Examples for BPS Solitons Destabilized by Quantum Effects

Abstract

We investigate serval models for two scalar fields in one space dimension with topologically stable solitons that are constructed from BPS equations. The asymptotic behavior of these solitons fully determines their classical energies. A particular feature of the considered models is that there are several translationally invariant ground states that we call primary and secondary vacua. The former are those that are asymptotically assumed by the solitons. Solitons that occupy a secondary vacuum in finite but eventually large portions of space are classically degenerate. Thus the quantum contributions to the energies are decisive for the energetically favored soliton. While some of these solitons were constructed previously, we, for the first time, compute the leading (one-loop) quantum contribution their energies. In all cases considered we find that this contribution is not bounded from below and that it is the more negative the larger the region is in which the soliton approaches a secondary vacuum. This corroborates the conjecture, earlier inferred from the Shifman-Voloshin soliton, that the availability of secondary vacua destabilizes these solitons on the quantum level.

1. Introduction

Even though strictly speaking they are solitary waves, we use the notion solitons [1,2,3,4] for solutions to non-linear field equations that have localized (classical) energy densities and finite total energies. Examples for solitons in physics are Skyrmions [5,6], monopoles in $D=3+1$ space-time dimensions [7,8] and vortices, strings and lumps in $D=2+1$ [9,10,11]. Solitons have almost uncountable applications in various disciplines: in cosmology [12], condensed matter physics [13,14], magnetic systems [15] as well as hadron [16] and nuclear physics [17]. We point to those textbooks and review articles for more details and further references.

Here we focus on particular models with two scalar fields, $\varphi$ and $\chi$, in $D=1+1$ which have the particular feature of possessing two translationally invariant minimal energy configurations that we call primary and secondary vacua. In addition these models have Bogomol’nyi-Prasad-Sommerfield (BPS) [18,19] constructions that simplify the static soliton equations to first order differential equations. Within BPS constructions the classical energies are fully determined by the solitons’ asymptotic values [20]. While the solitons assume primary vacua at spatial infinity and are kink-like ($\varphi$ can be smoothly modified into the hyperbolic tangent function without changes at spatial infinity), they may dwell in a secondary vacuum within a finite region of space. We will see that the solitons are classically degenerate in a single, continuous parameter that controls size of that region. Because of that degeneracy there is no unique classical soliton and the quantum contribution to the energy, even if small when compared to the classical energy, will decide which is the energetically favored soliton. This scenario has recently been investigated for the Shifman-Voloshin-soliton [21]. It was found that, as a function of that single parameter, the leading, one-loop quantum correction to the energy, the so-called vacuum polarization energy (VPE) did not have a lower bound [22]. Hence no stable soliton exists in that model at the one-loop quantum level. It was hence conjectured that such quantum destabilization scenarios will occur whenever the soliton has access to a secondary vacuum. Here we will provide further examples to corroborate that conjecture.

We will employ spectral methods [23] to compute the VPE. These methods have been demonstrated to be very efficient when expressing the contribution from the continuum quantum fluctuations as an integral over imaginary momenta [24]. In Section 3 we will explain that the spectral methods yield the VPE from solving a single differential equation for the quantum fluctuations in the soliton background. This will also reveal that these methods can be applied straightforwardly and are less intricate than other methods as, for example, the heat kernel expansion [25] which has also been applied [26] to particular soliton solutions of the Shifman-Voloshin model. We will adopt the simple no-tadpole renormalization scheme that fully removes the ultraviolet divergent Feynman diagrams. In $D=1+1$ this scheme is equivalent to the formalism of Ref. [27] which has recently been linked to a normal-ordering description [28]. For the prime example of the kink in the ${\varphi }^4$ model, the no-tadpole prescription yields [23] the historic Dashen-Hasslacher-Neveu result [29].

In Section 2 we will discuss the properties of the BPS construction for the models under consideration. The relevant techniques from the spectral methods will be provided in Section 3. Section 4 contains our results, both for the construction of the solitons as well as their VPEs. Some concluding comments are contained in Section 5.

This article contains quite a number of mathematical symbols. We summarize and describe them in Table 1.

Table 1. Mathematical symbols used in the text and their meaning.

Symbol(s)	Description
x and t	space and time coordinates, respectively
$\mathcal{L}$	Lagrangian (density)
$\varphi$, $\chi$, ${\varphi }_i$, $\gamma$	scalar fields
${\varphi }_s$ and ${\chi }_s$	secondary vacua of the scalar fields
W	super-potential for the scalar fields
${\varphi }_i^{\left(s\right)}$	soliton profiles of scalar fields
${\eta }_i$	fluctuations about the soliton
$M_{ij}=\mathrm{diag}(m_1^2,m_2^2)$	mass matrix, containing the (squared) masses of the fluctuations
$m_{\varphi }$ and $m_{\chi }$	masses of the fluctuations with the mapping $m_1=\min (m_{\varphi },m_{\chi })$
$V_{ij}$	potential matrix for the fluctuations, generated by the soliton
$\omega$ or ${\omega }_k$	frequency/energy eigenvalues of the fluctuations
k and $k_2\left(k\right)$	wave-numbers of the fluctuations with masses $m_1$ and $m_2$, respectively
t and $\tilde{t}$	analytic continuation of k and $k_2$, respectively, to the imaginary axis
	the context clarifies whether t is the time or the imaginary momentum
$F_k\left(x\right)$ and $Z_k\left(x\right)$	Jost solution and its factor function, respectively
$\nu \left(t\right)$ and ${\nu }_1\left(t\right)$	Jost function and its Born approximation
$E_{\mathrm{cl}}$	classical energy of the soliton
$E_{\mathrm{VPE}}$	vacuum polarization energy (VPE)
$E_{\mathrm{CT}}$	counterterm contribution to the VPE
${\mathcal{F}}_{S,A}$, ${\mathcal{F}}_{\pm }$	matrices of Jost functions in various parity channels
${\mu }_i$ and b	model parameters
a	variational parameter for soliton profiles, defined by $\chi \left(0\right)=a{\chi }_s$
$E_0$ and $E_1$	fit parameters for the VPE

2. General Structure of the Sample Models

The models that we will discuss are defined by so-called super-potentials $W(\varphi ,\chi )$ [30] whose derivatives specify the Lagrangian

$$\mathcal{L}={\displaystyle \frac{1}{2}}\left\{{\dot{\varphi }}^2+{\dot{\chi }}^2-{\varphi }^{\prime 2}-{\chi }^{\prime 2}-{\left({\displaystyle \frac{\partial W}{\partial \varphi }}\right)}^2-{\left({\displaystyle \frac{\partial W}{\partial \chi }}\right)}^2\right\}.$$

