{'fraction_non_alphanumeric': 0.034294328245713206, 'fraction_numerical': 0.011243012373594624, 'mean_word_length': 4.00219918316054, 'pattern_counts': {'":': 0, '<': 7, '<?xml version=': 0, '>': 3, 'https://': 0, 'lorem ipsum': 0, 'www.': 0, 'xml': 0}, 'pii_count': 0, 'substrings_counts': 0, 'word_list_counts': {'cursed_substrings.json': 7, 'profanity_word_list.json': 0, 'sexual_word_list.json': 0, 'zh_pornsignals.json': 0}}
Higgs inflation and suppression of axion isocurvature perturbation

We point out that cosmological constraint from the axion isocurvature perturbation is relaxed if the Higgs field obtains a large field value during inflation in the DFSZ axion model. This scenario is consistent with the Higgs inflation model, in which two Higgs doublets have non-minimal couplings and play a role of inflaton.


I. INTRODUCTION
Strong CP problem is one of the remaining mysteries of the standard model (SM). Among solutions to the strong CP problem proposed so far, the axion solution [1] is the most attractive one [2]. In axion models, the global U(1) symmetry, which is called Peccei-Quinn (PQ) symmetry, is spontaneously broken and the resulting pseudo Nambu-Goldstone (NG) boson takes a roll of axion to solve the strong CP problem. However, cosmological effects of the axion are highly non-trivial. If the PQ symmetry is broken after inflation, topological defects are formed and they may be harmful for cosmology. On the other hand, if the PQ symmetry is broken during inflation, the axion obtains quantum fluctuations which result in the cold dark matter (CDM) isocurvature perturbation [3].
In the standard cosmological scenario in which the PQ symmetry is already broken during inflation and the PQ scalar φ is stabilized at the potential minimum |φ| = f a / √ 2, with f a being the PQ scale, the magnitude of the axion isocurvature perturbation is given by where H inf denotes the Hubble scale during inflation and θ i is the initial misalignment angle. The CDM isocurvature perturbation is given by S CDM = r a (2δa/a) with r a being the axion fraction in the present CDM energy density, and is evaluated as The Planck constraint on the uncorrelated CDM isocurvature perturbation reads S CDM < ∼ 1.4 × 10 −6 [4]. For the axion window 10 9 GeV < ∼ f a < ∼ 10 12 GeV, the inflation scale is constrained to be H inf < ∼ 10 7−10 GeV taking account of non-Gaussian fluctuations [5,6]. In particular, if we demand that the axion is a dominant component of CDM, the constraint reads H inf < ∼ 10 7 GeV. It excludes high-scale inflation models unless PQ symmetry is restored after inflation. But in a class of axion models with domain wall number larger than one, such as the DFSZ axion model [7], the formation of axionic domain wall leads to a cosmological disaster.
There are some ways to solve or relax the axion isocurvature problem. For example, the PQ scale during inflation may be much larger than that in the present vacuum. In this case, the isocurvature perturbation is suppressed by the ratio of the PQ scale at present and during inflation [8]: see also [9][10][11][12]. Another way is to make the axion heavy during inflation so that it does not obtain large scale quantum fluctuations due to the stronger QCD [12][13][14][15] or the explicit PQ breaking term [16,17]. The non-minimal kinetic term of the axion may also relax the constraint [18].
In this letter we consider a variant type of the scenario that suppresses the axion isocurvature perturbation. To this end, we consider the DFSZ axion model in which there are two Higgs doublets with PQ charges. If the Higgs bosons have large field values during inflation, the effective PQ scale is much larger than the present vacuum; the angular component of PQ scalar is massive during inflation and does not obtain quantum fluctuations while the massless mode mostly consists of the pseudo scalar Higgs, which later becomes massive and does not lead to observable isocurvature perturbations. Actually, the effect of small mixing between the pseudo scalar Higgs and PQ scalar leads to the axion isocurvature perturbation, which is suppressed by the large field value of Higgs during inflation. a In particular, we will show that it can be consistent with the Higgs inflation scenario [19] in which the Higgs boson takes a roll of inflaton due to the non-minimal coupling to gravity.

