Emergent spontaneous symmetry breaking and emergent symmetry restoration in rippling gravitational background

We study effects of a rippling gravitational background on a scalar field with a double well potential, focusing on the analogy with the well known dynamics of the Kapitza’s pendulum. The ripples are rendered as infinitesimal but rapidly oscillating perturbations of the scale factor. We find that the resulting dynamics crucially depends on a value of the parameter ξ\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$\xi $$\end{document} in the ξRϕ2\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$\xi \,R\, \phi ^2$$\end{document} vertex. For the time-dependent perturbations of a proper form the resulting effective action is generally covariant, and at a high enough frequency at ξ<0\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$\xi <0$$\end{document} and at ξ>1/6\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$\xi >1/6$$\end{document} the effective potential has a single minimum at zero, thereby restoring spontaneously broken symmetry of the ground state. On the other side, at 0<ξ<1/6\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$0<\xi < 1/6$$\end{document} spontaneous symmetry breaking emerges even when it is absent in the unperturbed case.


Introduction
Oscillating gravitational backgrounds attract attention of theoretical physicists in various contexts starting from quantum decoherence [1,2] and finishing some cosmological [3] and extra dimensional constructions [4][5][6]. Effects of a rippling scale factor on a minimally coupled quantized scalar field were studied in [7]. One can also find some interesting consequences of rippling parameters in [8,9]. The first famous example of a rippling background, however, is not related to quantum physics or cosmology -it is the famous Kapitza's pendulum [10,11], i.e. a classical pendulum whose suspension point rapidly oscillates with a small amplitude. The highly nontrivial and counterintuitive classical dynamics of this simple object inspired us to write this article. As we show below already at classical level small but rapidly oscillating perturbations of the scale factor may affect the ground states of physically relevant models in a quite interesting way.
In this paper we study the effect of the rapidly oscillating gravitational field g μν on a classical dynamics of the scalar a e-mail: max.kurkov@gmail.com field φ. The latter is described by the most general action 1 which leads to renormalizable 2 quantum field theory in four dimensions, which is invariant upon the reflection φ −→ −φ. Such an action is of special importance, since the Higgs field of the Standard Model is described by the action of such a form. We consider the metric tensor given by the product of the slowly varying bare 3 metricḡ μν and the highly oscillating conformal factor, which is very close to one: g μν =ḡ μν e 2α cos (ωt) , where the dimensionless amplitude α is much smaller than 1, the frequency ω is much larger than μ and invariants of the metric tensorḡ μν (and its derivatives) of the dimension [length −1 ]. The main goal of the present paper is to generalize the result of Kapitza to this model. In particular, we show that solutions of the equation of motion, which comes out from the action (1), split into two parts where δφ is a rapidly oscillating and small correction, which approaches to zero as ω −1 in the high frequency limit, while the dynamics of the slowly varying fieldφ is described by the classical action, which we establish. Surely due to a manifest frame dependence of the perturbation law (2), the effective action generally speaking depends on the choice of the coordinates, which are used to perturb the bare metric tensorḡ μν . The most interesting result is related to the situation, when the oscillating metric takes the simple form (2) in the comoving frame. 4 In such a case the effective action has exactly the same structure (1), where the quantities g μν and φ are replaced correspondingly byḡ μν andφ, therefore it is generally covariant, and the only effect of the oscillations is an additive renormalization of the mass parameter μ 2 . A sign of the correction μ 2 ≡ μ 2 eff − μ 2 nontrivially depends on a choice of the coupling constant ξ , and this is probably the most interesting result of the paper.
We find that at ξ < 0 and at ξ > 1/6 the correction μ 2 is always negative, and at the high enough frequency ω it can easily compensate the bare mass parameter, what quite naturally implies that the effect of the rapid oscillations is similar to an increase in temperature: the effective potential (in contrast to the original one) has just a single minimum at φ = 0, and spontaneous symmetry breaking of the bare theory vanishes. All particles which obtain their mass due to the Higgs mechanism become massless.
In the another regime 0 < ξ < 1/6 the situation changes qualitatively. The correction μ 2 ≡ μ 2 eff − μ 2 becomes positive, and even when the mass parameter is absent in the bare theory, 5 it appears in the effective one. Such an effect can be regarded as some sort of emergent spontaneous symmetry breaking. At ξ = 1/6 (naturally) and ξ = 0 (less naturally) the effect is absent.
An influence of time dependent (but not oscillating) gravitational backgrounds on the vacuum state of a scalar field was studied in the context of inflation in [12], and the result crucially depends on the non minimal coupling ξ as well, in particular at ξ = 1/6 the influence is minimal. Nevertheless, the effects discussed in [12] and here are different, since in contrast to our setup in the framework of [12] at ξ = 0 the vacuum expectation value grows up exponentially with time.
This paper is organized as follows. In Sect. 2 we briefly describe relevant aspects of the dynamics of the Kapitza's pendulum in order to apply the same technique in the forthcoming discussion. In Sect. 3 we derive the effective action (1) and establish the renormalized mass parameter μ 2 eff . Section 4 is devoted to numerical illustrations of the results obtained for the flat bare metricḡ μν .

