(Higgs) vacuum decay during inflation

We develop the formalism for computing gravitational corrections to vacuum decay from de Sitter space as a sub-Planckian perturbative expansion. Non-minimal coupling to gravity can be encoded in an effective potential. The Coleman bounce continuously deforms into the Hawking-Moss bounce, until they coincide for a critical value of the Hubble constant. As an application, we reconsider the decay of the electroweak Higgs vacuum during inflation. Our vacuum decay computation reproduces and improves bounds on the maximal inflationary Hubble scale previously computed through statistical techniques.


Introduction
A false vacuum can decay through quantum tunnelling that leads to nucleation of regions of true vacuum. The rate of this non-perturbative phenomenon is exponentially suppressed by the action of the 'bounce', the field configuration that dominates the transition [1].
Coleman and de Luccia showed how to account for gravitational effects [2]. Their formalism can be simplified by restricting to sub-Planckian energies, which are the only ones for which Einstein gravity can be trusted. Simplified expressions were obtained in [3,4] for the decay of flat space-time.
We extend here the simplified formalism to tunnelling from de Sitter space (positive energy density), which is relevant during inflation with Hubble constant H. It is known that gravitational effects can dramatically enhance the tunnelling rate. The qualitative intuition is that a de Sitter space has a Gibbons-Hawking 'temperature' T = H/2π [5] that gives extra 'thermal' fluctuations that facilitate tunnelling. Equivalently, light scalar fields h undergo fluctuations δh ∼ H/2π per e-folding.
We show that tunnelling from de Sitter can be described by a simplified formalism assuming that H and the bounce energy density are sub-Planckian. We also show how to include perturbatively the small extra Planck-suppressed corrections due to gravity.
Vacuum decay in the presence of gravity receives an extra contribution from another bounce, known as the Hawking-Moss (HM) solution: a constant field configuration that sits at the top of the potential barrier [6]. Being constant, it has the higher O(5) symmetry of 4-dimensional de Sitter space, while the Coleman-de Luccia (CdL) bounce is only O(4) symmetric. The Hawking-Moss contribution to vacuum decay vanishes for flat space, which corresponds to H = 0. We show that the Coleman bounce continuously deforms into the Hawking-Moss bounce, and the two become equal at a critical value of H, usually equal to 1/2 of the curvature of the potential at its maximum.
Furthermore, the simplified formalism allows to easily include perturbatively the effect of a general non-minimal scalar coupling to gravity, as a modification of the effective scalar potential.
The above features are relevant for the possible destabilization of the Standard Model (SM) vacuum during inflation. The Higgs field can fluctuate towards values a few orders of magnitude below the Planck scale, for which its potential can be deeper than for the electroweak vacuum [7][8][9][10][11][12][13][14][15]. If vacuum decay happens during inflation, the regions of true vacuum expand and engulf the whole space [2,11,16]. This catastrophic scenario is avoided if H is small enough that vacuum decay is negligibly slow. The derivation of a precise bound on the scale of inflation has been based mainly on a stochastic approach, relying on the numerical solution of Fokker-Planck or Langevin equations that describe the real-time evolution of fluctuations in the scalar field. We pursue here the alternative approach of computing the Euclidean tunnelling rate. We reproduce some previous results and correct others.
The paper is structured as follows. In section 2 we derive a simple approximation for sub-Planckian vacuum decay. In section 3 we validate the analytical expressions by focusing on a toy renormalizable scalar potential, and show how the Coleman bounce connects to the Hawking-Moss bounce. In the final section 4 we obtain bounds on the scale of inflation H by computing the tunnelling rate, dominated by the Hawking-Moss bounce. Conclusions are given in section 5. decay is exponentially suppressed by the action of a 'bounce' configuration, like in flat space. 1 We consider the Euclidean action of a scalar field h(x) in the presence of gravity, is the Newton constant, withM Pl ≈ 2.43 × 10 18 GeV. For the time being V and f are generic functions of the scalar field h. The action in eq. (1) is the most general action for the metric g µν and h up to two-derivative terms: an extra generic function Z(h) multiplying the kinetic term of the scalar field can be removed by redefining h. The classical equations of motion for gravity and for h are [17] where ∇ 2 = ∇ µ ∇ µ . The use of these equations allows us to simplify the action. Taking the trace of eq. (2) one finds Substitution in eq. (1) gives The second term in the above expression is reduced to a boundary term upon integration.
For the problem at hand this term vanishes and one obtains We are interested in the possible decay of the false vacuum during a period in which the vacuum energy is dominated by a cosmological constant V 0 . We assume that V (h) has two minima, a false vacuum at h = h false and the true vacuum at h = h true , with h true > h false . In the following we will set h false = 0 without loss of generality. The two minima are separated by a maximum of the potential. We identify V 0 = V (0) and split the potential as 1 The proof valid in flat space cannot be extended to de Sitter space because the Hamiltonian is not well defined. One cannot isolate the ground state by computing a transition amplitude in the limit of infinite time, because Euclidean de Sitter has finite volume, so that multi-bounce configurations cannot be resummed in a dilute gas approximation.
such that δV (0) = 0. The vacuum energy density V 0 induces a de Sitter space with curvature R = 12H 2 , where the Hubble rate H is given by (we assume without loss of generality f (0) = 0: a non-vanishing value of f (0) can be absorbed in a redefinition of κ). In the following we will collectively denote with Φ false the field configuration with this de Sitter background and h = 0. In the semiclassical (small h) limit the decay rate Γ of the false vacuum per unit of space-time volume V is given by [1,2,18] dΓ where A is a quantity of order M 4 , where M is the mass scale in the potential. The dominant effect is the bounce action S. It is given by where Φ B is an unstable 'bounce' solution of the Euclidean equations of motion, such that S is finite and there is no other configuration with the same properties and lower S. In the rest of the paper we set the units such thath = 1. In order to find Φ B we follow [2] and introduce an O(4)-symmetric Euclidean ansatz for the Higgs field h(r) and for the geometry where dΩ is the volume element of the unit 3-sphere. On this background, the action becomes where the curvature is and a prime denotes d/dr. The simplified action of eq. (6) becomes: The equations of motion are Let us discuss the boundary conditions. Since in the false vacuum the space is a 4-sphere and topology cannot be changed dynamically, the space described by ρ will have the same topology; thus ρ will have two zeros. One can be conventionally chosen to occur at r = 0, and the other one at some value of r that we call r max , The whole space is covered by the coordinate interval [0, r max ]. In the de Sitter case one has r max = π/H. The equation of motion of h in (15) and the regularity of h at r = 0 and r = r max imply In the limit of small H (i.e. large r max ), the boundary condition h (r max ) = 0 implies h(∞) = 0 in view of the large volume outside the core of the bounce. Generically, in a non-trivial (r-dependent) bounce h(r) does not tend to the false vacuum solution, h false = 0, as r → r max , unless we are in the flat space case, r max → ∞. 2