(1)

Here dots and primes denote time (t) and space (x) derivatives, respectively. For static configurations, the classical energy then becomes a BPS construction

$$\begin{array}{cc}\hfill E_{\mathrm{cl}}& ={\displaystyle \frac{1}{2}}\int dx\left\{{\varphi }^{\prime 2}+{\chi }^{\prime 2}+{\left({\displaystyle \frac{\partial W}{\partial \varphi }}\right)}^2+{\left({\displaystyle \frac{\partial W}{\partial \chi }}\right)}^2\right\}\hfill \\ \hfill & ={\displaystyle \frac{1}{2}}\int dx\left\{{\left[{\varphi }^{\prime }\mp {\displaystyle \frac{\partial W}{\partial \varphi }}\right]}^2+{\left[{\chi }^{\prime }\mp {\displaystyle \frac{\partial W}{\partial \chi }}\right]}^2\right\}\pm W(\varphi ,\chi ){|}_{x=-\infty }^{\infty },\hfill \end{array}$$

(2)

where the signs must be chosen such that the boundary contribution is non-negative. Once the boundary values of the fields at positive and negative spatial infinity are prescribed, $E_{\mathrm{cl}}$ is minimized by the solutions to the first order equations

$${\varphi }^{\prime }=\pm {\displaystyle \frac{\partial W}{\partial \varphi }}\mathrm{and}{\chi }^{\prime }=\pm {\displaystyle \frac{\partial W}{\partial \chi }}.$$

(3)

As a consequence $E_{\mathrm{cl}}=\left|W(\varphi ,\chi ){|}_{x=\infty }-W(\varphi ,\chi ){|}_{x=-\infty }\right|$ whatever the solutions to the above equations look like.

Typically the super-potential is an even function of $\chi$ but it is odd in $\varphi$. Then ${\chi }^{\prime }$ vanishes whenever $\varphi$ does. In turn $\varphi$ and $\chi$ will, respectively, be odd and even functions of the spatial coordinate when the coordinate system is defined such that $\varphi \left(0\right)=0$. Hence the only undetermined initial condition for the BPS Equations (3) is $\chi \left(0\right)$. Without loss of generality we may take $\varphi (-\infty )>\varphi (\infty )$ and $W(\varphi ,\chi ){|}_{x=\infty }>W(\varphi ,\chi ){|}_{x=-\infty }$ so that the upper sign applies in Equations (2) and (3). Requiring that $\varphi$ is a monotonous function (like the ${\varphi }^4$-kink) then constrains ${\displaystyle \frac{\partial W}{\partial \varphi }}{|}_{x=0}<0$. Depending on the model parameters this condition can be fulfilled for a range of values $\chi \left(0\right)$. If so, the classical energy will be degenerate in $\chi \left(0\right)$ and the quantum correction to the energy will decide on the favored configuration.

Furthermore we have to specify the notion of primary and secondary vacua that correspond to the translationally invariant solutions of the BPS Equations (3). With the above mentioned properties of the super-potential under sign changes of the fields, ${\displaystyle \frac{\partial W}{\partial \chi }}=0$ when $\chi \equiv 0$ so that ${\displaystyle \frac{\partial W}{\partial \varphi }}{|}_{\chi =0}=0$ has (at least) two solutions (The two solutions must have opposite signs which allowed us to set $\varphi \left(0\right)=0$ above.) for $\varphi$. These are primary vacua and the soliton assumes one of them at negative spatial infinity and another one at the other end of the universe. As already mentioned, ${\displaystyle \frac{\partial W}{\partial \chi }}=0$ when $\varphi =0$. We can thus construct an alternative solution to ${\varphi }^{\prime }={\chi }^{\prime }=0$ by determining a constant, non-zero $\chi$ from ${\displaystyle \frac{\partial W}{\partial \varphi }}{|}_{\varphi =0}=0$. This is also a zero energy configuration which we call the secondary vacuum because we cannot build a (topological) soliton on top of it. The reason being that the profiles at positive and negative spatial infinity would be equal since $\chi$ is invariant under spatial reflection. However, by varying $\chi \left(0\right)$ we can find solitons on top of primary vacua that approach such a secondary vacuum configuration within a finite but eventually large portion of space. It is exactly this scenario that we will investigate for a number of models. We will also encounter situations in which the secondary vacuum has both $\chi \ne 0$ and $\varphi \ne 0$.

3. Vacuum Polarization Energy (VPE)

Here we briefly describe the computation of the VPE, i.e., the leading quantum contribution to the total energy, in the framework of spectral methods for the case of two scalar fields in $D=1+1$. These methods are by now well-established and in particular their almost effortless use when continuing the momenta of the scattering modes to the complex plane has recently been reviewed [24].

The point of departure is to parameterize the two fields as

$${\varphi }_i(x,t)={\varphi }_i^{\left(s\right)}\left(x\right)+{\eta }_i\left(x\right){\mathrm{e}}^{-\mathrm{i}\omega t}\mathrm{for}i=1,2.$$

(4)

The index $i=1,2$ stands for either the $\varphi$ or $\chi$ fields. The superscript refers to the soliton solutions constructed above and we have omitted the frequency argument for the small amplitude fluctuations ${\eta }_i\left(x\right)$. They are subject to the second order differential equations

$${\eta }_i^{″}=-{\omega }^2{\eta }_i+M_{ij}{\eta }_j+V_{ij}{\eta }_j,$$

(5)

that emerge from substituting the parameterization, Equation (4) into the Euler-Lagrangian equations derived from the Lagrangian $\mathcal{L}$, Equation (1) and linearizing in ${\eta }_i$. While $M=\left(M_{ij}\right)=\mathrm{diag}(m_1^2,m_2^2)$ contains the mass parameters, the potential matrix,

$$V_{ij}=V_{ij}\left(x\right)={\displaystyle \frac{1}{2}}{\displaystyle \frac{{\partial }^2}{\partial {\varphi }_i\partial {\varphi }_j}}{\left[{\left({\displaystyle \frac{\partial W}{\partial {\varphi }_1}}\right)}^2+{\left({\displaystyle \frac{\partial W}{\partial {\varphi }_2}}\right)}^2\right]}_{{\varphi }_i={\varphi }_i^{\left(s\right)}\left(x\right)}-M_{ij},$$

(6)

is generated by the soliton profiles and thus is time-independent so that different frequency modes decouple. The mass parameters are determined from the model parameters such that plane waves solve Equation (5) for $V\equiv 0$, which follows for a primary vacuum configuration. Once $m_{\varphi }$ and $m_{\chi }$ are determined, we map the fields $\varphi$ and $\chi$ onto ${\varphi }_1$ and ${\varphi }_2$ such that $m_1\le m_2$. We will provide more details on the matrices M and V in the context of the particular models in Section 4.