Kapitza's pendulum: a brief technical review
The mathematical pendulum is described by the following equation of motion where f (t) is the angular coordinate (we consider the length to be equal to one), and g > 0 is the free-fall acceleration; hereafter the dot stands for differentiation with respect to time. The only stable equilibrium position is located at f = 0, but the situation changes dramatically, when the pivot vibrates with the high frequency ω. In such a case the equation of motion reads where the constant α stands for the amplitude of the oscillations of the suspension, and it is supposed to be small. The most amazing fact is the appearance of a new stable equilibrium point in the inverted position i.e. at f = π . More precisely the solution of the equation of motion is given by a sum of the two functionsf (t) and δ f (t), where the former satisfies some "effective" equation of motion, which in particular exhibits slow oscillations in the vicinity of f = π , when the frequency ω is high enough. The latter is a rapidly oscillating correction of the order 6 of O(ω −1 ). It is remarkable that one can relatively easily give a precise mathematical description of such a nontrivial and unexpected phenomenon. Below we present a derivation of this well known result in the form which is the most suitable and clear for the forthcoming analysis of the scalar field in a rapidly oscillating gravitational background.
Step 1. Proper ansatz A numerical analysis of the Eq. (6) hints us, that its solution splits into the slowly varying partf (t) and the rapidly oscillating but small correction δ f . It is natural to expect that the correction δ f oscillates with the same frequency ω, therefore let us look for the solution in a form of an asymptotic expansion in inverse powers of ω where the (yet undetermined) functions A(t) and B(t) vary slowly. 7 Substituting the ansatz (7) and α = γ · ω −1 in the equation of motion (6) we obtain at the leading order at large ω: what defines A(t) = 0 and B(t) = γ sin(f ). From this moment on the ansatz (7) contains just one undetermined functionf .
Step 2. Averaging over rapid oscillations Substituting A(t) = 0 and B(t) = γ sin(f ) in the next to the leading order of our asymptotic expansion (8) we immediately arrive to the equation which determinesf (t).
Now let us average the function F(t) over the period of rapid oscillations 2π ω : Since by our assumption the quantityf and its derivative vary slowly during the period of rapid oscillations, one can easily compute the integral (10) in the limit ω → ∞, and the answer reads: The Eq. (11) is autonomous and it does not contain large parameters anymore, thereforef is indeed slowly varying function, 8 what justifies all our assumptions. Small deviations off from zero satisfy the standard pendulum Eq. (5) where g is replaced by g eff thus in the vicinity of this equilibrium point one has an additive (finite) renormalization of the free fall acceleration constant g. On the other side, and this is even more interesting, small deviations fromf = π satisfy linearized version of Eq. (5) with therefore in this regime the pendulum starts to oscillate near its upper position with the slow frequency ≡ −g + 1 2 α 2 ω 2 ω. Below we consider the system described 8 Unless one chooses large initial velocity.
by the action (1) along similar lines, and we find that it shares some similarities with the Kapitza's pendulum.

Scalar field in oscillating gravitational background
Now we study the effect of the rapid oscillations defined by (2) on the dynamics of the scalar field φ, which obeys the classical equation of motion The gravitational background is considered to be given, and we assume that the back-reaction of the scalar field on its dynamics is negligibly small. We simplify the forthcoming analysis substituting On the one hand, due to the local Weyl invariance of the action (1) at ξ = 1 6 the Eq. (14) rewritten in terms ofφ has simpler dependence on α and ω. On the other hand, we are interested in the evolution of the slowly varying part of φ, which coincides forφ and φ.
In order to carry out the computations it makes sense to rewrite the equation of motion splitting explicitly rapidly and slowly varying quontities whereḡ μν , Y μ ≡ 1 √ −ḡ (∂ νḡ μν √ −ḡ) and Rḡ vary slowly by construction. The function f α absorbs all influence of the rapidly oscillating exponential factor in (2), and it is defined by Below we study the leading asymptotic at large ω and small α keeping α = γ /ω = O(ω −1 ) by analogy with the Kapitza's pendulum.
Step 1. Proper ansatz Inspired by the example discussed in the previous section we look for the solution in a form of the following asymptotic ansatz: where T and W are slowly varying functions of all coordinates. We do not write the tilde overφ, since, as we said above, in the limit of infinitely large ω (and infinitely small α) the quantities φ andφ coincide. Substituting the ansatz (18) in the equation of motion (16) we immediately determine T and W : what implies As in the "canonical" example there is just one undetermined functionφ.
Step 2. Averaging over rapid oscillations Exactly as we did in the previous section, substituting (20) in the next to the leading order of our asymptotic expansion (19) we derive the equation which determinesφ.
