Oscillons and oscillating kinks in the Abelian-Higgs model

Oscillons and oscillating kinks in the Abelian-Higgs model

V. Achilleos    F.K. Diakonos    D.J. Frantzeskakis    G.C. Katsimiga    X.N. Maintas    E. Manousakis    C.E. Tsagkarakis    A. Tsapalis Department of Physics, University of Athens, GR-15771 Athens, Greece Department of Physics, Florida State University, Tallahassee, Florida, USA Hellenic Naval Academy, Hatzikyriakou Avenue, Pireaus 185 39, Greece
July 12, 2019
Abstract

We study the classical dynamics of the Abelian Higgs model employing an asymptotic multiscale expansion method, which uses the ratio of the Higgs to the gauge field amplitudes as a small parameter. We derive an effective nonlinear Schrödinger equation for the gauge field, and a linear equation for the scalar field containing the gauge field as a nonlinear source. This equation is used to predict the existence of oscillons and oscillating kinks for certain regimes of the ratio of the Higgs to the gauge field masses. Results of direct numerical simulations are found to be in very good agreement with the analytical findings, and show that the oscillons are robust, while kinks are unstable. It is also demonstrated that oscillons emerge spontaneously as a result of the onset of the modulational instability of plane wave solutions of the model. Connections of the results with the phenomenology of superconductors is discussed.

pacs:
11.15.Kc, 11.10.Lm, 05.45.Yv

I Introduction

The concepts and tools of classical field theory are useful for a large class of physical systems ranging from the electromagnetic field to Bose-Einstein condensates (BECs). For instance, in the context of the Landau-Ginzburg (LG) theory of phase transitions, the free-energy density as a functional of the order parameter (the expectation value of the quantum field operator for a BEC) maps to the same form as the energy density functional of a classical field.

Classical solutions minimizing the energy density functional of such models play an important role also in quantum field theory, as well as in high energy physics, and cosmology. Real time soliton solutions give rise to particle-like structures, such as magnetic monopoles, and extended structures, such as domain walls and cosmic strings, that have implications for the cosmology of the early universe earlyuniverse (); amin (); stama068 (); khlopov () . With respect to their dynamical characteristics, the classical field solutions can be both static or travelling solitons rajaraman (), as well as oscillons (alias breathers). Oscillons, are long-lived configurations localized in space and periodic in time. Such localized structures can be found in many physical systems, ranging from granular media granular () to water waves water (). Additionally, oscillons have also been extensively studied in the context of field theory, and can be found both in scalar sinegordon (); bogo (); campbell (); gleiser94 (); honda (); salmi06 (); salmi08 (); fodor06 (); fodor08 (); gleiser08 (); segur (); amin2 (), and Abelian or non Abelian gauge theories gleiser2 (); farhi05 (); graham (); sfakia (). Atomic Bose-Einstein condensates bec () offer a setting where a large variety of classical field solutions (relevant to elementary gauge fields spiel1 () or even to cosmological black holes bholes ()), can be studied both theoretically and experimentally emergent (). Thus, the search for classical field solutions and their phenomenological impact, nowadays appears to gain an increased attention.

