Advances in High Energy Physics

Volume 2019, Article ID 3187289, 10 pages

https://doi.org/10.1155/2019/3187289

## Vortices in a Generalized Maxwell-Higgs Model with Visible and Hidden Sectors

^{1}Departamento de Física, Universidade Federal da Paraíba, 58051-970 João Pessoa, PB, Brazil^{2}Departamento de Ciências Exatas, Universidade Federal da Paraíba, 58297-000 Rio Tinto, PB, Brazil

Correspondence should be addressed to D. Bazeia; moc.liamg@aiezabd

Received 19 February 2019; Accepted 14 April 2019; Published 5 May 2019

Academic Editor: Rong-Gen Cai

Copyright © 2019 D. Bazeia 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 investigate the presence of vortices in generalized Maxwell-Higgs models with a hidden sector. The model engenders symmetry, in a manner that the sectors are coupled via the visible magnetic permeability depending only on the hidden scalar field. We develop a first-order framework in which the hidden sector decouples from the visible one. We illustrate the results with two specific examples that give rise to the presence of vortices with internal structure.

#### 1. Introduction

Topological structures appear in high energy physics in a variety of dimensions [1–3]. Among the mostly known ones, there are kinks, vortices, and monopoles, which are static configurations that appear in , , and spacetime dimensions, respectively. These structures have been investigated for more than 40 years, and they find a myriad of applications in high energy and condensed matter physics [1–4].

Vortices, in particular, were firstly investigated by Helmholtz in [5] and are commonly found in fluid mechanics [6]. They also appear in condenser matter, in the study of type II superconductors under specific conditions [7] when one deals with the Ginzburg-Landau theory of superconductivity [8]. As it is known, the Ginzburg-Landau theory is nonrelativistic and the first relativistic model that supports vortex configurations was introduced by Nielsen and Olesen in [9]; see also [10, 11]. It consists of a Higgs field coupled to a gauge field with the Maxwell dynamics under a local symmetry. These vortices are electrically neutral but have quantized magnetic flux.

They were largely investigated in several different contexts, including the case of generalized models; see [12–30]. In [12, 13], for instance, the presence of a generalized magnetic permeability in a model of the Maxwell-Higgs type allowed simulating properties of Chern-Simons vortices [31]. By using a similar model in [28], we have found the presence of compact vortices, which seems to map the magnetic field of an infinitely long solenoid. Due to the aforementioned works with generalized kinematics, we have introduced a first-order formalism to describe vortices in generalized models in [29] and a procedure to find analytic solutions in [30].

More recently, in [32], we have enlarged the symmetry to accommodate a symmetry, with the addition of a single neutral scalar field that interacts with the gauge field via the magnetic permeability. In this case, it was shown that the neutral field acts as a source to generate the vortex. In the past, a similar idea was developed, but with an symmetry engendered by two gauge fields and two complex scalar fields interacting through an extension of the standard Higgs-like potential [33]. This model is of interest in the study of superconducting strings and has been used in several contexts, in particular in [34–36] and in references therein. For instance, in [35] the authors describe the presence of novel solutions for non-Abelian cosmic strings and in [36] the study focuses on the critical behavior of magnetic field in a superconductor coupled to a superfluid, intending to simulate the core of neutrons stars, where superconducting protons are supposed to couple with superfluid neutrons. Among other possibilities, the symmetry may be enlarged to accommodate other fields. In particular, in [37–39] the symmetry is enlarged to become , in which the symmetry is governed by the addition of some neutral scalar fields. Furthermore, in the recent work [40] we considered the symmetry , extending the study of monopoles in the non-Abelian model considered [41, 42] to include a new neutral scalar field to produce magnetic monopoles with internal structure in the three-dimensional space.

Models with the symmetry are useful to include the so-called hidden sector, which seems to be of current interest [43, 44] and may play a role in the study of dark matter [45–48]. This hidden (or dark) sector may be coupled to the visible one via the Higgs fields, as it appears in the Higgs portal [49, 50], in a way similar to the coupling that appeared before in [33–35]. Another possibility is to add the interaction of the gauge field strengths as in [51–55], with the two strength tensors coupled to each other. We can also enlarge the symmetry and consider , as in [35], for instance, and also , as investigated very recently in [56], to search for color-magnetic structures in dense quark matter, compatible with the interior of compact stars and able to produce detectable gravitational waves. In this work, however, we follow a different direction and consider the symmetry, choosing the magnetic permeability of the visible sector to be driven by the scalar field of the hidden sector, without the coupling between the electromagnetic strength tensors. This is a novel possibility, which leads to results of current interest.