The Hawking-Moss bounce
The Hawking-Moss configuration [6], which we denote with Φ HM , is a simple unstable finite-action solution satisfying the equations of motion and boundary conditions above.
In this configuration the scalar sits at the constant value h = h max that maximizes 3 where H(h) is the Hubble constant given by .
The Hawking-Moss solution exists whenever V H has a maximum. When f = 0, h max coincides with the maximum of the potential. We can compute the tunnelling rate by using the simplified action in eq. (14), obtaining for the Hawking-Moss solution 2 This can be shown whenever h and ρ are regular functions at r = r max : by Taylor-expanding the equations of motion eq.s (15)-(16) around r = r max , using h(r) = ∞ n=1 c n (r − r rmax ) n and ρ(r) = ∞ n=1 a n (r − r max ) n : one obtains a set of algebraic equations that force c n = 0. Namely, for r max < ∞, the only regular function that goes indefinitely close to the false vacuum solution as r → r max is the false vacuum solution itself. 3 The Coleman bounce is O(4)-symmetric. The Hawking-Moss bounce, having a constant h, has the full O(5) symmetry of de Sitter space. Vacuum decay at finite-temperature T is described by a configuration with period 1/T in the Euclidean time coordinate. At large T , the thermal bounce becomes constant in time, acquiring a O(3) ⊗ O(2) symmetry (see [4] for a recent discussion). These are different solutions: a de Sitter space with Hubble constant H is qualitatively similar but not fully equivalent to a thermal bath at temperature T = H/2π.
V 0 and at leading order in κ this formula simplifies to where H can be evaluated at h = 0. We shall examine the role of the Hawking-Moss solution for vacuum decay, finding that it is relevant for large values of H.
Generically, there are also non-trivial solutions with a non-constant Higgs profile h(r), which, in the flat-space limit, reduce to the Coleman bounce [1]. In order to determine the various bounces, one must solve the coupled eq.s (15) and (16) with the boundary conditions described above.