A prototype system of such a classical field emerges when one restricts himself to a mean-field treatment of the Gor’kov - Eliashberg - Landau - Ginzburg approach of superconductivity Gorkov (); GorkElia (); GinzbLand (); Abrikosov (). In this case, the order parameter is the expectation value of an electron-pair creation operators which, for the simple case of s-wave pairing, behaves as a complex field . The emerging effective field theory is an Abelian-Higgs model, where the Higgs field is the pair condensate order parameter, and the Abelian field is the electromagnetic field. This explains in a rather straightforward manner the Meissner effect (the fact that the magnetic field only penetrates the superconductor within a finite penetration depth) through the now called Higgs mechanism, namely: the appearance of the condensate spontaneously breaks the symmetry, giving rise to a finite mass to the gauge field. The existence of this gap (or mass) also ensures the phenomenon of perfect conductivity, through the collective dynamics of the condensed Cooper pair electrons. There is a considerable amount of works in the literature related to the search of classical solutions in this model (Abelian-Higgs), mainly in the context of localized and/or topologically charged forms. The existence of such solutions depends strongly on the space dimensionality. In two spatial dimensions, Abelian-Higgs models have vortex solutions (e.g., the Nielsen - Olesen vortex nielsen ()), which carry a non-vanishing topological charge, and play an important role in many aspects of contemporary physics (for example the Abrikosov vortices in Landau-Ginzburg theory of superconductivity gl ()). When time-dependence is taken into account, oscillon solutions can be found both in mclerran () and gleiser2 () dimensions. Recently, it was shown that oscillons can emerge dynamically from vortex-antivortex annihilation gleiser2 (), highlighting the fact that oscillon dynamics are intriguing, and may play a crucial role in many areas of physics featuring symmetry breaking, ranging from superfluids and superconductors to cosmology.

In the present work, we analyze the classical dynamics of the Abelian-Higgs model in -dimensions by means of a multiscale expansion method multiplescales (). We restrict our analysis on the case of small fluctuations of the condensate about its vacuum expectation value (vev). This is realized by choosing the amplitude of the Higgs field to be an order of magnitude smaller than that of the gauge field. Employing the method of multiple scales (see also Ref. emeis ()), the original nonlinear coupled field equations are reduced to an effective nonlinear Schrödinger (NLS) equation for the gauge field, and a linear equation for the Higgs field containing the gauge field as a source. These equations are analytically solved giving two types of localized solutions for the gauge field, namely in the form of oscillons and oscillating kinks. Subsequently, we numerically integrate the original equations of motion using, as initial conditions, the analytically found solutions. We find that the analytical predictions are in excellent agreement with the numerical findings for a large range of values of the parameters involved. We then discuss connections between the Abelian-Higgs model solutions and the phenomenology of superconducting materials, describing the temporal fluctuations of the condensate in a one-dimensional (1D) Josephson junction paterno () due to the presence of oscillating (in time) magnetic and electric fields.

The paper is organized as follows: in section II, we introduce the general formalism of the Abelian-Higgs model and we derive the equations of motion for the gauge and the scalar fields. We then use the method of multiple scales to reduce the equations of motion to the NLS system, and present the corresponding analytical solutions. In section III we present results of direct numerical integration of the original equations of motion to check the validity of our approximations and study the stability of our solutions. Finally, in section IV, we present our concluding remarks and make connections with the context of superconductors.

Ii The model and its analytical consideration

ii.1 Formulation and Equations of Motion

The -Higgs field dynamics is described by the Lagrangian:

(1)

where is the field strength tensor, is the covariant derivative ( is the coupling constant), and () is the Higgs self-interaction potential (asterisk denotes complex conjugate). In the broken phase, , the scalar field acquires a non vanishing vacuum expectation value (vev) and can be parametrized as: , where the real functions and denote the Higgs field and the Goldstone mode, respectively, and is the corresponding vev. Since the Lagrangian of Eq. (1) is invariant under the local gauge transformations

(2)
(3)

where is an arbitrary phase, by choosing the unitary gauge , we can gauge away the Goldstone mode . This gauge choice has the advantage of mapping the field to a real scalar field, namely the Higgs field. In this case, the fluctuations around the vev lead to the following system of equations of motion for and :

(4)

where and . We simplify Eqs. (4)-(LABEL:eq:eq3) choosing the field representation , and . Due to the fact that we are interested in 1D settings, the non vanishing field depends solely on and . As a consequence, the Lorentz condition is fulfilled automatically, leading to a coupled system of equations for the gauge field and the Higgs field . Furthermore, we express Eqs. (4)-(LABEL:eq:eq3) in a dimensionless form by rescaling space-time coordinates and fields as: , , , . This way, we end up with the following equations of motion:

(6)
(7)

where parameter is assumed to be of order . The Hamiltonian corresponding to the above equations of motion is:

(8)

where indices denote partial derivatives with respect to and , and the potential is given by:

Notice that exhibits a single minimum at .

