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Phase space deformations in phantom cosmology

We discuss the physical consequences of making general phase space deformations on the minisuperspace of phantom cosmology. Based on the principle of physically equivalent descriptions in the deformed theory, we investigate for what values of the deformation parameters the arising descriptions are physically equivalent. We also construct and solve the quantum model and derive the semiclassical dynamics.


Introduction
One of the most intriguing aspects in physics, is the current acceleration of the Universe. Is it a consequence of modifications to general relativity (GR) or is it a new kind of matter that drives this acceleration?. Although having some theoretical problems, the best answer to this question is the cosmological constant Λ. An alternative candidate that has been successful for the description of dark energy is the scalar field [1,2,3,4,5,6]. In particular, scalar fields with a negative kinetic term have been considered in the literature. This type of fields are known as Phantom fields. They have some interesting properties that allows them to be considered as a strange but viable matter which could be relevant in the evolution of the Universe [7]. In particular, a phantom field provides an effective negative pressure and a repulsive effect on the matter content of the Universe which in the long term could be responsible for the current accelerated expansion [8,9,10,11,12]. Therefore it has been considered as the matter source of the late time accelerated expansion of the Universe [13,14,15].
When considering the spacetime structure of the Universe it is usually done in reference to GR. But when regarding the micro structure of spacetime we do not have a universally accepted quantum theory of gravity. Although there are several candidates, noncommutativity has been considered as an alternative to understand the small scale structure of the Universe and help in the construction of quantum theory of gravity. For this reason, noncommutative versions of gravity have been constructed [16,17,18,19]. Noncommutativity is usually believed to be present near Planck's scale and is consistent with a discrete nature of spacetime. Motivated by this idea, it is justified to consider an inherently noncommutative spacetime at the early ages of the universe. Directly using noncommutative gravity is quite difficult, this is a consequence of the highly nonlinear character of these theories [16,17,18,19]. Fortunately there is an alternative, in [20] the authors introduce the effects of noncommutativity using the Moyal product of functions on the Wheeler-DeWitt (WDW) equation. The effects of the noncommutative deformation at the classical level was studied by a WKB approximation of noncommutative quantum model [21] and also by modifying the Poisson algebra [22,23]. More general minisuperspace deformations have been done in connection with Λ [24,25,26,27,28,29]. Phase space deformations give rise to two physically nonequivalent descriptions, the "C-frame" based on the original variables but with a modified interaction and the "NC-frame" frame based on the deformed variables but with the original interaction. Given this ambiguity, in [29] a principle was proposed to restrict the value of the deformation parameters in order to make both descriptions physically equivalent.
In this work we consider a Friedmann-Robertson-Walker (FRW) cosmological model coupled to a phantom scalar field and study the physical consequences of introducing general phase space deformations on the minisuperspace of the theory. We will study both, the classical and quantum models and we also find that the semiclassical approximation of the deformed quantum model agrees with the classical model. The deformation parameter space is determined by considering the principle of physically equivalent frames [29].
The paper is organized as follows. In section 2, the commutative model is presented. In section 3, the minisuperspace phase space deformation is implemented and the dynamics in the two frames is obtained. Also the deformation parameters are constrained by imposing physical equivalence between the "C-frame" and the "NC-frame". The quantum analysis is done in section 4, we find the solution to the deformed WDW equation and fix the parameters in the deformation in order to make the quantization possible. We also show that the classical paths arise from the semiclassical approximation of the WDW equation obtained from the deformed Hamiltonian. Finally, section 5 is devoted for concluding remarks.

Phantom field model
We start with the flat FRW metric a(t) corresponds to the scale factor and N(t) is lapse function.
In this background the action of a minimally coupled phantom scalar field ϕ(t) with constant potential is where we have set the units so 8πG = 1. The minus sign in the kinetic term of the scalar action is the difference between the usual scalar field and the phantom scalar field [12]. The canonical Hamiltonian derived from Eq.
With the the following change of variables where ω 2 = − 3 4 Λ. When one considers the usual scalar field, the Hamiltonian is transformed to a "ghost oscillator" which is simply a difference of two harmonic oscillators [26,29].