II. TOY MODEL ANALYSIS
Before going into the detailed study, we first roughly sketch the basic idea in a toy model. Let us consider the model with two gauge singlet complex scalars φ and S, both have opposite PQ charges. Then we write down the Lagrangian as a A similar idea has been proposed very recently in Ref. [12].
where λ can be taken real and positive without loss of generality, and Here λ φ , λ S and m 2 S are real and positive. η is defined as η ≡ N DW f a with N DW being the domain wall number which is a model dependent integer. In the following, we consider the case λ φS < 2λ for simplicity. For the stability of the potential at large |S| and |φ|, we need A term proportional to φS can be forbidden by a Z 2 symmetry, under which S transforms as S → −S. The vacuum lies at S = 0 and |φ| = η/ √ 2 where the NG mode, axion, is exactly the angular component of φ: However, the role of φ and S are inverted if S has a large field value during inflation. Actually it can be as large as v S ≡ |S| ∼ H inf / √ λ S and S can be the inflaton consistent with Planck observations for λ S ∼ 10 −13 by introducing higher order non-renormalizable terms to make the S potential polynomial [20] or for λ S ∼ O(1) by adding non-minimal couplings to gravity [19] or nonminimal kinetic terms of S [21]. Let us write φ and S as In the vacuum, v φ = η and v S = 0. But they need not coincide with the vacuum values in the early universe. We assume that initially S has a large field value v S .
Then v φ is given by If we introduce a Hubble induced mass term for φ as V ∼ −c 2 H 2 |φ| 2 with c being a constant, it can also stabilize the PQ scalar at around v φ ∼ cH/ λ φ . The massless mode, which we denote by a, mostly consists of the It is mostly the pseudo scalar a S that obtains quantum fluctuations of ∼ H inf /2π. On the other hand, the orthogonal component, mostly consisting of a φ , obtains a mass of Therefore, if this exceeds the Hubble scale during inflation, a φ does not develop quantum fluctuations. This condition is written as But a φ constitutes a small fraction (∼ v φ /v S ) of massless mode a, hence the fluctuation of a φ during inflation is estimated as Thus we obtain the axion isocurvature fluctuation at the QCD phase transition as Compared with the standard scenario with the broken PQ symmetry during inflation, the isocurvature perturbation is suppressed by the factor ∼ f a /v S ≪ 1. Since we do not introduce an explicit PQ breaking, there is always a NG mode, but the massless mode during inflation needs not coincide with that in the present vacuum. The axion at present was massive during inflation, while the massive mode was massless. The CDM isocurvature perturbation then is given by Thus inflation scale as large as H inf ∼ 10 13 GeV may be allowed for v S ∼ 10 18 GeV even if the axion is a dominant component of CDM.
In this class of scenario, S has a large field value initially and hence it begins a coherent oscillation after inflation and must decay into SM particles. Later we will see that S itself can be the inflaton. The oscillation of S potentially causes resonant particle production of axions [22] and may induce the dynamical motion of φ. We denote the frequency of S after the onset of the oscillation as m osc S . First, we consider the axion production due to the oscillation of S. If the condition √ λv S m osc holds, the axion production of the broad resonance type does not occur even just after the onset of the oscillation of S. In such a case, the narrow resonance would harmfully produce axion particles. However, the narrow resonance is ineffective if the decay rate of S is sizable [23]. Second, let us consider the motion of φ caused by the oscillation of S. The potential of φ varies as S oscillates and φ may also oscillate around the origin. In such a case, the nonthermal restoration of the PQ symmetry [24][25][26][27] could occur due to the parametric resonance at the origin because of the self interaction of φ. The parametric resonance at the origin becomes most effective when S decays just after the onset of oscillation of S. In such a case, the condition for the PQ symmetry not to be restored is obtained from the condition that the number of φ oscillation within one Hubble time remains less than ∼ O(10 2 ) until the oscillation amplitude of φ reduces to ∼ f a [27]. This leads to a constraint where n = 1/2 (1) for the matter (radiation) dominated background evolution, where we have assumed the inequality (11) is marginally satisfied: √ λv S ∼ H inf . Next, let us consider the thermal effects on φ. In order for the PQ symmetry not to be restored after inflation due to thermal effects, we need where T max denotes the maximum temperature after inflation and assumed that S is in thermal equilibrium due to interactions with SM particles. Otherwise, the PQ symmetry may be restored after inflation and isocurvature constraint disappears, but there arises a serious domain wall problem. Conditions (11), (15), (16) and (17) are satisfied for reasonable choice of parameters.