Here we should note that the above choice of field representation, and the concomitant simplification of the full system into Eqs. (6)-(7), are valid in the case of the unitary gauge. In a different gauge, the simplification would still be approximately valid, as long as the Goldstone fluctuations , are sufficiently smaller than the Higgs field or slowly-varying with respect to the spatial variables. However, if the Goldstone fluctuations become significant, Eqs. (6)-(7) should be modified to incorporate a phase field as well as more gauge field components. In such a case, it is clear that a solution of Eqs. (6)-(7) (such as the ones that we will present below) will not satisfy the full system. However, using continuation arguments, one can argue that for a sufficiently small phase field and for additional gauge field components solutions of Eqs. (6)-(7) will still persist. Further increase of the additional components may lead to bifurcations of these solutions and the emergence of other structures. This problem is important and interesting in its own right, but its consideration is beyond the scope of this work.

Thus, below we will focus on the simplified system (6)-(7) and employ an asymptotic multi-scale expansion method to derive approximate localized solutions, in the form of oscillons and oscillating kinks.

ii.2 Multiscale expansion and the NLS equation

Considering a small fluctuating field , we may employ a perturbation scheme, which uses a formal small parameter defined by the ratio of the amplitude of the Higgs field to the amplitude of the gauge field, i.e., . In particular, we will employ a multiscale expansion method multiplescales (), assuming that the Higgs and gauge fields depend on the set of independent variables , , and , , . Accordingly, the partial derivative operators are given (via the chain rule) by , . Furthermore, taking into regard that the fields should be expanded around the trivial solution of Eqs. (6)-(7), as well as as per our assumption, we introduce the following asymptotic expansions for and :

(10)
(11)

where and () denote the fields at the order . Substituting Eqs. (10)-(11) into Eqs. (6)-(7), and using the variables , , , , we obtain the following system of equations up to the third-order in the small parameter epsilon :

(12)
(15)

The solution of Eq. (12) at the first order is:

(16)

where is an unknown function, “c.c.” stands for complex conjugate, while , and the frequency and wavenumber are connected through the dispersion relation . The solvability condition for the second-order equation (15), is (the second term is “secular”, i.e., is in resonance with the first term which becomes , thus leading to blow-up of the solution for ). The above condition is satisfied in the frame moving with the group velocity , where , so that depends only on the variable and . Then, the field is taken to be of the same functional form as [cf. Eq. (16)]. Taking into regard the above results, Eq. (15) for the Higgs field yields:

(17)

where and ; here, it is assumed that and , as for these limiting values the field (which is assumed to be of as per the perturbation expansion) becomes infinitely large. Finally, at the order , we first note that the second term vanishes automatically in the frame moving with . Thus, the solvability condition (obtained —as before— by requiring that the secular part vanishes) is: . Below, for simplicity, we will consider the zero momentum case (); hence, , and also , i.e., the field is at rest. In this case, we derive the following NLS equation for the unknown function :

(18)

where the parameter is given by

(19)

The above NLS equation possesses exact localized solutions of two different types, depending on the sign of : for , the solutions are sech-shaped solitons, while for the solutions are tanh-shaped kinks. These solutions have been extensively studied in a variety of physical contexts including nonlinear optics yuri (), water waves johnson (), atomic Bose-Einstein condensates emergent (), and so on. Here, the type of solution, i.e., the sign of the nonlinear term in Eq. (18), depends solely on the parameter .