Sub-Planckian approximation to the bounce
The problem can be simplified by using the low-energy approximation, which, as explained at the beginning of this section, is not physically restrictive if one works within the regime of validity of Einstein gravity (as we do). We illustrate now such an approximation.
The low-energy approximation consists in assuming that gravity is weak in the sense that H, where R is the size of the bounce (1/R is roughly given by the mass scale that appears in the scalar potential V ). The two conditions arise because gravitational corrections are suppressed by powers of the Planck mass, and are thereby small if the massive parameters of the problem are small in Planck units. During inflation, the condition on H is satisfied in view of the experimental constraint H < 3.6 × 10 −5M Pl (see sec 5.1 of [19]). The first condition is also not restrictive because it is necessary to avoid energies of order of the Planck scale, for which Einstein's theory breaks down.
Assuming that these conditions are satisfied, we expand h and ρ in powers of κ = 1/M 2 Pl : The leading-order metric corresponds to de Sitter space: Furthermore, we are interested in a situation in which H ∼ 1/R: otherwise one can neglect H and return to the flat space approximation discussed in [4,11]. Thus we are in a regime in which the vacuum energy is dominated by V 0 = 3H 2M 2 Pl δV (h) and the gravitational background is perturbed only slightly by the bounce h(r).
The equation of motion of the zeroth order bounce h 0 (r) (that is the equation on the de Sitter non-dynamical background) and the first correction ρ 1 to the metric function can be obtained by inserting the expansion of eq. (24) in eq.s (15) and (16). The de Sitter bounce h 0 (r) at zeroth order in κ is given by where V H is given in eq. (19), where H can be evaluated at h = 0 rather than at h max : since the difference is an higher order effect in κ, we avoid introducing two different symbols. 4 The boundary conditions are At this lowest order, the effect of a general non-minimal coupling to gravity f (h) is equivalent to replacing the potential V (h) with the modified potential V H (h) given in eq. (19). The equation for ρ 1 is such that ρ 1 (r) can be obtained by solving either by integration starting from ρ 1 (0) = 0 (although some care is needed to handle apparent singularities at rH = π/2), or by converting eq. (29) into a 1st-order linear differential equation that can be solved numerically.
In the limit where the bounce has a size R much smaller than 1/H, the solution reduces to the flat-space solution of [4], times the overall cos(Hr) factor.
Our goal now is to compute the action (difference) S of eq. (10) because, which is the quantity that appears in the decay rate. The expansion for the fields in (24) leads to a corresponding expansion of S in powers of κ: (31) 4 As an aside comment, an O(4)-symmetric space is conformally flat, such that by performing a Weyl transformation one can revert to flat-space equations with a Weyl-transformed action. A de Sitter space is conformally flat when written in terms of conformal timer ≡ 2 tan(Hr/2)/H. Performing the associated Weyl transformation h 0 (r) =h 0 (r)/ cos 2 (Hr/2), the bounce equation (26) becomes whereṼ (n) is the n-th derivative ofṼ .
The zeroth order action is 5 The leading correction due to gravity, ∆S gravity ≡ κS 1 , is The expression of ∆S gravity above has been simplified by using the equation of h 0 in (26) and by an integration by parts. It can be further simplified as follows. Rescaling ρ 1 (r) → sρ 1 (r) corresponds to shifting ρ 1 (r) by (s − 1)ρ 1 (r). By noticing that (s − 1)ρ 1 (r) is a particular variation δρ 1 we conclude that the action must have an extremum at s = 1.
Applying this argument to eq. (33) relates the integrals of terms linear and quadratic in ρ 1 . The final simplified expression is: Note that the upper integration limit is simply π/H. In deriving it we have taken into account the dynamics of the spacetime volume: the shift in r max does not affect the integral because the integrand contains a function, sin Hr, which vanishes at the integration boundaries. 6 In the limit H → 0, eq. (34) reduces to the flat-space expression found in [4], which is positive-definite, unlike the result for generic H. Just like on flat space, ∆S gravity is independent of h 1 on-shell: the reason is that the only way h 1 could appear at first-order in κ is by taking the first variation of the h-dependent part of the action, eq. (12), but this vanishes when h 0 solves eq. (26).
to compute the bounce h 0 on the background de Sitter space. This is easier than solving the coupled equations for the bounce and the geometry in eq.s (15) and (16). Being a one-dimensional problem, it can be solved through an over-shooting/under-shooting method. Then, one needs to plug h 0 in the expression for ρ 1 to get S 0 + ∆S gravity . One can therefore focus on the equation of h 0 . Imposing the boundary conditions in eq. (28) leads to well-defined solutions, as we will show in the next sections.