III. DFSZ AXION MODEL
Let us move to the DFSZ axion model, two Higgs doublets are introduced [28]. In this model, S 2 in the toy model (3) may be identified with the gauge invariant combination of the Higgs doublets H u H d . The action in the Jordan frame is given by where and L (SM) contains kinetic terms for SM quarks, leptons and gauge bosons and yukawa couplings between quarks/leptons and Higgs bosons and R J is the Ricci scalar. Quantities with subscript J indicate those in the Jordan frame. Here H u is assumed to couple with uptype quarks and H d with down-type quarks and charged leptons. This can be done by assigning the PQ charge, e.g., 1 to the PQ scalar φ, −2 to H u and 2 to righthanded up-type quarks. In this model, the domain wall number N DW is equal to 6. In the present vacuum, the PQ scalar obtains a VEV of |φ| = η/ √ 2 and Higgs bosons have electroweak scale VEVs. Note that since the Higgs bosons also have PQ charges, the axion is a mixture of the angular components of φ and Higgs bosons: where we have defined and tan β ≡ v u /v d . However, the mixing angle is suppressed by the ratio v u,d /f a and hence the massless mode almost consists of a φ . Actually it is this small mixing that admits the axion-gluon-gluon coupling, required for solving the strong CP problem. Another massless mode, a G = cos βa d − sin βa u , is eaten by the Z-boson and the other orthogonal combination becomes massive, which we identify as the pseudo scalar Higgs and denote by a h . For large enough v u , v d ≫ v φ , however, the axion is identified as with v ≡ v 2 u + v 2 d . Actually, in the Higgs inflation model, v u and v d can take so large values that the axion isocurvature perturbation is suppressed as shown in the toy model in the previous section.
The detailed analysis of Higgs inflation with two Higgs doublets are found in Ref. [29]. Thanks to the PQ symmetry, allowed terms are limited. After the conformal transformation g E µν = Ω 2 g J µν where the Einstein frame action becomes with subscript E indicating the Einstein frame. The scalar potential is given by Focusing on only terms with fourth powers of h u and h d , it is expressed as whereλ ud ≡ λ ud + λ ′ ud . Thus it is easy to see that the potential becomes flat for v u ≫ M P / √ ξ u or v d ≫ M P / √ ξ d . Terms involving φ do not affect the inflaton dynamics as we will see. There is a stable inflationary path along v 2 if 2λ d ξ u −λ ud ξ d > 0 and 2λ u ξ d −λ ud ξ u > 0. Then the potential energy for the inflaton is given by where χ is the canonically normalized field in the large field limit: Thus it reduces to the single field Higgs inflation model.
to reproduce the density perturbation observed by Planck [4], where ξ and λ eff denote typical values of ξ's and λ's, respectively. To explain the 125 GeV Higgs boson, λ eff should be O(1), but the running tends to make λ smaller at high energy scale and hence ξ may be able to take a smaller value [30,31]. Next, let us see the behavior of the PQ scalar during inflation. It obtains a VEV of where v h (∼ v u ∼ v d ∼ 10M P / √ ξ) denotes the typical field value of the Higgs boson during inflation. The dynamics after inflation is effectively the same as that studied in the previous section. Note that a φ obtains a mass of Thus we impose the condition to suppress the fluctuation of a φ during inflation. Also note that the reheating temperature after inflation may be as high as ∼ 10 13 GeV taking account of efficient particle production and thermal dissipative effects [32][33][34].
To avoid the PQ symmetry restoration, we need a condition similar to (17): The pseudo scalar Higgs, a h , is almost massless during inflation and develops quantum fluctuations. Note that the canonically normarized field isã h ≡ a h M P / √ ξv h which obtains a fluctuation of δã h ≃ H inf /2π, while the mixing between a φ and a h is given by ∼ v φ /v h . Then we find the effective fluctuation of a φ as δa φ /v φ ∼ √ ξH inf /(2πM P ). Thus the axion isocurvature fluctuation is given by The CDM isocurvature perturbation is given by (14) with v S → M P / √ ξ. Thus the constraint is significantly relaxed.

IV. DISCUSSION
In this letter we have shown a way to suppress the axion isocurvature perturbation. Even if the PQ scalar itself does not have a field value much larger than f a during inflation, other PQ charged scalar fields can have large field values and it results in suppression of the isocurvature perturbation. Interestingly, the electroweak Higgs bosons may take such roles in the DFSZ axion model, and the Higgs bosons can also be the inflaton.
So far, we have considered the quartic interaction term between the PQ scalar and the Higgs bosons λφ 2 H u H d + h.c.. There are other possible choices. For example, let us consider the case with the cubic term V = µφH u H d + h.c.. In this case, φ settles around φ ∼ µ/λ uφ,dφ and has the mass of ∼ λ uφ,dφ v 2 h during the inflation. After the inflation, φ starts to oscillate. If µ < ∼ f a holds, S will not pass through the origin and the restoration of the PQ symmetry due to the particle production does not occur. The higher dimensional terms may also play important roles such as stabilization of the PQ scalar at some field value.
Although we considered the case of Higgs boson as the inflaton, we can also regard the PQ scalar as the inflaton in a similar way, by introducing a non-minimal coupling as [11] The PQ scalar can take a role of inflaton for ξ φ ∼ 5 × 10 4 λ φ . By noting that the canonically normalized axion field at v φ > M P / ξ φ is given byã φ ≡ a φ M P / ξ φ v φ and it obtains quantum fluctuations of ≃ H inf /2π, we would have the axion isocurvature perturbation of the same expression as (38), if the PQ symmetry is never restored thereafter. There is a subtlety, b The PQ scalar as the inflaton in the context of running kinetic inflation was mentioned in Ref. [17].
however, in this scenario. Because the canonically normalized PQ scalar has an oscillation amplitude of ∼ M P just after inflation, it induces efficient axion production when it passes through the origin of the potential, and the PQ symmetry may be restored nonthermally, leading to formation of axion domain walls if the domain wall number is larger than one [27]. We can arrange the model so that the Higgs bosons also have large VEVs during and after inflation just as we have done in the previous section for φ. Then the PQ symmetry is broken by Higgs VEVs even though φ is nonthermally trapped around the origin. Even in such a case, however, the model has a Z 2 symmetry under which φ → −φ and anything else uncharged, hence the domain wall formation is not avoided when φ relaxes to the minimum. Again, in-troducing V = µφH u H d + h.c. in the potential, instead of λφ 2 H u H d + h.c., by assigning appropriate PQ charges, may help the situation but a complete analysis is beyond the scope of this paper.