Averaging over the period of rapid oscillations (c.f. Eq. (10)) and passing to the limit of large ω we obtain the final effective equation forφ: The structure of Eq. (22) immediately suggests us, which oscillations of the form (2) are the most interesting. Surely we wish to obtain a generally covariant expression by the end of the day, what happens if and only if the simple perturbation equation (2) is written in the frame whereḡ 00 does not depend on coordinates e.g. the comoving frame. We emphasize that we are talking about preferred ways of perturbation of the bare metricḡ μν rather than preferred coordinate systems. Starting from now we assume that the perturbations are "good" in the mentioned above sense, and 9 the coordinates in Eq. (2) are chosen in such a way thatḡ 00 = +1, so we arrive to the manifestly generally covariant equation which holds for an arbitrary coordinate system, 10 and has exactly the same structure as Eq. (14). The effective mass parameter is given by As we announced in the Sect. 1, this quantity can be either positive or negative depending on the ratios between the parameters, what may dramatically affect the spontaneous symmetry breaking. The particular form (24) of the additive renormalization of the mass parameter μ 2 suggests us to consider two different regimes of the non minimal scalar-tensor coupling, defined by the dimensionless coupling constant ξ .
-At ξ < 0 and ξ > 1/6 the correction to the mass parameter is negative, and at . This regime becomes more interesting when the "bare theory" is not spontaneously broken, i.e. at μ 2 = −m 2 < 0. In such a situation at the effective mass parameter μ 2 eff becomes positive in contrast to the bare one μ 2 , what implies emergent spontaneous symmetry breaking. One can easily see, that this effect reaches its maximum at ξ = 1/12.
If for some application one prefers to avoid the mentioned above effects, one has to work with the minimal ξ = 0 or the conformal ξ = 1/6 couplings. Remark We notice that the coordinate x 0 ≡ t must not be necessary the conformal time, but it can be also the comoving time t c . Let us fix the gauge by the following condition g 00 = 1,ḡ 0 j = 0, j = 1, 2, 3, so the square of the infinitesimal four interval reads (c.f. Eq. (2)): where dx 2 ≡ḡ i j dx i dx j , i, j = 1, 2, 3. In other words instead of consideration of the fluctuations of the form (2) we could have considered g 00 =ḡ 00 , g i j =ḡ i j e 2α cos(ω t) , i, j = 1, 2, 3 from the very beginning, 11 what is more natural for Friedmann-Lemaître-Robertson-Walker metric. All the results viz the final effective equation (23), the renormalization of the mass parameter (24) and the conditions (25), (26), which define the phase transitions, remain absolutely the same. Note that in (29) we wrote t instead of t c , since up to a correction of the order of O(ω −1 ) these two quantities (but not their derivatives!) coincide: So far we discussed the ripples along the time direction t ≡ x 0 . One can easily elaborate the oscillations along some spatial direction e.g. z ≡ x 3 in a similar manner. Replacing t by z in the oscillating conformal factor in (2) and repeating all the discussion we arrive to (22), whereḡ 00 is replaced bȳ g 33 . The effective equation becomes generally covariant if and only if the (modified) perturbation law (2) is written in the coordinate system, whereḡ 33 = const, for example in the Gaussian normal coordinates in respect to the hypersurface of constant z. It is worth noting that for such a choice of coordinates in the perturbation law the effect of this "spatial" rippling has the opposite sign with respect to the timedependent rippling introduced in the comoving frame, sincē g 33 = −1 in the Gaussian normal coordinates.
In the next section we illustrate numerically how this mechanism works on a few examples. the parameter ξ , which is responsible for the non minimal tensor-scalar coupling.
Below we solve numerically the exact (14) and the effective (23) equations of motion for various values of the parameters γ and ξ . The slowly varying background metric is chosen to be flatḡ μν = η μν , and the perturbations are taken of the form (29). Since the metric g μν depends just on time, for the sake of simplicity we consider the field φ to be independent on the spatial coordinates, i.e. φ = φ(t). In such a setup the exact and the effective equations correspondingly read: and Let us consider the system which is spontaneously broken 13 at ω = 0. Varying the parameter γ ≡ α · ω above and below its critical value we solve numerically the Eqs. (31), (32); corresponding solutions are presented on Fig. 1. As one would have expected for small negative deviations γ of γ from the critical value γ 0 the effect of rapid oscillations results in a shift of the frequency of slow oscillations and a shift of the (nonzero) equilibrium point. When γ ≥ 0 the solutions with high precision are described by slow oscillations around the symmetric ground state φ = 0, so effectively at the scales of length much higher than ω −1 the system behaves as non spontaneously broken.
On Fig. 4 we illustrate the dependence on the parameter ξ for this situation. At ξ ≤ 0 and ξ ≥ 1/6 the only effect is a change of the frequency of slow oscillations around the symmetric ground state φ = 0, see Fig. 4a and f, in particular at ξ = 0 and ξ = 1/6 at the scales much higher than ω −1 there is no any effect at all, see Fig. 4b and e. Inside the interval 0 < ξ < 1/6 for sufficiently high values of γ one has the phase transition -emergent spontaneous symmetry breaking, see Fig. 4c and d.
In conclusion we present typical solutions of the exact (31) and the effective (32) equations at small scales, which are comparable with ω −1 . On Fig. 5a and b the small scale behavior is presented for various time intervals. One can see that the the exact solution oscillates with the frequency ω, while the difference between the two 15 is indeed of the order of ω −1 ∼ 10 −3 .