The VPE is computed as the renormalized sum of the shift in the zero-point energies

$$E_{\mathrm{VPE}}={\displaystyle \frac{1}{2}}\sum _k\left[{\omega }_k-{\omega }_k^{\left(0\right)}\right]+E_{\mathrm{CT}}.$$

(7)

The ${\omega }_k$ are the energy eigenvalues in Equation (5) and ${\omega }_k^{\left(0\right)}$ are their counterparts for $V\equiv 0$. The counterterm contribution, $E_{\mathrm{CT}}$ emerges from substituting the soliton profiles into the counterterm Lagrangian that cancels the ultra-violet divergences in the sum over the eigenmodes. In $D=1+1$ we only need a single counterterm and we implement the no-tadpole condition to fix its finite piece. This condition removes the $\mathcal{O}\left(V\right)$ contribution from the sum. We can indeed remove this contribution fully and not only at a particular renormalization scale because the only ultra-violet divergent Feynman diagram has a loop that starts and ends at the same point and thus does not depend on the momenta of the external line(s). We will compute the sum in Equation (7) from scattering data extracted from the solutions to Equation (5). The Born approximation to these data is $\mathcal{O}\left(V\right)$. Hence with the no-tadpole condition we merely subtract the Born approximation from the scattering data expression for the sum in Equation (7) and then drop $E_{\mathrm{CT}}$ completely.

The sum, Equation (7) has contributions from discrete bound states ${\omega }_k\le m_1$ and continuous scattering states ${\omega }_k>m_1$. For the considered scenarios there are typically two zero mode bound states. One for the translational symmetry and one that arises because the classical energy is invariant when $\chi \left(0\right)$ is varied. There may be further bound states depending on the peculiarities of the models. The continuum contribution is computed by integrating the dispersion relation $\omega =\sqrt{k^2+m_1^2}$ weighted by the change of the density of states induced by the soliton, $\delta \rho \left(k\right)={\displaystyle \frac{1}{\pi }}{\displaystyle \frac{d\delta \left(k\right)}{dk}}$ [29,31] where the phase shift is extracted from the scattering matrix: $\delta \left(k\right)={\displaystyle \frac{1}{2\mathrm{i}}}\ln \det S\left(k\right)$. However, for numerical purpose, the phase shift is not computed from the scattering matrix but rather we use that the phase shift is the phase of the Jost function which by itself is extracted from solutions to Equation (5) that resemble out-going plane waves as $x\to +\infty$. This function is analytic in the upper half of the complex momentum plane and has zeros at the imaginary wave-numbers of the bound states [32]. With the subtraction of its Born approximation we can then compute the integral over the continuum modes as a contour integral because there is no contribution from the semi-circle at $\left|k\right|\to \infty$. Furthermore the above mentioned zeros produce poles in the logarithmic derivative of the phase of the Jost function and cancel the explicit bound state contribution in Equation (7). All what is left in the contour integral is the contribution from circling the branch cut in $\sqrt{k^2+m_1^2}$ along the imaginary axis for $k=\mathrm{i}t\pm ϵ$ and $t\ge m_1$. After a final integration by parts we are left with a very compact formula for the VPE

$$E_{\mathrm{VPE}}={\displaystyle \frac{1}{2\pi }}{\int }_{m_1}^{\infty }{\displaystyle \frac{dt}{\sqrt{t^2-m_1^2}}}\left[\nu \left(t\right)-{\nu }_1\left(t\right)\right]={\int }_0^{\infty }{\displaystyle \frac{d\tau }{2\pi }}{\left[\nu \left(t\right)-{\nu }_1\left(t\right)\right]}_{t=\sqrt{{\tau }^2+m_1^2}},$$

(8)

where $\nu$ is logarithm of the Jost function and ${\nu }_1$ is its Born approximation. In either case a sum of scattering channels is understood.

Next we recall the calculation of the Jost function for theories with two fields in $D=1+1$ which has been developed in Ref. [33] for the case that there is some kind of symmetry that relates the wave-equation for $x\ge 0$ and $x\le 0$. Starting point is the Jost solution that we elevate to a matrix function

$$F_k\left(x\right)=Z_k\left(x\right)\left(\begin{array}{cc}{\mathrm{e}}^{\mathrm{i}kx}& 0\\ 0& {\mathrm{e}}^{\mathrm{i}{k}_{2}x}\end{array}\right)\mathrm{with}{k}_2=k_2\left(k\right)\equiv k\sqrt{1-{\displaystyle \frac{m_2^2-m_1^2}{{\left[k+\mathrm{i}{0}^{+}\right]}^2}}},$$

(9)

and ${lim}_{x\to \infty }{Z}_k\left(x\right)=1$. The elements within a given column represent the two fields while the two columns represent the scattering channels, i.e., out-going plane waves for only either the ${\varphi }_1$ or ${\varphi }_2$ fields. The $\mathrm{i}{0}^{+}$ prescription for the momentum of the heavier field ensures that $F_k\left(x\right)$ is also analytic in the gap $0\le k\le \sqrt{m_2^2-m_1^2}$. Yet, this problem does not occur when, as motivated above, the VPE is computed from imaginary momenta (See Ref. [34] for the real momenta version.). The scattering wave-function, ${\Psi }_{\mathrm{sc}.\left(\mathrm{x}\right)}$, is a linear combination of $F_k\left(x\right)$ and $F_{-k}\left(x\right)$. Assuming, for the time being, that the symmetric (S) and anti-symmetric (A) channels decouple, the corresponding scattering matrices are obtained from ${\Psi }_{\mathrm{sc}.}^{\left(S\right)\prime }\left(0\right)=0$ and ${\Psi }_{\mathrm{sc}.}^{\left(A\right)}\left(0\right)=0$. That is, the scattering matrices $S^{(S,A)}\left(k\right)$ are determined from $F_k\left(0\right)$ and $F_k^{\prime }\left(0\right)$. The phase shifts ${\delta }_{S,A}\left(k\right)={\displaystyle \frac{1}{2\mathrm{i}}}\ln \det \left[S_{S,A}\left(k\right)\right]$ are then expressed in terms of $F_k\left(0\right)$ and $F_k^{\prime }\left(0\right)$. We will not present these expression but rather turn to the imaginary axis formulation and write $Z_{\mathrm{i}t}\left(x\right)=Z(t,x)$ for the analytically continuated factor matrix, whose second order differential equation is

$$Z^{\prime \prime }(t,x)=2Z^{\prime }(t,x)D\left(t\right)+\left[M^2,Z(t,x)\right]+V\left(x\right)Z(t,x)\mathrm{with}D\left(t\right)=\left(\begin{array}{cc}t& 0\\ 0& \tilde{t}\end{array}\right)$$