In particular, for and , we obtain [attractive (focusing) nonlinearity] and the soliton solution of Eq. (18) has the following form:

(20)

where is a free parameter [considered to be of order ] characterizing the amplitude of the soliton, while the soliton frequency is . Accordingly, the approximate solutions of Eqs. (6)-(7) for and can be expressed in terms of the original variables and as follows:

(21)
(22)

and are characterized by a single free parameter, . The above approximate solutions for the gauge field and the Higgs field are localized in space (decaying for ) and are oscillating in time; thus, they correspond to oscillons (alias breathers). At the leading-order in , the oscillation frequencies for and are respectively given by: and (in units of ) respectively.

On the other hand, for , we obtain [repulsive (defocusing) nonlinearity], and Eq. (18) possesses a kink solution of the following form:

(23)

where is a free parameter and . In this case, the approximate solutions for the gauge and Higgs fields read:

(24)
(25)

These solutions correspond to oscillating kinks, for both fields, which are zero exactly at the core of the kink and acquire non vanishing values at . Again the fields oscillate with the frequencies and respectively.

Iii Numerical results

To further elaborate on our analytical findings, in this Section we will present results stemming from direct numerical integration of Eqs. (6)-(7). Our aim is to check the validity of our analytical predictions, namely the existence of oscillons and oscillating kinks, as well as study numerically their stability. The equations of motion are integrated by using a fourth-order Runge-Kutta time integrator and a pseudo-spectral method for the space derivatives jianke (). The lattice spacing used was fixed to , the time step , and the total length of the lattice . In all simulations we used, as an initial condition, the approximate solutions of Eqs. (21)-(22) for the oscillons and of Eqs. (24)-(25) for the oscillating kinks for ; in all cases we have fixed the free parameter value to , and the ratio of the two fields amplitudes to .

iii.1 Oscillons

Figure 1: (Color online) Top panel: Evolution of the gauge field as a function of and . Bottom panel: Profile snapshots of the field at different instants of its breathing motion. Parameter values used are , and the oscillation period is .
Figure 2: (Color online) Same as in Fig. 1, but for the Higgs field . Notice that the oscilation period of the Higgs field is .

In the top panels of Fig. 1 and Fig. 2 a contour plot showing the evolution of an oscillon solution is shown (for ) at the end of the integration time . Note that the periods of the two fields are and , and thus oscillations for the gauge field and oscillations for the field are depicted. In the bottom panels of Figs. 1 and 2, we show the profiles of and respectively, during the interval of one period, exhibiting their breathing motion. While the gauge field performs symmetric oscillations, the Higgs field oscillates asymmetrically with respect to its amplitude. This is due to the constant in the solution of Eq. (22). The evolution of an oscillon for (lying in the second region where oscillons exist) is also shown in the top panels of Fig. 3 and Fig. 4, where due to the form of the solutions the breathers become more localized in this region, as can be seen from their snapshots (bottom panels of Figs. 3-4).

In order to also highlight the localization of the energy of the oscillons, in the top and middle panels of Fig. 5, we show a contour of the total Hamiltonian density [cf. Eq. (8)] for . The top panel, corresponds to an initial condition using only Eqs. (21)-(22), while in the middle panel we have also added a random Gaussian noise to the initial condition, as large as of the oscillon’s amplitude (the rest of the parameters are as in Fig. 1). We observe that the energy density remains localized during the numerical integration in both cases (with and without noise). We would like to stress here that, the latter result, shows that oscillons are robust under the effect of a random noise, and this was also confirmed for different values of in the domain of existence of the oscillon. For completeness, the total energy , normalized to its initial value , is also shown in the bottom panel of Fig. 5; here, the dashed dotted line corresponds to both and . In fact the energy fluctuations, defined as , as shown in Fig. 5 [for (top solid line) and (bottom dashed line)] are of the order of .