Deformed Phase Space Model
There exist different approaches to incorporate noncommutativity into physical theories. Particularly, in cosmology there is a broadly explored path to study noncommutativity [20], where noncommutativity is realized in the so called minisuperspace variables. We will follow a deformed phase space approach. The deformation is introduced by the Moyal bracket { f, g} α = f α g − g α f . By substituting the usual product with the Moyal product ( f g)(x) = exp 1 2 The 2 × 2 antisymmetric matrices θ i j and β i j represent the noncommutativity in the coordinates and momenta respectively. The α deformed algebra becomes In this work we use the particular deformations, θ i j = −θ i j and There is an alternative to derive a similar algebra to Eq. (7). For this we follow the procedure given in [24,26]. Start with the transformation on the classical phase space variables {x, y, P x , P y }, these are the variables that satisfy the usual Poisson algebra. The new variables satisfy a deformed algebra where σ = θβ/4. Furthermore, as in [24,26], we assume that the deformed variables satisfy the same relations as their commutative counterparts. The resulting algebra is the same, but the Poisson bracket is different in the two algebras. In Eq. (7), the brackets are the α deformed ones related to the Moyal product, for the other algebra the brackets are the usual Poisson brackets.
To construct the deformed theory, we start with a Hamiltonian which is formally analogous to Eq.(5) but constructed with the variables that obey the modified algebra Eq.(9), this gives the deformed Hamiltonian where 2 and ω 2 are given by There is a significant difference between the transformed Hamiltonian of the scalar field cosmology model [26] and Eq. (10), the deformed Hamiltonian of the phantom cosmology model. Unlike the scalar field case, the crossed term involving position and momentum in the phantom model, corresponds to an angular momentum term. To understand the physics of the deformation, it is necessary to remember that the deformation Eq.(8) defines two physical nonequivalent descriptions, the "C-frame" where the effects of the deformation are interpreted as a commutative space (x, y) but with modification of the original interaction and the "NC-frame" where we work with the deformed variables ( x, y) and the original interaction. In general, the dynamics in the two frames is different but the physical interpretation in the "C-frame" is easier. In this frame we can interpret the deformed model as a bidimensional harmonic oscillator and the minisuperspace deformation comes into play as an angular momentum term in the Hamiltonian. For this reason we will do the calculations in the "C-frame".
We obtain the equations of motion from the Hamiltonian Eq. (10), which in the (x, y) variables are given bẏ and getẍ With the transformation z = x + iy we can easily solve Eq.(13).
We have three different solutions depending on the sign of ω 2 .
For ω 2 > 0, we get A 1 , B 1 are arbitrary constants that, from the Hamiltonian constraint, satisfy for this case the integrating constants satisfy the condition A 2 3 = B 2 3 . The last solution is for the case ω = 0, the constraint imposes B 2 = 0. The condition arises when the cosmological constant satisfies 2β = −3Λ.
In analyzing the evolution of the Universe, we will focus our attention on its volume and calculate a 3 (t) in the two frames. Let us start in the "C-frame", using the solutions for the model, Eq. (14), Eq.(15) and Eq. (16), together with the change of variables in Eq.(4) we get where V (i) 0 , V (i) 1 are constructed from the integrating constants. To study the dynamics in the "NC-frame" we use the "Cframe" solutions. The volume is constructed with the "NCframe" variables, a 3 (t) = m 2 ( x 2 + y 2 ) where It is important to mention that even if we have a positive volume in the "Cframe" we might need to impose some restriction in order to have a valid description in the "NC-frame". In order to determine the valid range of the deformation parameters we use the principle used in [29] which states the following, "Deformed phase space models are only valid when the NC-frame and Cframe descriptions are physically equivalent". To impose that the description in the two frames should be physically equivalent, we start by analyzing the expression for the "C-frame" volume. It is easy to show that the volume is always positive. In the first case one obtains that V (1) 0 + V (1) 1 = (A 1 + B 1 ) 2 ≥ 0 so is positive for any t. For the second case the volume is also positive, and finally for the third case the constant V (3) 1 > 0. Then we conclude that for the three cases, the "C-frame" volume is always positive for any choice of the integration constants. The constants in the "NC-frame" solutions are related to the "C-frame" constants as follows. For the first case, A 1 = (1 + | ω|θ/2)A 1 and B 1 = (1 − | ω|θ/2)B 1 , for the second case the volume is the same and for the last case the constant in the "NC-frame" is related by A 2 3 = (1 +ω 2 θ 2 /4)A 2 3 . We see from Eq. (17) and Eq.(18) that for θ = 0, the two frames are physically equivalent. We can conclude that θ = 0 and β 0 are valid values for the deformation parameters. Now we consider the general case θ 0 and β 0. It is clear that in the first two cases, that the volume has the same physical behavior in the two frames then there are no restriction for the deformation parameters. For the third case, we have the same behavior as long as we satisfy the condition 1 + θ 2 ω 2 4 > 0. Furthermore, the evolution is that of an exponential scale factor for an accelerating Universe. Then comparing with a de-Sitter Universe we find (only for the third case), an effective positive cosmological constant This effective cosmological constant is determined by the deformation parameters as well as the value of Λ. Since current observations point to a positive cosmological constant. This gives and extra condition that restricts the values of the deformation parameters by imposing that Λ e f f > 0. After fixing the value of Λ, we have three definite restrictions: ii) f (β, Λ) = 3Λ − β 2 and g(θ, Λ) = 1 − 3θ 2 Λ 16 must have the same sign.
iii) 1 + θ 2 ω 2 4 > 0. From ii), we can see in Fig.(1) and Fig.(2) the regions where these inequalities are satisfied. We did not consider Λ ≤ 0, since condition ii) would not be satisfied, for this reason the plots only show the region where Λ > 0.  We want to emphasize that for the phantom scalar field we cannot define an effective cosmological constant when Λ = 0, as it was done for the usual scalar field in [26]. When setting Λ = 0 we will have ω 2 > 0 meaning that we are in the first case and therefore we will not have an exponential behavior. For this model the deformation maps an initial positive cosmological constant model to another positive cosmological constant model, the two cosmological constants have different values but they are both positive. This fact also leads to a more restrictive space of parameters than the one analyzed in [29].

