Gravitational waves from hidden QCD phase transition

Aoki, M.; Goto, Hiroya; Kubo, Jisuke

doi:10.1103/physrevd.96.075045

Cited by 59 publications

(66 citation statements)

References 132 publications

(221 reference statements)

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“…In this paper we have studied the stochastic GW background produced at the cosmological chiral PT in a conformal extension of the SM [21,22] and extended the analysis of ref. [31]. There are, in the SU (3) flavor symmetry limit, five independent parameters, λ H , λ S , λ HS , y and g H (or the hidden sector scale Λ H ), where effectively two of them are used to obtain m h = 125 GeV and h = 246 GeV.…”

Section: Discussionmentioning

confidence: 99%

“…At finite temperature the real QCD does not undergo a phase transition (PT), rather a continuous change of crossover type [25]. However, for sufficiently small current quark masses, the system a mayumi@hep.s.kanazawa-u.ac.jp b jikubo4@gmail.com arXiv:1910.05025v1 [hep-ph] 11 Oct 2019 can undergo a first-order PT [26][27][28][29], and such a situation can be realized in hidden sector models [17,30,31] (see also [32] and references therein), in which dynamical breaking of scale symmetry takes place at energies higher than the SM scale. If the coupling of the hidden sector to the SM is very small, a chief signal from the hidden sector is the gravitational wave (GW) background produced at a first-order PT in a certain epoch of the Universe [33], see e.g.…”

Section: Introductionmentioning

confidence: 99%

“…We have decided to extend the analysis of ref. [31] from the following reasons: a) The GW energy density depends strongly on the ratio of the duration time τ PT = 1/β of the first-order PT to the Hubble time 1/H, i.e., (β/H) −1 [33,[57][58][59]. Using effective field theories it has been shown [60] that, in contrast to the commonly assumed value of β/H ∼ O(10 2 ) [33,61] (see also [34]), it is of order 10 4 in QCD like theories if the coupling to the SM is neglected, i.e., in the absence of the mediator S. This means a large suppression of the GW energy density.…”

Section: Introductionmentioning

confidence: 99%

“…Since the hidden sector of the model is strongly interacting, we use an effective theory for the dynamical chiral symmetry breaking -the Nambu-Jona-Lasinio (NJL) model [12][13][14] -as in refs. [17,21,22,31], where our approximation method, the self-consistent mean-field approximation (SCMF) of refs. [77,78], is also briefly elucidated in this section.…”

Section: Introductionmentioning

confidence: 99%

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Gravitational waves from chiral phase transition in a conformally extended standard model

Aoki

Kubo

2020

J. Cosmol. Astropart. Phys.

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The gravitational wave (GW) background produced at the cosmological chiral phase transition in a conformal extension of the standard model is studied. To obtain the bounce solution of coupled field equations we implement an iterative method. We find that the corresponding O(3) symmetric Euclidean action S 3 divided by the temperature T has a simple behavior near the critical temperaturewhich is subsequently used to determine the transition's inverse duration β normalized to the Hubble parameter H. It turns out that β/H > ∼ 10 3 , implying that the sound wave period τ sw as an active GW source, too, can be much shorter than the Hubble time. We therefore compute τ sw H and use it as the reduction factor for the sound wave contribution. The signal-to-noise ratio (SNR) for Deci-Hertz Interferometer Gravitational Wave Observatory (DECIGO) and Big Bang Observer (BBO) is evaluated, with the result: SNR DECIGO < ∼ 1.2 and SNR BBO < ∼ 12.0 for five years observation, from which we conclude that the GW signal predicted by the model in the optimistic case could be detected at BBO. 1 The crossover transition in the real QCD can influence the spectrum of the inflationary GW [36-40]. The frequency band of the damped GWs is what has been predicted by Witten [33]. 2 The GWs produced during a cosmological first-oder PT in classically scale invariant models have been recently studied in refs. [44-56].

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Gravitational waves from chiral phase transition in a conformally extended standard model

Aoki

Kubo

2020

J. Cosmol. Astropart. Phys.

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“…At low energies, the dynamics of the quark condensate Σ ij ∼ ψ Rj ψ Li can be described by a linear sigma model. The effective potential for the dynamical field Σ which transforms as a 3 An alternative choice is to study gravitational waves from the chiral phase transition using the Nambu-Jona-Lasinio model [36,37]. 4 Additional model building is needed to solve the strong CP problem completely in these types of models.…”

Section: Low Energy Effective Theorymentioning

confidence: 99%

Dynamical axions and gravitational waves

Croon

Houtz

Sanz

2019

J. High Energ. Phys.

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In this paper we explore the possibility of observable gravitational waves as a manifestation of the QCD axion dynamics. In particular, we focus on dynamical axion models which solve the strong CP problem, and include the confinement of a QCD-like gauge group at the TeV scale. We study the resulting chiral symmetry breaking phase transition for models with N F = 3 and N F = 4 light flavors using the linear sigma model. This model describes the scalar meson spectrum and its interactions, with the diagonal field ϕ as the order parameter. We find that the amplitude of the gravitational wave spectrum depends on the mass of the dynamical axion η via the ratio m η /m ϕ . The resulting spectra may be observed at future mid-range gravitational wave experiments such as AION/MAGIS, DECIGO, and BBO. Moreover, the TeV states can be searched for at colliders and their quantum numbers characterized, providing a unique connection between axion physics, gravitational waves and collider searches.

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String Fragmentation in Supercooled Confinement and Implications for Dark Matter

Gouttenoire

2022

Beyond the Standard Model Cocktail

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A strongly-coupled sector can feature a supercooled confinement transition in the early universe. We point out that, when fundamental quanta of the strong sector are swept into expanding bubbles of the confined phase, the distance between them is large compared to the confinement scale. The flux linking the fundamental quanta then deforms and stretches towards the wall, producing an enhanced number of composite states upon string fragmentation. The composite states are highly boosted in the plasma frame, which leads to additional particle production through the subsequent deep inelastic scattering. We propose a modelling of these dynamics and study the consequences for the abundance and energetics of particles in the universe and for bubble-wall Lorentz factors. This opens several new avenues of investigation, which we begin to explore here, showing that the composite dark matter relic density is affected by many orders of magnitude.

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Gravitational waves from hidden QCD phase transition

Cited by 59 publications

References 132 publications

Gravitational waves from chiral phase transition in a conformally extended standard model

Gravitational waves from chiral phase transition in a conformally extended standard model

Dynamical axions and gravitational waves

String Fragmentation in Supercooled Confinement and Implications for Dark Matter

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