtekar-Barbero variables, with a free massless scalar field. The Ashtekar-Barbero variables cast General Relativity in the form of a gauge theory, in which phase space is described by an gauge connection, the Ashtekar-Barbero connection , and its canonical conjugate momentum, the densitized triad . In both, the Ashtekar-Barbero and the densitized triad, , denote internal indices while , denote spatial indices. These quantities are defined aswhere , with and being the triad and cotriad, respectively, which satisfied and ; is defined through the spin connection compatible with the triad by the relation with the totally antisymmetric symbol and ( being the usual spatial covariant derivative); is a real constant called the Barbero-Immirzi parameter. The canonical pair has the following Poisson structurewith being the Dirac delta distribution on the space-like hypersurface . In these variables, the gravitational Hamiltonian density takes the formwhere is the curvature of the Ashtekar-Barbero connection and is the determinant of the densitized triad.

From the gravitational Hamiltonian density (15), one can cast the gravitational Hamiltonian throughin the case for spatially flat homogeneous models reduces to [27]where the integral is taken in a fiducial cell . When imposing also isotropy, the connection and triad can be described by parameters and , respectively, defined by [27]where is a fiducial flat metric and , are constant triad and cotriad compatible with ; is the volume of with respect to . These variables do not depend on the choice of the fiducial metric. The relation among these variables and the usual geometrodynamical variables iswhere the canonical relations for this last two variables obeyPerforming the following change of variablesthe Hamiltonian (17), with a free massless scalar field as the matter content, takes the formwith the canonical relations for and beingThe holonomy correction due to Quantum Gravity effects is coded in the replacement [27]where is the smallest eigenvalue of the area operator in the full Loop Quantum Gravity [25]. The resulting effective Hamiltonian is thus given byBefore we proceed any further, it is convenient to address some issues that exist regarding the lapse function . In earlier treatments of the FLRW with a free scalar field in LQC, the classical dynamics were studied in terms of the proper time (which corresponds to ) and after the quantization of the Hamiltonian constraint the dynamics were describe by an internal time defined by the scalar field [28]. All these investigations were done numerically. On the other hand, in [44] they obtain an analytical soluble model for the FLRW with a free scalar field in the LQC paradigm, employing the scalar field (using ) as an internal clock to describe the (effective) dynamics already at the classical level. Furthermore, they show that either choice of the lapse function, or , at the classical level, then proceeding to quantize the Hamiltonian constraint, results on slightly different factor orderings in the quantize Hamiltonian constraint. For details see [44]. From this point on and through the manuscript, we will use .

Taking into account the discussion of the last paragraph for the Hamiltonian constraint (25), the field equations are Since , where is the Hubble parameter, then, taking into account the effective Hamiltonian constraint, , and the field equation for , we have that the Friedmann equation now reads [45]where and is the maximum value that can take in view of the effective Hamiltonian constraint, that is, . The turning points of the volume function occur at , which correspond to a bounce. Equation (27) is the modified Friedmann equation, which incorporates holonomy corrections due to Loop Quantum Gravity. In the limit (no area gap) we recover the ordinary Friedmann equation (12).

The relational evolution of in terms of is given bywhere we have used the field equations for and and the effective Hamiltonian constraint.

#### 3. Deformations in Classical and Quantum Mechanics

The ideas of deformed minisuperspace, in connection with noncommutative cosmology, were introduced in the seminal work of García-Compeán et al. [16]. The introduction of a deformation to the minisuperspace, in order to incorporate an effective noncommutativity, made it possible to avoid working with a noncommutative theory of gravity and still get relevant physics of the Kantoswki-Sachs cosmological model. In the canonical quantum cosmological scenario, the Wheeler-DeWitt equation is responsible for the description of the quantum behavior of the Universe. An alternative approach to study quantum mechanical effects is to introduce deformations to the Poisson structure of classical phase space; the approach is an equivalent path to quantization and is part of a complete and consistent type of quantization known as deformation quantization [2–4]. In [46], the authors apply the deformation quantization formalism to cosmological models in the flat minisuperspace. Within this setup, relevant minisuperspace cosmological models are studied in detail, namely, the de Sitter and Katowski-Sachs, among others.

