Research Article | Open Access

# Particle Production via Dirac Dipole Moments in the Magnetized and Nonmagnetized Exponentially Expanding Universe

**Academic Editor:**Kazuharu Bamba

#### Abstract

In the present paper, we solve the Dirac equation in the 2+1 dimensional exponentially expanding magnetized by uniform magnetic field and nonmagnetized universes, separately. Asymptotic behaviors of the solutions are determined. Using these results we discuss the current of a Dirac particle to discuss the polarization densities and the magnetization density in the context of Gordon decomposition method. In this work we also calculate the total polarization and magnetization, to investigate how the magnetic field affects the particle production. Furthermore, the electric and the magnetic dipole moments are calculated, and based on these, we have discussed the effects of the dipole moments on the charge distribution of the universe and its conductivity for both the early and the future time epoch in the presence/absence of a constant magnetic field and exponentially expanding spacetime.

#### 1. Introduction

One of the most interesting and important results of the formulation of the relativistic quantum mechanics in curved spacetime is the particle creation event in the expanding universe which was firstly discussed by Parker for the scalar particles and Dirac particles [1–3]. So, he computed the number density of the created particles by means of the Bogolibov transformation by using the out vacuum states constructed from the solutions of the relativistic particles wave equations. After these important works of Parker, the solutions of the relativistic particle wave equations have extensively been studied in various 3+1 dimensional spacetime backgrounds [4–19]. Using the WKB approach, the number density and renormalized energy-momentum tensor of the created spin-1/2 particle in the spatially flat (3+1)-dimensional Friedmann-Robertson-Walker (FRW) spacetime have been calculated [20]. The effect of the scalar particle creation on the collapse of a spherically symmetric massive star was investigated and it was demonstrated that the collapsing process was not independent from the particle creation rate [21]. Moreover, in [22] thermodynamics laws and equilibrium conditions are discussed in the presence of particle creation in the context of the (3+1)-dimensional Chern-Simons gravity theory. Recently, creation of the massless fermion in the Bianchi type-I spacetime investigated and showed that the massless particles can be created during the early anisotropic expansion epoch [23].

The Gordon decomposition of the Dirac currents is another useful tool for discussing the particle creation phenomena [4, 9, 10, 24]. In the decomposition method, the Dirac currents constructed from the solutions of the Dirac equations are separated into three parts, the convective, polarization with three components, and magnetization with three components, in the 3+1 dimensional spacetime. This method includes some complexities stemming from the 3+1 dimensional spacetime. Using this method in a 2+1 dimensional curved spacetime, the densities of the particle currents are separated into three parts, as in the 3+1 dimensional spacetime, but polarization density has two components and the magnetization density has only one component [24], and, moreover, as the Dirac spinor can be defined by only two components, the computations in the 2+1 dimensional spacetime become more simple than that of 3+1 dimensional spacetime. Because of the simplicity stemming from the dimensions, the dipole moments that are computed from the polarization and magnetization densities of the Dirac electron under influence in a constant magnetic field are easily computed and their result are, furthermore, compatible with the current experimental results [25]. With these motivations, in this study, we solve the Dirac equation in the 2+1 dimensional exponentially expanding magnetized by uniform magnetic field and nonmagnetized universes, separately, and discuss the particle creation event by means of the Dirac currents written in terms of these solutions. As a result, we observe that the polarization and magnetization parts of the currents are affected differently whether the exponentially expanding universe is magnetized or not and find expressions for the electric and magnetic dipole moments by integrating the polarization and magnetization densities on hypersurface.

The outline of the work is as follows; in Section 2, we, at first, discuss the Dirac equation solutions in the 2+1 dimensional exponentially expanding universe. In Section 3, the Dirac equation is solved in the 2+1 dimensional exponentially expanding universe with a constant magnetic field. In Section 4, we derive the components of Dirac currents for the solutions obtained in Sections 2 and 3 and also compute the polarization density, the magnetization density, total polarization (electric dipole moment), and the total magnetization (magnetic dipole moment). Finally, the last section, conclusion, includes a discussion about the results of this work.

#### 2. Dirac Particle in the 2+1 Dimensional Exponentially Expanding Universe

The behavior of the electron in 2+1 dimensional curved space is represented by the covariant form of the Dirac equation [24], which is important application in curved spacetime [26–33]where = is the Dirac spinorial wave function with two components that are positive and negative energy eigenstates, is the mass of Dirac particle, is the charge of the Dirac particle, and are 3-vectors of electromagnetic potential. Using triads, , Dirac matrices that dependent on spacetime, , are written in terms of the constant Dirac matrices, ;So, we choose the constant Dirac matrices, , in the flat spacetime as follows:withwhere , , and are Pauli matrices. The spin connection, , for the diagonal metrics is defined aswhere is the Christoffel symbol given as follows [34]:Also, the metric tensor is written in terms of triads as follows:where and are curved spacetime indices run from to , and are flat spacetime indices run to , and is the signature with (1,-1,-1).