Renormalizable potential
In order to understand the influence of the de Sitter background on vacuum decay, we perform a numerical study of the problem for a toy renormalizable potential with M 2 = λh max h true and A = λ(h max + h true ), such that the potential has a maximum at h = h max and two vacua at h = 0 and at h = h true : the latter vacuum is the true deeper vacuum provided that h true > 2h max > 0. Quantum corrections are perturbatively small when λ 4π and A 4πM . The curvature of the potential at its maximum is The constant term V 0 gives a Hubble constant H through eq. (8).

Zeroth order in H, M M Pl
The main qualitative influence of the Hubble rate H on vacuum decay is most easily understood at zeroth order in the sub-Planckian expansion, ignoring the gravitational corrections that will be discussed in the next section. We consider a typical illustrative example: vanishing non-minimal coupling to gravity (introduced later), λ = 0.6 and h true = 3h max . In fig. 1 we show the resulting bounces h 0 (t) at zeroth order in H, M M Pl for increasing values of H. For H M the de Sitter radius 1/H is much larger than the scale of the flatspace bounce, of order 1/M . Thereby, the flat space bounce is negligibly affected by the curvature of the space, fitting comfortably into a horizon.
We see that the critical value above which H starts influencing the bounce action is of order M . Thereby the bounce correction to the energy density is of order M 4 , which is negligible with respect to V 0 = 3M 2 Pl H 2 . This confirms that, in the relevant range, the bounce correction to the background is negligible, being Planck suppressed, so that it makes sense to first consider the zeroth-order approximation. Fig. 1a   order M . 7 The critical value of H can be analytically computed by approximating the potential as a quadratic Taylor series in h around its maximum:

such that the bounce equation at lowest order in κ becomes
This linear equation is solved by The thin-wall approximation approximates the bounce as two different constants, at r < R and r > R. In cases where the thin-wall approximation holds in flat space at H M , it ceases to be valid as H is increased. Thereby the continuous transition from the Coleman bounce to the Hawking-Moss bounce is not visible in the thin-wall approximation [15,20]. We emphasize that the Hawking-Moss bounce is not an approximation to the Coleman bounce: they are two different solutions. is the order of the Legendre function P 1 n ; the other independent solution is not regular in r = 0. The solution diverges at π/H unless n is integer. For n = 1 one gets the constant Hawking-Moss solution. The first non constant solution, h 0 (r) − h max ∝ cos(Hr), arises for n = 2, corresponding to the critical value For values of H close to H cr , by expanding the potential to higher orders around its maximum, one finds that Coleman bounces must satisfy and their action is S Coleman S HM + 2π 2 (h 0 (0) − h max ) 2 ∆/15H 2 [21]. The sign of ∆ is fixed by the potential, so that Coleman bounces exist for H < H cr when ∆ < 0, and for H > H cr otherwise. 8 Our potential has V (4) > 0 and thereby ∆ < 0, so that Coleman bounces exist only for H < H cr .
Higher values of n ≥ 3 correspond to bounces that cross the top of the potential n − 1 times and exist for H ≤ −V (2) (h max )/(n 2 + n − 2). They never dominate the pathintegral, as their action is between the Coleman action and the Hawking-Moss action, as shown in fig. 2. For H −V (2) (h max ) their actions, S n , are multiple integers of the Coleman action, allowing the resummation of their contributions in the dilute-gas approximation [18]. As H grows, multi-bounce solutions progressively no longer fit into the Euclidean de Sitter space. Fig. 1b shows the bounce actions. In order to compute them, including gravitational corrections, we need to fix the overall mass scale of the potential. We choose a mildly sub-Planckian value of the field value of the top of the potential, h max = 0.25M Pl , in order to have mild Planck-suppressed corrections.