In the deformation phase space approach, the deformation is introduced by the Moyal brackets , where the product between functions is replaced by the Moyal -productsuch thatwhere the matrices and are assume to be antisymmetric and represent the noncommutativity in the coordinates and the momenta, respectively. The resulting -deformed algebra for the phase space isAn alternative to derive an algebra similar to (31) is making the following transformation on the classical phase variables where particular expressions for the deformations have been considered, namely, and . The resulting algebra is the same as (31), but the Poisson brackets are different in the two algebras. For (31), the brackets are the -deformed ones and are related to the Moyal product; for the other algebra the brackets are the usual Poisson brackets, which readwhere .

In this two scenarios the outcome can be summarized as follows: first, in the deformation quantization formalism, the -deformed algebra (31), when applied to a given system characterized by a canonical Hamiltonian , one gets a deformed Hamiltonian given rise to deformed equations of motion. Secondly, constructing a deformed phase space introducing the transformations (32a) and (32b), it is possible to formulate a Hamiltonian, formally analogous to a canonical one, but with the variables that obey the modified algebra (33). In this paper we will work under the lines of thought of the latter.

#### 4. Noncommutativity in Flat FLRW Loop Quantum Cosmology

##### 4.1. FLRW without LQC Corrections

We will start this section analysing the flat FLRW model for a free scalar field and without the LQC corrections. In Ashtekar variables and volume representation, the classical Hamiltonian takes the formIn view of the above discussion, we would like to consider effects of a deformed algebra (noncommutativity)with the remaining brackets zero. The above relations can be implemented by working with the shifted variableswhere and satisfy the relation .

The deformed Hamiltonian constraint arising from the steps above has the same functional form as (34) but is valued in the new noncommuting variables (as in [20]); that is,in the limit this Hamiltonian reduces to the usual one (34). The noncommutative equations of motion are and as expected, these Hamiltonian equations reduce to the usual ones when taking . Furthermore, the energy density is given byThe exact solutions to the system of ((38a)-(38d)) are where are integration constants. These solutions reduce to the usual ones (those obtain with (34)) when taking . We note that the solution for the volume function is the same as in the usual commutative case [47].

##### 4.2. FLRW with LQC Corrections

Now we want to implement noncommutativity in the flat FLRW model, by working in the shifted variables (36) defined atop. Since we are not actually performing a deformation of the symplectic structure, the loop quantization of the original variables can be carried as usual.

Considering the steps above and taking into account the ideas posed in the last section, we can therefore implement the effects of relation (36) at the effective scheme of LQC by considering the Hamiltonianwhere the noncommutative effective field equations result to be and again, in the limit we recover the commutative field equations. Due to the field equation for , we note that now the matter density is not given only by , but byIn order to construct the analog of the Friedmann equation we would need to obtain a relation for in terms of , but, due to the equation for being now more tangled, such relation can not be obtained. The relational evolution of in terms of is now given bywhen taking this relation reduces to (28).

We note that the equations for and are very similar to their commutative counterparts; the equation for is the only one being considerably more tangled, as pointed out above. The equation for is exactly the same, indicating that is a constant of motion.

We observe that for , furthermore, . So these values of correspond to a minimum in the volume function and to a change in sign in , indicating that a bounce takes place. The energy density at the bounce is , the same as in the commutative case; this means that the key features of LQC are maintained.

The equation for can be solved at once with the help of the Hamiltonian constraint (): is an integration constant. If the bounce takes place at (like in standard LQC) then we must have and takes the formand we can see the behavior of as a function of in Figure 1. This solution reduces to the commutative one [47] upon taking .