Figure 3: (Color online) Same as Fig. 1, for parameter values and .
Figure 4: (Color online) Same as Fig. 2, with parameter values , .
Figure 5: (Color online) Top and middle panel: contour plot showing the energy density , as a function of time, for . For the middle panel the initial condition was perturbed by a small random noise with an amplitude of the oscillon’s amplitude. Bottom panel: the total energy normalized to its initial value at , where the dashed dotted [upper (black)] line corresponds to and respectively. The energy difference , for solid [middle (blue)] line and dashed [bottom (red)] line.

iii.2 Spontaneous oscillon formation

In this section we show that oscillons can emerge spontaneously, through the mechanism of modulation instability (for more details see Ref. mi ()). The latter concerns the instability of plane wave solutions of the NLS Eq. (18), of the form

(26)

under small perturbations. To briefly describe the emergence of this instability, we consider the following ansatz:

(27)

where the amplitude and phase perturbations and are given by:

(28)
(29)

with and being constants, and being a formal small parameter. Substituting Eqs. (27)-(29) into Eq. (18) it is found that, for , the frequency and the wavenumber of the perturbations, obey the dispersion relation:

(30)

It is evident from Eq. (30) that for there exists an instability band for wavenumbers , where becomes complex. Note that this instability can only emerge in the region where oscillons exist. When this instability manifests itself, the exponential growth of the perturbations leads to the generation of localized excitations, which are identified as the oscillons described in Eqs. (21)-(22).

To illustrate the above, we have numerically integrated Eqs. (6)-(7), with an initial condition corresponding to the plane wave of Eq. (26), perturbed as in Eq. (27), with , , (inside the instability band), and ; the rest of the parameters used are , , and . In the top panel of Fig. 6, we show a contour plot of the energy density, . It is observed that, at , localization of energy is observed due to the onset of the modulation instability. This localization is due to the fact that harmonics of the unstable wavenumber of the perturbation are generated, which deform the plane wave and lead to the formation of localized entities. In fact, the latter are eventually reformed into oscillons, as is clearly observed in the bottom panel of Fig. 6: there, we show the profile of the gauge field [solid (black) line] at , and we identify at least two well formed oscillons located at and . The latter are found to be in a very good agreement with the respective analytical profile depicted by the dashed (red and blue) lines. To perform the fitting, we plotted the approximate solutions of Eq. (21), using the value at the peak of the oscillons, in order to identify the oscillon amplitude . Then, the solution was also displaced by a constant factor, in order to match the center of the oscillon. Additionally, time was set to zero () and the fitting was made at the beginning of the period of oscillation for the particular oscillons. The very good agreement between the analytical and numerical field profiles highlights the fact that the oscillons considered in this section can be generated spontaneously via the modulational instability mechanism.

Figure 6: (Color online) Top panel: Contour plot showing the energy functional , for , , , for an initial condition corresponding to an unstable plane wave. Bottom panel: Profile of the gauge field , (solid [black] line), at after the instability has set in. Dashed (blue and red) lines, correspond to the the solutions of Eq. (21), fitted with the parameter at the peak of the oscillons (indicated by the dotted [grey] lines at and ).

iii.3 Oscillating kinks

We now proceed with the numerical study of solutions corresponding to the kinks of the NLS Eq. (18). Such solutions in the form of Eqs. (24)-(25) are expected to exist in the parameter region . Performing the same procedure as in the previous section, we numerically integrate the equations of motion and study the relevant dynamics. In the top panels of Figs. 7 and 8, the contour plot of a kink solution is plotted, showing the evolution of both fields and , during the interval of three and six periods, respectively (for ). In addition, the profiles of both fields are shown in the bottom panels of Figs. 78. The oscillating kinks were found to be unstable for all values of the parameter within their region of existence. The instability is manifested by an abrupt deformation of the kink solution, even near its core, characterized by the inverse width , (where ). In Fig. 9, the top panel shows the profiles of the gauge field at the beginning () [solid (blue) line], and at the end of the integration () [solid (red) line]. While the shape of the kink is somehow preserved, it is clear that the solution profile has been significantly deformed. More importantly, the Higgs field , shown in the bottom panel, not only has been distorted but it has also become an order of magnitude larger than its initial amplitude. Thus, it can be concluded that oscillating kinks are unstable.