(10)

and $\tilde{t}=\sqrt{t^2-m_1^2+m_2^2}$. The analytically continued combinations of $F_k\left(0\right)$ and $F_k^{\prime }\left(0\right)$ that enter $S_{S,A}\left(k\right)$ are

$${\mathcal{F}}_S\left(t\right)=\underset{x\to 0}{lim}\left[Z(t,x)-Z^{\prime }(t,x)D^{-1}\left(t\right)\right]\mathrm{and}{\mathcal{F}}_A\left(t\right)=\underset{x\to 0}{lim}Z(t,x).$$

(11)

These are the so-called Jost matrices in the symmetric and anti-symmetric channels. For the problem at hand the symmetric and anti-symmetric channel do, unfortunately, not decouple. The field potential in Equation (1) is even in both fields. Hence the diagonal elements of the scattering potential, Equation (6) are even functions of both fields while its off-diagonals are odd. With the above discussed properties of the profiles, it is then obvious that $V(-x)={\tau }_{3}V\left(x\right){\tau }_3$. Therefore the scattering problem decouples in the parity channels ${\Psi }_{\pm }(-x)=\pm {\tau }_3{\Psi }_{\pm }\left(x\right)$ and the relevant Jost matrices are [33]

$${\mathcal{F}}_{\pm }\left(t\right)=\left[P_{\pm }{\mathcal{F}}_S\left(t\right)D_{\mp }\left(t\right)+P_{\mp }{\mathcal{F}}_A\left(t\right)D_{\pm }^{-1}\left(t\right)\right],$$

(12)

with projectors $P_{\pm }={\displaystyle \frac{1}{2}}\left[1\pm {\tau }_3\right]$ as well as modified factor matrices $D_{+}\left(t\right)=\left(\begin{array}{cc}-t& 0\\ 0& 1\end{array}\right)$ and $D_{-}\left(t\right)=\left(\begin{array}{cc}1& 0\\ 0& -\tilde{t}\end{array}\right)$. The combinations in Equation (12) essentially exchange the second (first) rows of ${\mathcal{F}}_S$ and ${\mathcal{F}}_A$ for the positive (negative) parity channel and add appropriate kinematic factors. From this we find the relevant logarithm that enters Equation (8)

$$\nu \left(t\right)\equiv \ln \det \left[{\mathcal{F}}_{+}\left(t\right){\mathcal{F}}_{-}\left(t\right)\right],$$

(13)

since the sum of the logarithms is the logarithm of the product. The off-diagonal elements of $V\left(x\right)$ only enter at second order. Hence the Born approximation is just the sum of the Born approximations for the decoupled problem,

$${\nu }_1\left(t\right)={\int }_0^{\infty }dx\left[{\displaystyle \frac{V_{11}\left(x\right)}{t}}+{\displaystyle \frac{V_{22}\left(x\right)}{\tilde{t}}}\right].$$

(14)

Now we have collected all entries to compute the VPE in the no-tadpole renormalization scheme.

As we have summarized the theoretical background, we briefly describe the numerical treatment leading to the VPE as a function of $\chi \left(0\right)$. Generally, all differential equations are integrated with Runge-Kutta algorithms combined with adaptive step size controls. For a particular model described by the superpotential W we determine the vacua, in particular the secondary vacuum ${\chi }_s$ of the second scalar field, as functions of the model parameters. Then we prescribe $0\le \chi \left(0\right)<{\chi }_s$ (and $\varphi \left(0\right)=0$) to solve the first order Equations (3). This yields arrays of the profile functions ${\varphi }_n$ and ${\chi }_n$ at distinct points $0\le x_n<\infty$. (In all numerical computations ‘∞’ refers to a numerical value large enough so that the numerical results are stable under moderate changes of this value.) These arrays enter the scattering potential $V_{ij}({\varphi }_n,{\chi }_n)$. Typically the adaptive step size control requires the potential at points $x\notin \left\{x_n\right\}$ and we interpolate between neighboring points. Using ${lim}_{x\to \infty }{Z}_k\left(x\right)=1$ we then integrate the differential Equation (10) to obtain $Z(t,0)$ and $Z^{\prime }(t,0)$. To determine the (imaginary) momentum t for which we actually integrate the differential Equation (10) we define the function $ϵ\left(\tau \right)$ subject to the differential equation

$${\displaystyle \frac{dϵ\left(\tau \right)}{d\tau }}=\nu \left(\sqrt{{\tau }^2-m_1^2}\right)-{\nu }_1\left(\sqrt{{\tau }^2-m_1^2}\right)\mathrm{with}ϵ\left(0\right)=0,$$

so that $E_{\mathrm{VPE}}={\displaystyle \frac{1}{2\pi }}ϵ(\infty )$. Integrating this differential equation with an adaptive step control is advantageous because it carefully treats the logarithmic behavior of $\nu \left(\tau \right)$ for $\tau \lesssim 0$ that originates from the zero modes. This behavior also requires a very tiny lower bound, $\mathcal{O}\left({10}^{-5}\right)$ when numerically integrating the above differential equation. Within a given model we finally obtain $E_{\mathrm{VPE}}$ as a function of the variational parameter a defined by $\chi \left(0\right)=a{\chi }_s$.

4. Sample Models

We introduce dimensionless variables and fields. This rescaling leaves an overall factor for the Lagrangian which does not affect the classical equations of motion. However, it enters the relation between the canonical field momenta and their velocities. In turn it acts as a loop-counter in the sense that it is a relative weight between $E_{\mathrm{cl}}$ and $E_{\mathrm{VPE}}$. Fortunately, for a given model with fixed model parameters, we will only compare the VPEs for configurations with equal $E_{\mathrm{cl}}$ so that this relative factor is not relevant.