The (2+1) dimensional de Sitter spacetime metric can be written as [35]where is Hubble parameter. From (3)-(8), the spin connections for the metric readUsing (2), (8), and (9), then the Dirac equation in the 2+1 dimensional exponentially expanding universe becomesLetting (4) and (10) and the Dirac spinor, =, we write the Dirac equation in explicit form as follows:To find the solutions of (11), thanks to the separation of variables method, the wave function components can be defined asBy these definitions, the Dirac equation is separated into the following two differential equation systems:andwhere is a separation constant, and we find the solutions of (13) in terms of the Bessel and confluent hypergeometric functions as follows:On the other hand, to solve (14), we must define a new variable such as . With the definition , the solutions of (14) are obtained in terms of Bessel functions or confluent hypergeometric functions:Then, the wave function, , can be written aswhere is normalization constant. To find the normalization constant, we use the Dirac-delta normalization condition [4, 36, 37]:where is determinant of the metric tensor and and for the surface [25]. Thus, the normalization constant is computed aswhere we use the following relation [4, 36, 37]:

#### 3. Dirac Particle in the 2+1 Dimensional Exponentially Expanding Magnetized Universe

It is interesting in discussing if the universe is under influence in an external constant magnetic field in the beginning time. Therefore, an electromagnetic potential can be chosen as and for a constant magnetic field in 2+1 dimensional spacetime. Then, the Dirac equation in the 2+1 dimensional exponential expanding universe with a constant magnetic field becomes and, thus, the explicit form of the equation is written asTo solve (22), we use the same procedure as the section before. The solutions of the equations arewhere , , , and is normalization constant. As all the contributions for particle creation and dipole moments are taking place from the boundaries, we can write the wave function in the following asymptotic form [36]:Then, the normalization constant can be obtained from (18) as follows: where we use and .

#### 4. Dirac Currents

The 2+1 dimensional Dirac current is written aswhere is Hermitian conjugate of the Dirac spinor and equal to [24]. As shown in [24], (26) is expressed in explicit form as follows:The components of the Dirac current in the 2+1 dimensional exponential expanding universe, and , areandwhere , , , and is Dirac-delta function. Also these components can be rewritten in terms of the convective, the polarization, and magnetization parts as follows:andwhere are polarization densities and is magnetization density, and their explicit forms are given byandrespectively. From these relations, the total polarizations, , and magnetization, , are defined asandwhere is an hypersurface for constant and [25].

Now, we are going to discuss the Dirac currents and the dipole moments expressions for the exponentially expending universe. So, inserting (17) and its conjugate into (26), we compute the components of the Dirac currents in asymptotic region as follows:Similarly, substituting (17) and its conjugate in (32) and (33), the components of the polarization densities and the magnetization density are written as follows:respectively, where we use the following abbreviations:Giving to the polarization densities and magnetization density depending spacetime coordinates, we can say that particle production event takes place. To calculate the total polarizations and magnetization, we insert (37), the polarization densities, and magnetization density, into (34) and (35), respectively, and later integrate them on the hypersurface. Then, we obtain the total polarization densities (electric dipole moments) and magnetization density (magnetic dipole moment) as follows: where we use the integral representation of Bessel function [36] and and are total polarizations, i.e., electric dipole moment components, and also is total magnetization, i.e., magnetic dipole moment. From these results, we see that the particle creation events are affected from only total polarization density, electric dipole moment. On the other hand, in the limit , vanishes by the following way: that is, there is not particle production in this limit or the universe has a symmetric charge distribution in the beginning time and, of course, the universe has not any dipole moments, but, in the limit , becomeswhere is Planck constant, is the speed of light, and , and, thus, the universe has a permanent complex dipole moment, which it oscillates with Zitterbewegung frequency,

To calculate the Dirac current components for the Dirac particle in the 2+1 dimensional exponentially expanding magnetized universe, we insert (24) and its conjugate in (26). Thus, we find that the current components areUsing (24) in (32) and in (33), the components of polarization and magnetization can be found as follows:To calculate the total polarizations and total magnetization, we insert (43) into (34) and (35). Then, using the integral representation of Bessel function [36], we find the following dipole moments expressions: From these expressions, we see that, in finite time intervals, the particle creation is influenced by both polarization and magnetization components. On the other hand, in the limit the magnetic dipole moment, , goes to zero faster than the electric dipole moment components, and . Therefore, the electric dipole moments in the particle creation events become more dominant than the magnetic dipole moment in finite time intervals if there exists in an external constant magnetic field.

#### 5. Summary and Conclusion

We exactly solve the Dirac equation in existence of the exponentially expanding magnetized and nonmagnetized universe and, from these solutions, derive some expressions for the Dirac current components and dipole moments. The particle creation in the exponentially expanding universe is only affected by the polarization in the finite time interval. However, this component goes to zero in the limit , i.e., in the beginning of the universe, but, in the limit , the universe has a permanent complex dipole moment oscillating with Zitterbewegung frequency, : . The complexity of the dipole moment points out the conductivity of the exponentially expanding universe. Also, the universe has the electric and magnetic dipole moments which are dependent on time in existence of an external constant magnetic field with the expansion such that, in the limit , the dipole moment expressions become infinite, but, in the limit , they go to zero. The dependence on time of the polarization and magnetization shows that the particle creation happens. Furthermore, in the limit , the particle creation events are affected only via the polarization because the magnetization, , goes to zero faster than and . From the point of view, we point out that the exponential expansion of the universe causes a particle creation, a permanent complex electric dipole moment and asymmetric charge distribution, but, in existence of an external constant magnetic field with exponential expansion in time, the universe charge distribution is get and getting symmetric and thus all the dipole moments become zero as .

#### Data Availability

No data were used to support this study.

#### Conflicts of Interest

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

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#### Copyright

Copyright © 2019 Semra Gurtas Dogan 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}.