Noncommutative quantum model
Now we proceed with the quantization of the deformed Hamiltonian. The usual canonical quantization approach H nc ψ = 0, gives the corresponding WDW equation. The Hamiltonian H nc , explicitly contains the angular momentum operator (xP y − yP x ) = L z and can be written in terms of the Hamiltonian of a 2-dimensional harmonic oscillator H xy , with frequency ω 2 plus an angular momentum term, that is H nc = H xy + L z . Using the similarity of the WDW equation, with the 2-dimensional harmonic oscillator, we will follow the approach in [30,31]. First we write the eigenvalue equation for the harmonic oscillator, then we will find the energy eigenvalues and finally impose the zero energy condition. After writing the quantum equation in polar coordinates, we obtain the equation for the energy eigenstates, and is given by It is well known that the Hamiltonian of the 2d harmonic oscillator commutes with the angular momentum. This means that we have [H xy , L z ] = 0, allowing us to write the wave function with eigenstates common to both operators. This breaks the degeneracy in energy eigenstates and every state is uniquely specified by the quantum numbers n and m. Solving Eq.(20) we find the wave function of the Universe ψ n,m (r, φ) where n = 0, 1, 2, ... ; m = 0, ±1, ±2, ..., ±n, and L α n (z) are the generalized Laguerre polynomials. The zero energy condition E = 0 from the WDW equation is trivially satisfied by = ω = 0. For 0, ω 0 (for instance for a single state of quantum numbers n and m) we get the general equation By using the definitions for 2 and ω 2 > 0 we can write this equation as With respect to the condition in Eq. (23), we need to find the values of θ, β and Λ to satisfy the condition. The first thing to notice is that the right hand side of this equation . The quantum solution is possible when ω 2 > 0, which corresponds to the first solution in Eq. (17) and Eq. (18). Therefore, the space of parameters is already depicted in Fig.(1) and Fig.(2), corresponding to the condition that the functions f (β, Λ) and g(θ, Λ) have opposite sign. The valid values of parameters θ, β and Λ, corresponds to the gray region of Fig. 1 and white region of Fig. 2, or vice versa. We use the inverse transformation of Eq.(4) with Eq. (21) to find the wave function ψ n,m (a, ϕ) in terms of the scale factor a and the phantom field ϕ. We can construct a general wave packet ψ(a, ϕ) = N n c n,m ψ (n,m) (a, ϕ), with m fixed and c n,m arbitrary constants as long as the condition E = N n E (n,m) = 0 also holds. When this is the case, it is always possible to find values of θ, β and Λ to satisfy the constriction Eq. (22), under which these values are fixed unambiguously. For a given value of m, the sum in Eq.(25) runs over odd/even values of n depending on the odd/even value of m respectively. The wave packet is normalizable by the use of the orthogonality relation of generalized Laguerre polynomials. The total energy of the wave packet will satisfy the generalized zero energy condition Eq. (22), but replacing n by N. From the arguments given above, we conclude that it is always possible to find, for a given Λ > 0 values for θ and β for which the condition holds.