In all numerical calculations we adopt sign conventions such that the kink-like profile, $\varphi \left(x\right)$ connects a positive primary vacuum at negative spatial infinity to its negative counterpart at positive spatial infinity. Furthermore we take all model parameters to be non-negative.

As a reminder we list the super-potential of the Shifman-Voloshin model [21], see also [35],

$$W(\varphi ,\chi )={\displaystyle \frac{1}{3}}{\varphi }^3-\varphi +{\displaystyle \frac{\mu }{2}}\varphi {\chi }^2.$$

(15)

The primary vacua are at $\varphi =\pm 1$ and $\chi =0$. The secondary vacua are at ${\varphi }_s=0$ and ${\chi }_s=\pm \sqrt{{\displaystyle \frac{2}{\mu }}}$. Solutions (that are classically degenerate) exist for $\left|\chi \left(0\right)\right|\le \sqrt{{\displaystyle \frac{2}{\mu }}}$ and, as shown in Ref. [22], the VPE does not have a lower bound as $\left|\chi \left(0\right)\right|\nearrow \sqrt{{\displaystyle \frac{2}{\mu }}}$ except for the particular case of $\mu =2$ for which the model can be mapped onto a model with two decoupled scalar fields that have the standard quartic interaction with spontaneous symmetry breaking. We next turn to three further models that exhibit similar features.

In the following we will discuss solitons in three other models with secondary vacua. We will encounter that the structure of these secondary vacua varies with the model parameters. We will tabulate numerical results for our main objective, the VPEs in these models, as functions of the model parameters and, more enlightening, as functions of the variational parameters that distinguish the classically degenerate solitons. The dependencies of the VPEs on these variational parameters will be our central results.

4.1. Model A

We replace the last term in Equation (15) by a sine-Gordon type interaction and introduce a second model parameter

$$W(\varphi ,\chi )={\displaystyle \frac{{\mu }_2}{3}}{\varphi }^3-\varphi +{\mu }_1\varphi \left[1-cos\chi \right].$$

(16)

From the super-potential in Equation (16) we get the static BPS equations

$${\varphi }^{\prime }={\mu }_2{\varphi }^2-1+{\mu }_1\left[1-cos\chi \right]\mathrm{and}{\chi }^{\prime }={\mu }_1\varphi sin\chi .$$

(17)

The primary vacua are at $\varphi =\pm {\displaystyle \frac{1}{\sqrt{{\mu }_2}}}$ and $\chi =0$. We expand the fields around these vacua and read of the mass parameters $m_{\varphi }=2\sqrt{{\mu }_2}$ and $m_{\chi }={\displaystyle \frac{{\mu }_1}{\sqrt{{\mu }_2}}}$. For ${\mu }_1\ge {\displaystyle \frac{1}{2}}$ the secondary vacua are obviously at $\varphi =0$ and $\chi =\arccos \left(1-{\displaystyle \frac{1}{{\mu }_1}}\right)$ and the situation is similar to the Shifman-Voloshin model. Examples for the soliton profiles are shown in Figure 1 for various values of $a=\chi \left(0\right)/\arccos \left(1-{\displaystyle \frac{1}{{\mu }_1}}\right)$. While, by construction, the profiles approach a primary vacuum at spatial infinity, they occupy a secondary vacuum in an ever increasing region as $a\nearrow 1$. Of course, the classical energy, $E_{\mathrm{cl}}={\displaystyle \frac{4}{3\sqrt{{\mu }_2}}}$ does not depend on a.

Figure 1. Soliton profiles for model A with ${\mu }_1=0.7$ and ${\mu }_2=0.6$ for various values of the variational parameter a. The secondary vacuum has ${\varphi }_s=0$ and ${\chi }_s=\arccos \left(1-{\displaystyle \frac{1}{{\mu }_1}}\right)\approx 2.014$.

The computation of the VPE requires the potential matrix (for the case $m_{\varphi }\le m_{\chi }$ so that ${\varphi }_1=\varphi$ and ${\varphi }_2=\chi$)

$$V=\left(\begin{array}{cc}6{\mu }_2\left[{\mu }_2{\varphi }^2-1+{\displaystyle \frac{{\mu }_1}{3}}\left(1-c\right)\right]+{\mu }_1^2{s}^2& 2{\mu }_1{\mu }_2\varphi s+{\mu }_1^2\varphi sc\\ 2{\mu }_1{\mu }_2\varphi s+2{\mu }_1^2\varphi sc& \begin{array}{cc}\hfill & {\mu }_1\left[{\mu }_2{\varphi }^2-1+{\mu }_1\left(1-c\right)\right]c\hfill \\ \hfill & +{\mu }_1^2{s}^2+{\mu }_1^2{\varphi }^2\left[c^2-s^2\right]-{\displaystyle \frac{{\mu }_1^2}{{\mu }_2}}\hfill \end{array}\end{array}\right),$$

(18)

with $s=sin\chi$ and $c=cos\chi$. By substituting the soliton profiles for $\varphi$ and $\chi$ we compute the VPE with the formalism of Section 3. Not surprisingly we find that it does depend on the degeneracy parameter a. Neither are we surprised that the VPE does not have a lower bound as can be inferred from Table 2 in which we list the VPE for numerous values of ${\mu }_1>{\displaystyle \frac{1}{2}}$.

Table 2. VPE for model A as a function of the model parameter ${\mu }_1>{\displaystyle \frac{1}{2}}$ and the variational parameter a for ${\mu }_2=0.4$.

	${\mathit{\mu }}_1$	0.6	0.8	1.0	1.2	1.6
a
0.0		−0.728	−0.843	−0.969	−1.107	−1.421
0.2		−0.731	−0.845	−0.971	−1.109	−1.423
0.5		−0.757	−0.859	−0.982	−1.120	−1.441
0.9		−0.999	−0.961	−1.059	−1.206	−1.590
0.99		−1.548	−1.153	−1.190	−1.344	−1.832
0.999		−2.116	−1.348	−1.321	−1.482	−2.073
0.9999		−2.683	−1.543	−1.452	−1.620	−2.314
0.99999		−3.250	−1.737	−1.582	−1.758	−2.555

For ${\mu }_1<{\displaystyle \frac{1}{2}}$ and $\left|\varphi \right|<{\displaystyle \frac{1}{\sqrt{{\mu }_2}}}$ we cannot accommodate ${\varphi }^{\prime }=0$. However, there is a secondary vacuum since ${\chi }^{\prime }=0$ when $\chi =\pi$ and then we have ${\varphi }^{\prime }=0$ for $\varphi =\sqrt{{\displaystyle \frac{1-2{\mu }_1}{{\mu }_2}}}$. Such a scenario is not contained in the Shifman-Voloshin model. Examples for the resulting soliton profiles are shown in Figure 2 for various values of the variational parameter $a={\displaystyle \frac{\chi \left(0\right)}{\pi }}$.