Figure 7: (Color online) Same as Fig. 1, but for a kink solution, for .
Figure 8: (Color online) Same as Fig. 2 for the kink solution, and for .
Figure 9: (Color online) Top panel: profile snapshots of the gauge field at the beginning [solid (blue) line], and at the end of the simulation [solid (red) line], for . Bottom panel: same as in top panel but for the Higgs field.
Figure 10: (Color online) Top panel: profile snapshots of the electric field for . Bottom panel: profile snapshots of the magnetic field for the same .

Iv Discussion and conclusions

In this work we have presented a class of classical solutions of the 1D Abelian Higgs model obtained with the use of a multiscale expansion method. The key assumption in our treatment is that the scalar field amplitude is much weaker than that of the gauge field; the relevant ratio was then used as a formal small parameter in the perturbation expansion. We have shown that the equations of motion can be reduced to a NLS equation; by means of the latter, localized solutions in the form of oscillons and oscillating kinks were derived. Results obtained by direct numerical integration of the original equations of motion where found to be in very good agreement with the analytical findings. In addition, we have numerically studied stability of the solutions against a Gaussian noise with amplitude up to of the Higgs field amplitude, and found that the oscillons remain robust.

It is also relevant to discuss the possible connection of the presented solutions to the physics of superconductors. One could, in principle, write down the form of the magnetic and electric fields originating from the gauge field which was chosen to be in the direction: , and . In the case of the oscillon solutions given in Eqs. (21)-(22), the above equations describe the electric field in he direction, which produces a magnetic field in the direction; both fields are localized around the origin of the axis – cf. Fig. 10, where the profiles of the fields are shown. This can be thought of as a configuration, describing Superconductor–Normal metal–Superconductor (SNS) Josephson junction paterno (), where two superconductors are linked by a thin normal conductor placed at the origin. Then, our solutions describe a condensate that oscillates around its vev near the origin, and acquires its vev value when entering the superconductors. Accordingly, the magnetic field is shown to oscillate inside the normal conductor, but vanishes exponentially inside the superconductors as per the Meissner effect.

We would like to add that these oscillon solutions are different from the phase-slip solutions which correspond to “electric” flux quantization in close loops in one-time one-space dimensions. The latter solutions correspond to an integer number of electric flux quanta through a space-time loop ivlev (); Langer () and they are topological singularities which correspond to the change of the phase of the condensate order parameter by a multiple of when we “travel” around such a loop once. Oscillons on the other hand are soliton solutions which are created by small-amplitude excitations around the (superconducting) vacuum with the spontaneously broken symmetry.

We note that it may be easier to observe such oscillon solutions more directly in rotating superfluids and, in particular, in atomic Bose-Einstein condensates of trapped ultra-cold bosonic atoms or in optical lattices in their superfluid phase. The same U(1)-Higgs classical field theory may describe the dynamics of the condensate order parameter, where the role of the external magnetic field is played by the local angular momentum of the rotating superfluid.

Our approach not only reveals a new class of solutions of the Abelian-Higgs model, but also dictates a straightforward general strategy for the search of non-trivial dynamics in models involving classical fields with nonlinear interactions. It is a natural perspective to determine the impact of these solutions on the thermal and quantum behaviour of the involved fields. Additionally, it would be extremely interesting to study the persistence and possible bifurcations of the solutions presented in this work in the presence of the Goldstone mode and additional components of the gauge field. In such a case, other nontrivial structures may emerge, whose stability and dynamics deserve to be investigated in detail. Still another interesting direction is the consideration of higher-dimensional settings. Such studies are currently in progress and relevant results will be reported elsewhere.

Acknowledgments. Illuminating discussions with L. P. Gork’ov are kindly acknowledged.