Classical paths from a WKB approximation
One can apply a WKB type approximation on the WDW equation H nc Ψ = 0, to see if we get the classical solutions. First we notice that the effective classical cosmological constant given in Eq. (19) is the same quantum cosmological constant in the Hamiltonian H nc . Remembering that in the commutative Hamiltonian 4ω 2 = −3Λ, for the deformed Hamiltonian 4 ω 2 = −3Λ E f f . This is the generalized deformed frequency and using the definition of ω 2 we get the same effective cosmological constant.
We now apply the standard procedure for the semiclassical approximation. We propose a wave function of the form which upon substitution in H nc Ψ = 0, in the limit → 0 and using the approximation we get the Einstein-Hamilton-Jacobi (EHJ) equation With the identification ∂S 1 (x) ∂x = P x , ∂S 2 (y) ∂y = P y , the EHJ equation takes the forṁ x 2 + y 2 = 0.
Now we take the time derivative of the EHJ equation and divide the result byẋẏ to geẗ we can separate the expression by equating the first two terms to − 2 and the last two to 2 . The two resulting equations are the equations of motion in Eq. (13). We can be confident that the same classical paths arise in the classical limit of the WDW equation obtained from the deformed Hamiltonian.

Conclusions
In this paper we have studied the effects of the minisuperspace phase space deformations in the dynamics of phantom scalar cosmology. The deformation was applied on the minisuperspace variables. From the deformed Hamiltonian we derived the equations of motion. It is known that from the deformation two generally nonequivalent descriptions arise. Using the solutions to Eq.(13), we calculate the volume of the Universe in the "C-frame" and in the "NC-frame". To constrain the deformation parameters β and θ, we impose that for phase space deformations to be valid, the physical description in the two frames must be equivalent. From the value of ω 2 three different cases appear. For ω 2 > 0, we get a bouncing Universe and the solutions in the two frames are equivalent. For the last case, when the Hamiltonian constraint is applied, we have a de Sitter Universe and the parameter ω 2 can be interpreted as an effective positive cosmological constant Λ E f f . The value of Λ E f f depends on the deformation parameters θ and β as well as the original Λ. If we set the original cosmological constant Λ = 0, then ω 2 > 0 and is not possible to have Λ E f f ≥ 0. This imposes a stronger restriction on the values of β and θ and the parameter space is even more restricted, but even when this is the case we have a region of values where the two descriptions are physically equivalent.
We quantized the model, obtaining the corresponding WDW equation and found the wave function of the Universe. We derived a relation that fixes the values of the parameters θ, β and Λ in order to satisfy the zero energy condition of the WDW equation. We showed that the deformed phantom cosmological model is physically viable. Also, when ω 2 > 0 the quantization can be achieved and the introduction of the deformation breaks the degeneracy of the quantum states. A general condition on the parameters θ and β arises from the zero energy condition that can be satisfied by the general wave packets. It is worth to mention that there is a nice physical interpretation in the "C-frame". It is related to the introduction to an effective perpendicular and constant "magnetic field" B. This can be seen by taking the bidimensional harmonic oscillator coupled to the vector potential A = ( B 2 y, − B 2 x) where the magnitude of the field will be B = 2 . Then we can see that the zero energy condition is related to the manipulation of this field and corresponds to a modification in the deformation parameters (θ, β). Finally, we performed the WKB approximation and show that the same classical solutions arise in the classical limit of the WDW equation of the corresponding deformed Hamiltonian.