First order in H, M M Pl
The Hawking-Moss bounce exists whenever the potential has a barrier, and its action can be easily computed exactly. When the Hubble constant is much smaller than the inverse size of the bounce, the Hawking-Moss bounce becomes negligible because its action (plotted in blue) becomes large.
The Coleman bounce only exists for sub-critical values of H, and its action (plotted in red) smoothly merges with the Hawking-Moss action for H = H cr . We plotted 3 different results for its action: 1. The continuous curve is the full numerical result S.
2. The dashed curve is S 0 , the action at zeroth order in κ = 1/M 2 Pl . We see that it already provides a reasonably accurate approximation.
3. The dotted curve is the first-order approximation S 0 + κS 1 , and it almost coincides with the exact numerical curve.

Effect of non-minimal couplings
Finally, the effect of a non-minimal coupling to gravity f (h) can be trivially discussed at zeroth order in the sub-Planckian limit, being just equivalent to a shift in the scalar potential V → V H = V − 6H 2 f , see eq. (26). This effect is not present in flat space, where the Hubble constant vanishes, H = 0. For example a non-minimal coupling to gravity f (h) = ξh 2 , governed by a dimensionless coupling ξ, is equivalent to a shift M 2 → M 2 H ≡ M 2 − 12ξH 2 in our renormalizable quartic potential of eq. (36). This is just a redefinition of the potential parameters which makes the qualitative implications obvious, in agreement with the full numerical result shown in fig. 3: H < M 2 and thereby the potential barrier, decreasing the actions and increasing the tunnelling rate (see also [15]). The critical value H cr depends on ξ, so that by increasing ξ one first violates the condition H < H cr , leading to the disappearance of Coleman bounces. A larger ξ leads to M 2  fig. 1. Its main effect is to modify the effective potential, so that the true vacuum disappears for negative large ξ, and the potential barrier disappears for positive large ξ. Gravitational corrections to the action are again well approximated by our sub-Planckian expansion.
that the potential barrier disappears and the false vacuum is classically destabilised: this corresponds to S HM = 0 in fig. 3.
• A negative ξ has the effect of increasing the potential barrier. Ultimately, a too large negative ξ destabilizes the true vacuum: at this point V (h true ) = V (h max ), such that the Coleman bounce becomes equal to the Hawking-Moss bounce.
In fig. 3 we also depict the full numerical action assuming a mildly sub-Planckian potential with h max = 0.25M Pl : our sub-Planckian expansion again reproduces the full numerical result. The above simplicity is lost if Planckian energies are involved; however in such a case Einstein gravity cannot be trusted.

Standard Model vacuum decay during inflation
Finally, we apply our general formalism to the case of physical interest: instability of the electro-weak SM vacuum during inflation.
The probability per unit time and volume of vacuum decay during inflation can be estimated on dimensional grounds as d℘/dV dt ∼ H 4 exp(−S), where S is the action of the relevant bounce configuration. The total probability of vacuum decay during inflation then is ℘ ∼ T L 3 H 4 exp(−S), corresponding to a total time T ∼ N/H and volume L 3 ∼ H −3 exp(3N ), such that ℘ ∼ exp(3N − S). Therefore, a small 'probability' ℘ ∼ 1 of vacuum tunnelling during inflation needs a bounce action S > ∼ 3N . 9 The horizon of the visible universe corresponds to a minimal number of N ∼ 60 e-foldings of inflation.
The computation of the bounce actions S in the SM case needs to take into account the peculiar features of the SM Higgs potential, which is nearly scale-invariant and can be approximated as where the running Higgs quartic can turn negative, λ(h) < 0, at large field values. This happens for the present best-fit values of M t , M h and α 3 , that lead to h cr = 5 × 10 10 GeV [11,24,25]. The β-function of λ around h cr can be approximated as b ≈ 0.15/(4π) 2 .
Furthermore, we add a nonminimal coupling of the Higgs field to gravity f (h) = ξ H h 2 , such that the effective potential of eq. (19) relevant in the sub-Planckian limit is Finally, we assume that inflation can be approximated as an extra constant term V 0 in the potential. A possible extra quartic scalar coupling of the inflaton to the Higgs would manifest itself as an extra contribution to the effective Higgs mass term in eq. (42), which is equivalent to a modified effective ξ H .