Figure 2. Soliton profiles for model A with ${\mu }_1=0.4$ and ${\mu }_2=0.6$ for various values of the variational parameter a. Here the secondary vacuum is at $\varphi =-\sqrt{{\displaystyle \frac{1-2{\mu }_1}{{\mu }_2}}}\approx -0.577$ and $\chi =\pi$.

As a tends to one, the $\chi$ profile remains in that secondary vacuum for an ever growing region while the $\varphi$ profile quickly drops from zero to its secondary vacuum value. Again, the VPE does not have a lower bound as the region grows in which the profiles assume their secondary vacua. In Table 3 we list the $E_{\mathrm{VPE}}$ for an exemplary set of model parameters as a function of a for the scenario that has ${\chi }_s=\pi$.

Table 3. Same as Table 2 for various model parameters ${\mu }_1<{\displaystyle \frac{1}{2}}$ and ${\mu }_2=0.1$.

	${\mathit{\mu }}_{\mathbf{1}}$	0.10	0.20	0.30	0.40	0.45
$\mathit{a}$
0.0		−0.311	−0.421	−0.554	−0.710	−0.798
0.2		−0.312	−0.424	−0.559	−0.720	−0.810
0.5		−0.324	−0.451	−0.605	−0.796	−0.908
0.9		−0.401	−0.618	−0.9193	−1.429	−1.916
0.99		−0.439	−0.714	−1.147	−2.037	−3.122
0.999		−0.449	−0.750	−1.260	−2.405	−3.902
0.9999		−0.456	−0.778	−1.356	−2.730	−4.598
0.99999		−0.463	−0.806	−1.449	−3.044	−5.271

In Figure 3 we verify that as $a\nearrow 1$ for both ${\mu }_1<{\displaystyle \frac{1}{2}}$ and ${\mu }_1>{\displaystyle \frac{1}{2}}$ the VPE essentially approaches negative infinity like $ln(1-a)$. Obviously there is no lower bound to the VPE and the quantum effects tend to destabilize this soliton whatever the secondary vacuum is.

Figure 3. The VPE for the model defined in Equation (16) as a function of the variable that measures the deviation from the secondary vacuum.

4.2. Model B

The next model is characterized by the super-potential

$$W(\varphi ,\chi )={\displaystyle \frac{1}{3}}{\varphi }^3-\varphi -\varphi {\left({\chi }^2-{\mu }_1\right)}^2+{\mu }_2\varphi {\chi }^2,$$

(19)

leading to the BPS equations

$${\varphi }^{\prime }={\varphi }^2-1-{\left({\chi }^2-{\mu }_1\right)}^2+{\mu }_2{\chi }^2\mathrm{and}{\chi }^{\prime }=-2\varphi \chi \left(2{\chi }^2-2{\mu }_1-{\mu }_2\right).$$

(20)

The primary vacua are at $\chi =0$ and $\varphi =\pm \sqrt{1+{\mu }_1^2}$. The associated mass parameters are $m_{\varphi }=2\sqrt{1+{\mu }_1^2}$ and $m_{\chi }=\left(2{\mu }_1+{\mu }_2\right)m_{\varphi }$. When $g({\mu }_1,{\mu }_2)\equiv {\mu }_2\left({\mu }_1+{\displaystyle \frac{{\mu }_2}{4}}\right)\le 1$, or equivalently ${\mu }_2\le 2\left(\sqrt{1+{\mu }_1^2}-{\mu }_1\right)$ there are secondary vacua at ${\chi }_s^2={\mu }_1+{\displaystyle \frac{{\mu }_2}{2}}$ and ${\varphi }_s=\pm \sqrt{1-{\mu }_2\left({\mu }_1+{\displaystyle \frac{{\mu }_2}{4}}\right)}$. If we want to construct soliton solutions whose profiles decrease monotonously so that $\varphi \left(ϵ\right)=-Kϵ$ with $K>0$ and $ϵ\to 0$, the right-hand-sides in Equation (20) may not be positive. This requires ${\chi }^2\le {\mu }_1+{\displaystyle \frac{{\mu }_2}{2}}$. Parameterizing $\chi \left(0\right)=a\sqrt{{\mu }_1+{\displaystyle \frac{{\mu }_2}{2}}}$ the right hand side of the differential equation for $\varphi$ is non-positive for $\varphi \sim 0$ and $a\lesssim 1$ only when the above condition on the secondary vacuum is fulfilled. That is, the conditions on the secondary vacuum and the existence of a soliton are identical. A sample soliton solution is shown in Figure 4. The behavior generalizes: as $a\nearrow 1$ the profiles approach a secondary vacuum in a large portion of space. However, that portion does not include $x=0$ because $\varphi \ne 0$ in that vacuum.

Figure 4. Soliton profiles for model B with ${\mu }_1=0.2$ and ${\mu }_2=1.6$ for various values of the variational parameter a. The secondary vacuum has ${\varphi }_s=-0.2$ and ${\chi }_s=1$.

We abstain from presenting the potential matrix V for this model and directly move to the discussion of our numerical results for the VPE. To explore the parameter dependence efficiently we write ${\mu }_2=2b\left(\sqrt{1+{\mu }_1^2}-{\mu }_1\right)$ with $b<1$. The results in terms of the model parameter b and the variational parameter a are listed in Table 4.

Table 4. Vacuum polarization energy for the model defined by the super-potential Equation (19) for ${\mu }_1=0.2$. The parameters b and a, respectively, determine the model parameter ${\mu }_2$ and initial value of the profile $\chi \left(0\right)$, cf. text.