There are other interesting issues that suggest the study of topological structures in models described by the symmetry, as in [54, 55] and in references therein. In this work, however, we deal with a relativistic model in spacetime dimension and, inspired by [9–11], we consider a model in which the first portion describes the visible sector and the second accounts for the hidden sector. The system engenders two complex scalars of the Higgs type, the visible , and the hidden fields, with the coupling between the two sectors coming from a nonnegative function that is controlled by the hidden scalar field. As we show below, the function describes the magnetic permeability of the visible sector, and the main motivation for this is the fact that the dark matter seems to be always permeating the medium where the visible or baryonic matter appears to form galaxies in the Universe. Although we are dealing with a three-dimensional toy model, we believe that it is worth exploring this kind of coupling, since we still have no important insight on how the visible matter interacts with the dark component. Also, we will be searching for static vortexlike configurations at the classical level, intending to see how the topological structure of the hidden sector may modify the profile of the corresponding visible counterpart.

Dark matter is one among several problems that cannot be solved inside the Standard Model of particle physics, so the enhancement of the symmetry to the case is welcome to the study involving the visible and hidden sectors; see, e.g., the recent works [57, 58] and references therein, on several open problems in physics, in particular on dark matter. Moreover, since we are working at the classical level, the current study makes no progress on possible quantum features of the model. However, it can also be of interest to study pipelike vortices in two-component condensates [59] and also the interaction between vortices that can find applications in magnetic materials, for instance, if one changes the formulation in terms of the visible and hidden sectors to the case of hard and soft arrangements that appear in bimagnetic materials; see, e.g., [60, 61] and references therein. In this sense, the doubling of the symmetry to the case is of good use to investigate systems composed of two components condensates, not only in the case of visible and hidden sectors [51–54], but also in other contexts, such as the normal and superconductor components firstly studied in [33], the superconductor and superfluid coupling that is supposed to be present in the core of neutron stars [36], the study of pipelike vortex in two-component condensates [59], and the possibility of building two-component magnetic materials, with a hard magnetic component interacting with a soft magnetic component of the bimagnetic material [60, 61].

In order to introduce and investigate the model, we organize the paper as follows: in Section 2, we present the model and develop the Bogomol’nyi procedure [11], to find first-order differential equations which are very relevant to describe stable vortex configurations. For the proposed model, we also show that the first-order framework acts to decouple the hidden sector from the visible one. This is an interesting result, and we can then use the hidden sector as a source to describe the visible sector. In Section 3, we illustrate the results with two examples, which give rise to vortices with features of current interest. We end the work in Section 4, where we add conclusions and perspectives for future works.

#### 2. The General Model

We work in flat spacetime dimensions with the action , where the Lagrangian density is Here and are the visible complex scalar and gauge fields, and the corresponding hidden fields are and . As usual, is the visible electromagnetic strength tensor, and stands for the covariant derivative. Their equivalent hidden counterparts are and . The potential is denoted by and may present terms that couple both the visible and hidden scalar fields. In principle, the explicit form of the potential is unknown, and the generalized magnetic permeabilities are controlled by and , which are nonnegative functions that depend exclusively on the field . The above gauge invariant Lagrangian density engenders the symmetry. The inclusion of functions of the scalar field multiplying the Maxwell term is also present in models related to holography; see, e.g., [62, 63] for two distinct possibilities, used to describe an holographic insulator model with nonsingular zero temperature infrared geometry [62] and the electric charge transport in a strongly coupled quark-gluon plasma [63].

In our model, the visible and hidden sectors are coupled through , i.e., the hidden scalar field controls the magnetic permeability of the visible sector. This is a different approach from the one considered in [55], where the coupling was done with the electromagnetic strength tensors, through the term , which we are not considering in the current work. Here, we use the metric tensor and the natural units .

By varying the action with respect to the fields, we get that the equations of motion associated with the Lagrangian density (1) arewhere the currents are and . Also, we have used the notation , and so on. By setting in (2c) and (2d) and considering static field configurations, one can show the Gauss’ laws are identities for and for . In this case, the solutions are electrically neutral since the electric charges vanish.

Invariance under spacetime translations , with constant, lead to the conserved energy-momentum tensorTo search for vortexlike solutions, we consider static configurations and the usual ansatzin which and are nonvanishing integer numbers that control the vorticity of the visible and hidden solutions, respectively. Although this is not the most general situation, the above cylindrically symmetric ansatz for the fields is largely used in the search for vortex solutions in planar systems; see, e.g., [9–11, 54, 55] and references therein. Also, when the visible and hidden sectors decouple, and the expressions in (4) lead us back to the standard situation. The functions , , , and obey the boundary conditionsHere, and are parameters that control the asymptotic behavior of the functions and . Considering (4), the visible and hidden magnetic fields are giving by, respectively,where the prime stands for the derivative with respect to . By using this, one can show the magnetic fluxes are quantizedThese results allow that we introduce two topological currents, one in the visible sector, defined by , and the other in the hidden sector, defined by ; they are conserved and describe conserved charges that are directly identified with the corresponding magnetic fluxes The above results inform us that the suggested solutions are topologically protected against decay into the elementary excitations of the system.