SM vacuum decay for small H
In the limit of small H one can view curvature, gravity and quantum effects as perturbative corrections to the simple approximation of a constant λ < 0. Perturbing around a potential with no barrier and no true vacuum requires a careful understanding [26]. Kinetic energy acts as a barrier, such that the dimension-less potential admits a continuous family of flat-space bounces, parameterized by their arbitrary scale R: The action of these 'Fubini' bounces is S = 8π 2 /3|λ| [3]. Minimal gravitational couplings have been included numerically in [27,28]; in this section we will apply our analytic sub-Planckian approximation to take into account gravity (including non-minimal couplings).
Quantum corrections can be included roughly by renormalizing the quartic coupling at the scale of the bounce, S ≈ 8π 2 /3|λ(1/R)| [26]. For the best-fit values of the SM parameters, the Higgs quartic λ runs in such a way that tunnelling is dominated by mildly sub-Planckian bounces, such that Planck-suppressed corrections are small in flat space [3,4].
We now include curvature and gravitational effects, assuming H 1/R. Performing the integral in eq. (30) we obtain the leading correction in small HR to the metric: The gravitational corrections to the action combine with the quantum corrections (see also [10]) in order to give the final formula valid for H 1/R M Pl : This expression only holds when the corrections are small. In this regime, the vacuum decay rate during inflation is negligible, having a rate similar to the rate in the longer post-inflationary phase.

SM vacuum decay for large H h cr
The interesting case that can lead to possibly significant inflationary enhancements of the tunnelling rate corresponds to values of H comparable or larger than the inverse size 1/R of the bounce, so that the approximation used in the previous section 4.1 does not apply. For simplicity, we start by discussing the opposite limit, in which the Hubble constant H during inflation is sub-Planckian and much larger than the critical scale h cr above which the Higgs quartic coupling turns negative. Then, we can approximate the SM potential at field values around h ∼ H as a quartic potential, with a constant negative λ renormalized around H. Adding the non-minimal coupling to gravity f (h) = ξ H h 2 gives the effective potential relevant in the sub-Planckian limit: Scale invariance is broken by the de Sitter background with Hubble constant H, so that the bounce action can only depend on the dimensionless parameters ξ H and λ. By performing the field redefinition h(r) → αh(r), where α is a constant, one obtains S(ξ H , λ) = α 2 S(ξ H , α 2 λ) which implies S ∝ 1/λ. Therefore, we only need to compute S as function of ξ H . A potential barrier exists for ξ H < 0: then h max = H 12ξ H /λ and Hawking-Moss bounces have action S HM = −96π 2 ξ 2 H /λ.
According to the argument in section 3.1, the critical value of H that controls the existence of Coleman bounces is H cr = −V (2) (h max )/2. For the potential of eq. (46) this means H/H cr = 1/ √ −6ξ H , so that H = H cr for ξ H = −1/6. As discussed in section 3.1, Coleman bounces exist for H < H cr or H > H cr depending on the sign of the higherorder coefficient ∆ defined in eq. (40). In the present case ∆ ∝ −λ(1 + 6ξ H ), with a positive proportionality constant. This potential behaves in an unusual way: ∆ vanishes at the critical value ξ H = −1/6, for which Hawking-Moss bounces have the same action S = −8π 2 /3λ as flat-space Fubini bounces. Flat-space bounces are relevant because the action is Weyl invariant for ξ H = −1/6, such that de Sitter space is conformally equivalent to flat space. Indeed, the Weyl-transformed eq. (27) reduces toh 0 +3h 0 /r = λh 3 0 , satisfied by Fubini bouncesh 0 = 2/|λ|2R/(R 2 +r 2 ), where R is an arbitrary constant. By Weylrescaling them back to the original field h 0 and coordinate r we obtain the Coleman bounce for ξ H = −1/6, and thereby H = H cr : Eq. (47) together with de Sitter space actually solve the full gravitational equations (not only those in the sub-Planckian limit), as can be explicitly verified or understood from the argument given in flat space in footnote 6 of [4]. In conclusion, vacuum decay is safely slow if S HM > 3N which implies the condition This bound can be compared with the bound H/h max < ∼ 0.045 derived in [11] by solving the Fokker-Planck or Langevin equation that describes the evolution in real time of the inflationary quantum fluctuations of the Higgs field. There is numerical agreement, even though the parametric dependence in eq. (50) does not match the one in [11]. Indeed [11] found that the Higgs acquires a Gaussian distribution with variance that grows with the number N of e-foldings as h 2 = H √ N /2π, without approaching a limiting distribution. Thereby the dedicated study of [11] was necessary and cannot be reproduced by the where W (z) is the product-log function defined by z = W e W : it is real for z > −1/e. Otherwise, the potential V H has no potential barrier because M 2 h is too negative: The action of the Hawking-Moss bounce is The conditions that determine the relative role of Coleman and Hawking-Moss bounces around the critical situation H = H cr give rise to a non-trivial pattern, plotted in fig. 5.
The conclusion is again that only relevant vacuum decay bound is S HM > 3N . In the limit H h cr this reduces to eq. (48). For generic values of H the bound is plotted numerically in fig. 5, where the red region is excluded because inflationary vacuum decay is too fast. For ξ H < 0 such bound agrees with the corresponding result of [11]. Indeed [11] found that a positive M 2 h > 0 limits the Higgs fluctuations which, after a few e-foldings, converge towards a limiting distribution, well described by the Hawking-Moss transition. On the other hand, for M 2 h ≤ 0 (ξ H ≥ 0) the Higgs fluctuations grow with N (as √ N for M 2 h = 0, and exponentially for M 2 h < 0), so that the detailed dynamical study of [11] is needed. Nevertheless, for ξ H > 0, the bound S HM > 3N , is almost numerically equivalent to the simpler bound on M 2 h in eq. (52) that guarantees that V H has a potential barrier, which reads Fig. 5 shows that this bound is weaker than the bound of [11]. A Langevin simulation performed along the lines of [11] agrees with our bound, while [11] made a simplifying approximation ('neglecting the small Higgs quartic coupling') which is not accurate around the bound at ξ H > 0.