	$\mathit{b}$	0.00	0.20	0.40	0.60	0.80	0.99
$\mathit{a}$
0.0		−0.940	−1.158	−1.403	−1.679	−1.990	−2.316
0.2		−0.940	−1.161	−1.409	−1.689	−2.002	−2.334
0.5		−0.947	−1.189	−1.458	−1.762	−2.109	−2.498
0.9		−1.086	−1.433	−1.823	−2.306	−3.035	−5.285
0.99		−1.289	−1.684	−2.096	−2.653	−3.761	−13.268
0.999		−1.462	−1.900	−2.265	−2.731	−3.883	−17.852
0.9999		−1.639	−2.155	−2.496	−2.848	−3.934	−21.425
0.99999		−1.817	−2.425	−2.763	−3.009	−3.992	−24.677
0.999999		−1.995	−2.699	−3.045	−3.192	−4.059	−27.782

Again we can fit a function linear in $ln(1-a)$ to the VPE for $a\lesssim 1$. We find that the critical value for a at which this behavior sets in increases with b. In any event, there is no lower bound for the VPE suggesting again that the soliton is not stable. The effect is the more pronounced as the model parameters get closer to the limiting case for which the soliton accesses the secondary vacuum.

As $g({\mu }_1,{\mu }_2)\nearrow 1$, $\varphi$ approaches zero in the secondary vacuum. When $g({\mu }_1,{\mu }_2)$ exceeds unity, ${\varphi }_s$ stays at zero but ${\chi }_s^2$ decreases from ${\mu }_1+{\displaystyle \frac{{\mu }_2}{2}}$ to ${\mu }_1+{\displaystyle \frac{{\mu }_2}{2}}-\sqrt{{\mu }_2\left({\mu }_1+{\displaystyle \frac{{\mu }_2}{4}}\right)-1}$ in the secondary vacuum. (The configuration with the positive square root is also a solution but does not support stable solitons.) A set of soliton solutions for the parameterization $\chi \left(0\right)=a{\left[{\mu }_1+{\displaystyle \frac{{\mu }_2}{2}}-\sqrt{{\mu }_2\left({\mu }_1+{\displaystyle \frac{{\mu }_2}{4}}\right)-1}\right]}^{{\displaystyle \frac{1}{2}}}$ and $a\nearrow 1$ is shown in Figure 5.

Figure 5. Soliton profiles for model B with ${\mu }_1=0.8$ and ${\mu }_2=1.2$ for various values of the variational parameter a. The secondary vacuum has ${\varphi }_s=0$ and ${\chi }_s\approx 0.91$.

The notation for the model parameters remains unchanged, but now we take $b>1$. As before, for large enough a we can approximate the VPEs listed in Table 5 by a function that is linear in $ln(1-a)$.

Table 5. Vacuum polarization energy for the model defined by the super-potential Equation (19) for ${\mu }_1=0.2$. The parameters b and a, respectively, determine the model parameter ${\mu }_2$ and initial value of the profile $\chi \left(0\right)$, cf. text.

	$\mathit{b}$	1.10	1.20	1.30	1.40	1.50	1.60
$\mathit{a}$
0.0		−2.520	−2.714	−2.917	−3.130	−3.351	−3.581
0.2		−2.533	−2.726	−2.930	−3.142	−3.364	−3.595
0.5		−2.639	−2.825	−3.027	−3.243	−3.469	−3.707
0.9		−3.536	−3.559	−3.720	−3.940	−4.195	−4.476
0.99		−5.387	−4.882	−4.894	−5.088	−5.374	−5.719
0.999		−7.318	−6.231	−6.080	−6.241	−6.555	−6.963
0.9999		−9.251	−7.580	−7.265	−7.393	−7.736	−8.206
0.99999		−11.184	−8.929	−8.450	−8.546	−8.917	−9.449
0.999999		−13.117	−10.278	−9.635	−9.698	−10.097	−10.692

4.3. Model C

This model is taken from Ref. [36]. It is motivated by the super-potential of model A but subsequently the kink-type field is written as $\varphi =sinh\gamma$, so that the metric in the field space $\gamma -\chi$ depends on the fields. To return to a constant metric but nevertheless have a BPS construction the super-potential is modified to

$$W(\gamma ,\chi )=\mu {\chi }^{2}sinh\gamma +\int d\gamma \left[{sinh}^2\gamma -1\right]\left[{\displaystyle \frac{2\mu }{cosh\gamma }}+(1-2\mu )cosh\left(\gamma \right)\right].$$

(21)

The fact that this potential is only known as an indefinite integral is not really a problem. We would need to integrate from $\gamma (-\infty )$ to $\gamma (\infty )$ for the classical energy. The integral is over $\gamma$ rather than the spatial coordinate and thus is not sensitive to the form of the soliton.

For the BPS equations we only require the $\gamma$-derivative of that integral yielding

$${\gamma }^{\prime }=\mu {\chi }^{2}cosh\gamma +\left[{sinh}^2\gamma -1\right]\left[{\displaystyle \frac{2\mu }{cosh\gamma }}+(1-2\mu )cosh\left(\gamma \right)\right]\mathrm{and}{\chi }^{\prime }=2\mu \chi sinh\gamma .$$

(22)

Again the primary vacua are at $sinh\gamma =\pm 1$ and $\chi =0$ while the secondary vacua are at ${\gamma }_s=0$ and ${\chi }_s=\pm {\displaystyle \frac{1}{\sqrt{\mu }}}$. We therefore introduce the variational parameter a in the initial condition $\chi \left(0\right)={\displaystyle \frac{a}{\sqrt{\mu }}}$. As long as $\chi \le {\displaystyle \frac{1}{\sqrt{\left|\mu \right|}}}$, the right-hand-side of ${\gamma }^{\prime }$ is negative for $\gamma =0$ and any value of $\mu$. Hence we expect degenerate solutions for all $\mu >0$. The inequality arises from the demanding that the right-hand-side of ${\chi }^{\prime }$ is negative when $\chi >0$ and $\gamma <0$. Furthermore the mass parameters $m_{\gamma }=4\left(1-\mu \right)$ and $m_{\chi }=2\mu$ are obtained from expanding Equation (22) around the primary vacuum ($sinh\gamma =\pm 1,\chi =0$). Thus the existence of a BPS soliton on top of the above mentioned primary vacua yields the upper bound $\mu <1$. Profiles determined subject to this condition are shown in Figure 6.

Figure 6. Soliton profiles $\varphi =sinh\gamma$ and $\varphi$ for model C with $\mu =0.5$. The secondary vacuum has ${\gamma }_s=0$ and ${\chi }_s=\sqrt{2}\approx 1.41$.

We observe the by now familiar behavior that the soliton approaches the secondary vacuum as $a\nearrow 1$.

Again we abstain from displaying the bulky expressions for the scattering potential and immediately list the numerical results for the VPE in Table 6.

Table 6. VPE of model C for different values of the model parameter $\mu <1$ and the variational parameter a.