We use (4) to rewrite the equations of motion (2a), (2b), (2c), and (2d) in the formUsing (4), the nonvanishing components of energy-momentum tensor (3) becomeIn the above equations, we identify the energy density as and the stress tensor as . The equations of motion (9a), (9b), (9c), and (9d) present coupling between the functions and are of second order. In order to simplify the problem, it is of interest to find a first-order formalism for the model. This can be done by using (10a) to develop the Bogomol’nyi procedure [11]. After some algebraic manipulations, we can writeAs we stated before, the potential is in principle arbitrary. However, motivated by the Bogomol’nyi procedure [11], the choiceallows that one writes the energy in the formwhereAlthough the choice (12) is not necessary, it leads us to (13), which unveils the interesting possibility: the first four terms are all nonnegative, so we see that the energy is bounded to the value , if the solutions obey the first-order equationsfor and controlling the gauge and scalar fields in the visible sector, andfor and controlling the gauge and scalar in the hidden sector. Therefore, we have obtained four first-order equations to study the problem. One can show that they satisfy the equations of motion (9a), (9b), (9c), and (9d) with the potential (12). An interesting fact is that solutions of the first-order equations are endowed with minimum energy, so they are stable according to the classical result of Bogomol’nyi [11] and also, they are compatible with the stressless condition, , which assures stability of the solutions under rescaling; see [29, 64, 65]. Notice that the first-order equations (16a) and (16b) are decoupled from the ones for the visible sector in (15a) and (15b). Therefore, we firstly solve the hidden sector to see how it modifies the visible one by choosing .

Before doing that, however, we notice that the presence of the first-order equations (16a) and (16b) and (15a) and (15b) allows us to write the energy density (10a) in the form , whereindicate the contribution of the visible and hidden sectors, respectively. We also highlight the fact that, from (14), the energy of the visible and hidden sectors are independent and fixed, despite the presence of the functions and . For the visible sector, we have and for the hidden one, .

Another feature of the above procedure, which can be seen from the potential in (12) and the first-order equations (15a) and (15b) and (16a) and (16b), is the presence of spontaneous symmetry breaking (SSB) in both the visible and hidden sectors. The presence of SSB in the hidden sector is necessary to give rise to vortex in the sector, and the first term in (12) induces SSB in the visible sector and is mandatory to generate the first-order equations that attain stable minima energy configurations. In particular, for and , one gets to the case of two uncoupled and similar ( and ) Maxwell-Higgs models, each one with its own Nielsen-Olesen vortex configuration [8]. To keep the two sectors coupled one has to make nontrivial, and this we discuss in the next section. Moreover, one has to choose and carefully, because they have to lead to first-order equations (15a) and (15b) and (16a) and (16b) that support solutions compatible with the boundary conditions (5a) and (5b).

#### 3. Some Specific Models

Let us now illustrate our findings with two distinct examples. Before doing so, we can simplify the problem by rescaling the fields asand taking and This leads us to work with dimensionless quantities. We also consider and and understand the parameter and as the ratio of the respective constants and of the hidden and visible sectors.

##### 3.1. First Example

Considering the hidden sector to be controlled by , its first-order equations (16a) and (16b) take the form which admits vortexlike solutions of the Nielsen-Olesen type. Unfortunately, the analytical solutions and are currently unknown. Therefore, one has to use numerical methods to find them. Since their profiles are well known (see [9, 10]), we will not display them here.

We then go on and investigate how the hidden fields modify the visible sector. We take the choicewhere is a nonnegative, dimensionless parameter. Notice that controls how strongly the hidden scalar field modifies the magnetic permeability of the visible sector. The case leads to , which decouples the sectors. The above function makes the potential in (12) to be written as From (16a) and (16b), we get that the first-order equations for the visible sector areIt is straightforward to see that the case leads to Nielsen-Olesen solutions, which are very similar to the ones of the hidden sector, except for the constants and . The parameter plays an important role in the model. One can show that vanishes for . We then expect to see a region in which is approximately uniform. Since , this feature appears only for , which is the range that we will consider here.

In Figure 1, we plot the solutions of the above equations, the visible magnetic field (6) and the energy density (10a) for some values of and . As increases, the solutions, the magnetic field, and the energy density shrink. The solution , in particular, presents a region in which it is approximately uniform, as expected. This region is very wide for and tends to shrink and to become closer to the origin as we increase . Due to this behavior in the solution, the magnetic field presents a splitting. This also happens, in a more subtle manner, with the energy density. Therefore, the presence of the hidden sector generates an internal structure to the vortex engendered by the visible sector of the model. It is worth commenting that these features do not affect the magnetic flux and the energy of the vortex, which remain unchanged, given by (7) and (14).