Conclusions
In section 2 we developed a simplified formalism for computing vacuum decay from a de Sitter space with Hubble constant H, assuming that both H and the mass scale of the scalar potential are sub-Planckian. This is not a limitation, given that otherwise Einstein gravity cannot anyhow be trusted. In this approximation, the bounce action is obtained as a power series in 1/M Pl , and a non-minimal scalar coupling to gravity can be reabsorbed in an effective scalar potential, see eq. (19). In section 3 we considered a renormalizable single-field potential. We verified that our expansion reproduces full numerical result. Furthermore we found that, increasing H, the flat-space Coleman bounce continuously deforms into the Hawking-Moss bounce. Only the Hawking-Moss bounce exists above a critical value of the Hubble constant, equal to H 2 cr = −V (2) (h max )/4. For H < H cr the Coleman bounce appears and dominates vacuum decay, having a smaller action than the Hawking-Moss bounce. For smaller values of H extra bounces that oscillate around the top of the barrier appear, but they never dominate the path-integral. In the flat space limit H → 0 they reduce to the infinite series of multi-bounce solutions.
In section 4 we studied quantum tunnelling of the electroweak vacuum during inflation, assuming that the SM Higgs potential is unstable at large field values, as happens for present central values of the SM parameters. Coleman bounces are still connected to Hawking-Moss bounces, altough the fact that the SM potential has a negative quartic at large field values and is quasi-scale-invariant makes their relation different. We exhibit a limit where they are conformally equivalent. Anyhow we found that only Hawking-Moss bounces imply a significant bound on vacuum decay during inflation. If the minimal coupling of the Higgs to gravity is negative, ξ H < 0, our tunnelling computation confirms previous upper bounds on H obtained from statistical simulations (needed to address other cosmological issues). If ξ H > 0 we find weaker bounds, and explain why the approximation made in earlier works [11] is not accurate.