References

  • (1) E. J. Weinberg, Classical Solutions in Quantum Field Theory (Cambridge University Press, Cambridge, England, 2012). M. Gleiser, Int. J. Mod. Phys. D 16, 219 (2007); A. Rajantie and E. J. Copeland, Phys. Rev. Lett. 85, 916 (2000).
  • (2) M. A. Amin, R. Easther, H. Finkel, R. Flauger, and M. P. Hertzberg, Phys. Rev. Lett. 108, 241302 (2012).
  • (3) N. Graham, N. Stamatopoulos, Phys. Lett. B 639, 541 (2006);E. Farhi, N. Graham, A. H. Guth, N. Iqbal, R. R. Rosales, and N. Stamatopoulos, Phys. Rev. D 77, 085019 (2008).
  • (4) R. V. Konoplich, S. G. Rubin, A. S. Sakharov, M. Yu. Khlopov, Phys. Atom. Nucl. 62, 1593 (1999); I. Dymnikova, L. Koziel, M. Khlopov and S. Rubin, Grav. Cosmol. 6, 311 (2000); M. Yu. Khlopov, R. V. Konoplich, S. G. Rubin, A. S. Sakharov, Grav. Cosmol. 6, 153 (2000).
  • (5) S. Coleman, Aspects of Symmetry (Cambridge University Press, Cambridge, England, 1985); R. Rajaraman, Solitons and Instantons (North-Holland, Amsterdam, 1982).
  • (6) P. B. Umbanhowar, F. Melo, and H. L. Swinney, Nature 382, 793 (1996); L. S. Tsimring and I. S. Aranson, Phys. Rev. Lett. 79, 213 (1997).
  • (7) J. Rajchenbach, A. Leroux, and D. Clamond, Phys. Rev. Lett. 107, 024502 (2011); H. Xia, T. Maimbourg, H. Punzmann, and M. Shats, Phys. Rev. Lett. 109, 114502 (2012);
  • (8) R. F. Dashen, B. Hasslacher, and A. Neveu, Phys. Rev. D11, 3424 (1975); B. Piette and W. J. Zakrzewski, Nonlinearity 11, 1103 (1998).
  • (9) I.L. Bogolyubskii and V.G. Makhan’kov, [JETP Lett. 24, 12 (1976)]; I.L. Bogolyubskii and V.G. Makhan’kov, JETP Lett. 25, 107 (1977).
  • (10) D. K. Campbell, J. F. Schonfeld, and C. A. Wingate, Physica, D 9, 1 (1983).
  • (11) M. Gleiser, Phys. Rev. D 49, 2978 (1994); E. J. Copeland, M. Gleiser, H. -R. Müller, Phys. Rev. D 52, 1920 (1995); M. Gleiser, R. M. Haas, Phys. Rev. D 54, 1626 (1996).
  • (12) E. P. Honda and M. W. Choptuik, Phys. Rev. D 65, 084037 (2002).
  • (13) M. Hindmarsh and P. Salmi, Phys. Rev. D 74, 105005 (2006).
  • (14) M. Hindmarsh and P. Salmi, Phys. Rev. D 77, 105025 (2008).
  • (15) G. Fodor, P. Forgács, P. Grandclément, and I. Rácz, Phys. Rev. D 74, 124003 (2006).
  • (16) G. Fodor, P. Forgács, Z. Horváth, and Á. Lukács, Phys. Rev. D 78, 025003 (2008).
  • (17) M. Gleiser and D. Sicilia, Phys. Rev. Lett. 101, 011602 (2008).
  • (18) H. Segur and M. D. Kruskal, Phys. Rev. Lett. 58, 747 (1987).
  • (19) M. A. Amin, Phys. Rev. D 87, 123505 (2013).
  • (20) M. Gleiser and J. Thorarinson, Phys. Rev. D 76, 041701(R) (2007);M. Gleiser and J. Thorarinson, Phys. Rev. D 79, 025016 (2009).
  • (21) E. Farhi, N. Graham, V. Khemani, R. Markov, and R. Rosales, Phys. Rev. D 72, 101701(R) (2005).
  • (22) N. Graham, Phys. Rev. Lett. 98, 101801 (2007); N. Graham, Phys. Rev. D 76, 085017 (2007).
  • (23) E. I. Sfakianakis, arXiv:hep-th/1210.7568.