	$\mathit{\mu }$	0.4	0.6	0.8	0.9	0.95
$\mathit{a}$
0.0		−1.076	−0.899	−1.046	−1.482	−2.050
0.2		−1.090	−0.908	−1.075	−1.541	−2.142
0.5		−1.169	−0.958	−1.233	−1.859	−2.630
0.9		−1.487	−1.080	−1.683	−2.828	−4.152
0.99		−1.886	−1.126	−1.998	−3.658	−5.539
0.999		−2.268	−1.159	−2.273	−4.414	−6.816
0.9999		−2.647	−1.191	−2.546	−5.167	−8.094
0.99999		−3.026	−1.223	−2.819	−5.919	−9.367

For $\mu >{\displaystyle \frac{1}{2}}$ and $\chi =0$ the right-hand-side of the differential equation for $\gamma$ has another zero at ${cosh}^2\gamma ={\displaystyle \frac{2\mu }{2\mu -1}}$ or ${sinh}^2\gamma ={\displaystyle \frac{1}{2\mu -1}}$, which is less than 1 for $\mu >1$. In that case the soliton assumes $\pm \mathrm{arcosh}\left(\sqrt{{\displaystyle \frac{2\mu }{2\mu -1}}}\right)$ at spatial infinity (This configuration actually is a maximum of the action density for ${\displaystyle \frac{1}{2}}<\mu <1$.). The mass parameters for these primary vacua are $m_{\gamma }={\displaystyle \frac{4\mu -4}{\sqrt{2\mu -1}}}$ and $m_{\chi }={\displaystyle \frac{2\mu }{\sqrt{2\mu -1}}}$. The expressions for the secondary vacua are as in the case with $\mu <1$.

From the graphs in Figure 7 and the data in Table 7 we observe that the resulting VPEs show the same tendency as the other models (including the Shifman-Voloshin case) to approach negative infinity like $ln(1-a)$.

Figure 7. Soliton profiles $\varphi =sinh\gamma$ and $\varphi$ for model C with $\mu =1.5$. The primary vacua are at $\varphi ={\displaystyle \frac{\pm 1}{\sqrt{2\mu -1}}}\approx \pm 0.71$ or $\gamma \approx \pm 0.66$ and $\chi =0$. The secondary vacuum has ${\varphi }_s=0$ and ${\chi }_s=\sqrt{{\displaystyle \frac{2}{3}}}\approx 0.82$.

Table 7. Same as Table 6 for $\mu >1$.

	$\mathit{\mu }$	1.05	1.10	1.20	1.40	1.60
$\mathit{a}$
0.2		−2.312	−1.814	−1.464	−1.322	−1.355
0.5		−2.830	−2.182	−1.700	−1.457	−1.448
0.9		−4.465	−3.342	−2.439	−1.865	−1.720
0.99		−5.996	−4.401	−3.082	−2.183	−1.908
0.999		−7.415	−5.379	−3.671	−2.469	−2.071
0.9999		−8.828	−6.352	−4.256	−2.752	−2.232
0.99999		−10.239	−7.325	−4.841	−3.036	−2.394

4.4. A Note on Zero Modes

In the context of our numerical analysis we have verified the existence of the two zero modes mentioned in Section 3. With the current techniques an effortless way to do so is to numerically determine $\alpha$ in $\nu \left(t\right)\approx \alpha ln(t-m)$ for $t\searrow m$ since the Jost function has zeros at the imaginary momenta associated with the bound state energies. In almost all cases the numerical fit indeed produced results consistent with $\alpha =2$. The only exceptions were observed in cases with the soliton being in secondary vacua with $\varphi \ne 0$ for large regions of space. In those cases the fit yielded $\alpha \approx 3$. We then employed techniques as in section III of Ref. [33] and found that the third (would-be) zero mode was dynamical: it emerged from an ordinary bound state with a non-zero energy eigenvalue in the limit $a\nearrow 1$. When the secondary vacuum does not include $\varphi =0$, the profile has distinct plateaus along the negative and positive half-lines. Moving around those plateaus produces two independent zero modes in addition to the translational one.

5. Conclusions

We have investigated a number of BPS solitons in one space dimension. The models under consideration have several distinct translationally invariant zero energy solutions, at least for certain ranges of model parameters. We refer to these solutions as primary and secondary vacua. At negative spatial infinity topologically stable solitons approach a primary vacuum but its negative at the opposite end. Yet, the soliton may close in on a secondary vacuum in an arbitrarily large portion of space without any classical energy cost so that there are infinitely many classically degenerate solutions. We must then include the quantum corrections to identify the energetically favored solution. For this purpose we have computed the leading, one-loop quantum correction which is the vacuum polarization energy (VPE) of such solitons.

The sample models considered here have two scalar fields $\varphi \left(x\right)$ and $\chi \left(x\right)$ with the corresponding static soliton profiles being respectively odd and even under spatial reflection. This guarantees topological stability and selects the primary vacua as those with $\chi \equiv 0$. On the other hand the secondary vacua have $\chi \equiv {\chi }_s\ne 0$. The value of ${\varphi }_s$ in secondary vacua as well as other peculiarities of the secondary vacua depend on the model parameters. Further conditions on the availablility of these vacua arise from requiring the existence of localized static solutions.

We have introduced the variational parameter $a={\displaystyle \frac{\chi \left(0\right)}{{\chi }_s}}$ as the measure of how the spatially symmetric component of the soliton approaches its secondary vacuum, and have found that the classical energy is independent of a by the BPS construction. On the other hand the VPE decreases like $E_{\mathrm{VPE}}\sim E_0-E_{1}ln(1-a)$ with $E_1<0$ as $a\nearrow 1$ and hence has no lower bound. In the same limit the soliton dwells in a secondary vacuum for an increasing and unbound region. Though $E_0$ and $E_1$ are model dependent, this functional behavior has been reproduced in all of the considered models. Hence our computations corroborate the earlier conjecture [22] that quantum corrections destabilize classically degenerate BPS solitons when they may approach secondary vacua in an arbitrarily large portion of space.

Eventually soliton solutions with constant $\chi \left(x\right)\equiv {\chi }_s$ and $\varphi \left(x\right)\ne 0$ exist when ${\varphi }_s\ne 0$. They connect ${\varphi }_s$ and $-{\varphi }_s$ along the coordinate axis. These borderline cases have different classical energies when ${\varphi }_s$ is not a primary vacuum. Since these solutions are merely variants of the ordinary kink we have not considered them here.

Of course, when the first order correction is sizable, higher orders may be as relevant. Studies on higher order quantum corrections for solitons have just recently commenced [37].