  • (24) L. P. Pitaevskii and S. Stringari, Bose-Einstein Condensation (Oxford University Press, Oxford, 2003).
  • (25) Y.-J. Lin, K. Jimenez-Garcia, and I. B. Spielman, Nature 471, 83 (2011).
  • (26) L. J. Garay, J. R. Anglin, J. I. Cirac, and P. Zoller, Phys. Rev. Lett. 85, 4643 (2000).
  • (27) P. G. Kevrekidis, D. J. Frantzeskakis and R. Carretero-González (eds.), Emergent Nonlinear Phenomena in Bose-Einstein Condensates: Theory and Experiment (Springer-Verlag, Heidelberg, 2008).
  • (28) L. P. Gork’ov, Sov. Phys. JETP 36, 1364 (1959).
  • (29) L. P. Gork’ov and G. M. Eliashberg, Z. Éksp. Teor. Fiz. 54, 612 (1968) [Sov. Phys. JETP 27, 328 (1968)]
  • (30) V. L. Ginzburg, L.D. Landau, Zh. Eksp. Teor. Fiz. 20, 1064 (1950).
  • (31) A. A. Abrikosov, Zh. Eksp. Teor. Fiz. 32, 1442 (1957) [Sov. Phys. JETP 5, 1174 (1957)].
  • (32) A. Vilenkin and E. P. S. Shellard, Cosmic Strings and Other Topological Defects (Cambridge University Press, Cambridge, England, 1994).
  • (33) L. D. Landau and E. M. Lifshitz Statistical Physics (Pergamon, New York, 1980), 3rd ed., part 2.
  • (34) C. Rebbi and R. Singleton, Jr., Phys. Rev. D 54, 1020 (1996); P. Arnold and L. McLerran, Phys. Rev. D 37, 1020 (1988).
  • (35) A. Jeffrey and T. Kawahara, Asymptotic methods in nonlinear wave theory, Pitman (1982).
  • (36) X. N. Maintas, C. E. Tsagkarakis, F. K. Diakonos, and D. J. Frantzeskakis, J. Mod. Phys. 3, 637 (2012); V. Achilleos, F. K. Diakonos, D. J. Frantzeskakis, G. C. Katsimiga, X. N. Maintas, C. E. Tsagkarakis, and A. Tsapalis, Phys. Rev. D 85, 027702 (2012).
  • (37) A. Barone and G. Paterno, Physics and Applications of the Josephson Effect (Wiley-Interscience, New York, 1982).
  • (38) Yu. S. Kivshar and G. P. Agrawal, Optical solitons: from fibers to photonic crystals (Academic Press, San Diego, 2003).
  • (39) R. S. Johnson, A modern introduction to the mathematical theory of water waves (Cambridge University Press, Cambridge, 2005).
  • (40) J. Yang, Nonlinear Waves in Integrable and Nonintegrable Systems (SIAM, Philadelphia, USA, 2010).
  • (41) The destabilization of plane waves under small-amplitude long-wavelength perturbations is known as €˜modulational instability™ or Benjamin-Feir instability [T. B. Benjamin and J. E. Feir, J. Fluid Mech. 27, 417 (1967)], and occurs in various contexts, including fluid mechanics [G. B. Whitham, J. Fluid Mech. 22, 273 (1965)], dielectrics [L. A. Ostrovsky, Sov. Phys. JETP 24, 797 (1967)], plasmas [A. Hasegawa, Phys. Fluids 15, 870 (1972)], etc.
  • (42) B. I. Ivlev and N. B. Kopnin, Sov. Phys. JETP Lett. 28, 592 (1979). B. I. Ivlev and N. B. Kopnin, Sov. Phys. Usp. 27, 206 (1984).
  • (43) J. S. Langer and V. Ambegaokar, Phys. Rev. 164, 498 (1967).
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