Gravitational waves from bubble walls

Mégevand, Ariel; Membiela, Federico Agustín

doi:10.1088/1475-7516/2021/10/073

Cited by 10 publications

(16 citation statements)

References 69 publications

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“…For that aim we have applied the approach of Ref. [125] to this mechanism with the envelope approximation. Besides computing the GW spectrum for a couple of phase transition models, we have studied its asymptotic limits for arbitrary nucleation rate Γ(t) and wall velocity v(t).…”

Section: Conclusion and Discussionmentioning

confidence: 99%

“…This can be seen in the general expressions derived in Ref. [125] and, for the envelope approximation, in the form of the source (15). For the simultaneous nucleation, the average uncollided wall area of a bubble is given by [135]…”

Section: Time and Size Scalesmentioning

confidence: 90%

“…We shall use the approach of Ref. [125], which we summarize very briefly. For a large volume V , the GW power spectrum is written in the form…”

Section: Gws From Bubble Wallsmentioning

confidence: 99%

“…Here, Θ is the Heaviside step function, and we have used the notation r = R(t , t), r = R(t , t ) (for more details and interpretation, see [135] or [125]). The final expressions from Ref.…”

Section: Gws From Bubble Wallsmentioning

confidence: 99%

“…This model was investigated either with semi-analytical calculations [123] and by simulating the formation and expansion of the thin fluid shells [124]. Recently, we discussed a more general semi-analytic approach [125], which can be applied to the envelope or bulk-flow approximations, as well as to more general wall kinematics.…”

Section: Introductionmentioning

confidence: 99%

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Model-independent features of gravitational waves from bubble collisions

Megevand,

Membiela

2021

Preprint

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We study the gravitational radiation produced by the collisions of bubble walls or thin fluid shells in cosmological phase transitions. Using the so-called envelope approximation, we obtain analytically the asymptotic behavior of the gravitational wave spectrum at low and high frequencies for any phase transition model. The complete spectrum can thus be approximated by a simple interpolation between these asymptotes. We verify this approximation with specific examples. We use these results to discuss the dependence of the spectrum on the time and size scales of the source.

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Section: Conclusion and Discussionmentioning

confidence: 99%

Section: Time and Size Scalesmentioning

confidence: 90%

“…We shall use the approach of Ref. [125], which we summarize very briefly. For a large volume V , the GW power spectrum is written in the form…”

Section: Gws From Bubble Wallsmentioning

confidence: 99%

Section: Gws From Bubble Wallsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Model-independent features of gravitational waves from bubble collisions

Megevand,

Membiela

2021

Preprint

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Particle shells from relativistic bubble walls

Baldes,

Dichtl,

Gouttenoire

et al. 2024

J. High Energ. Phys.

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Relativistic bubble walls from cosmological phase transitions (PT) necessarily accumulate expanding shells of particles. We systematically characterize shell properties, and identify and calculate the processes that prevent them from free streaming: phase-space saturation effects, out-of-equilibrium 2 → 2 and 3 → 2 shell-shell and shell-bath interactions, and shell interactions with bubble walls. We find that shells do not free stream in scenarios widely studied in the literature, where standard predictions will need to be reevaluated, including those of bubble wall velocities, gravitational waves (GW) and particle production. Our results support the use of bulk-flow GW predictions in all regions where shells free stream, irrespectively of whether or not the latent heat is mostly converted in the scalar field gradient.

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Searching for heavy leptophilic Z′: from lepton colliders to gravitational waves

Dasgupta,

Dev,

Han

et al. 2023

J. High Energ. Phys.

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We study the phenomenology of leptophilic Z′ gauge bosons at the future high-energy e+e− and μ+μ− colliders, as well as at the gravitational wave observatories. The leptophilic Z′ model, although well-motivated, remains largely unconstrained from current low-energy and collider searches for Z′ masses above $$ \mathcal{O} $$ O (100 GeV), thus providing a unique opportunity for future lepton colliders. Taking $$ \textrm{U}{(1)}_{L_{\alpha }-{L}_{\beta }} $$ U 1 L α − L β (α, β = e, μ, τ) models as concrete examples, we show that future e+e− and μ+μ− colliders with multi-TeV center-of-mass energies provide unprecedented sensitivity to heavy leptophilic Z′ bosons. Moreover, if these U(1) models are classically scale-invariant, the phase transition at the U(1) symmetry-breaking scale tends to be strongly first-order with ultra-supercooling, and leads to observable stochastic gravitational wave signatures. We find that the future sensitivity of gravitational wave observatories, such as advanced LIGO-VIRGO and Cosmic Explorer, can be complementary to the collider experiments, probing higher Z′ masses up to $$ \mathcal{O} $$ O (104 TeV), while being consistent with naturalness and perturbativity considerations.

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Gravitational waves from bubble walls

Cited by 10 publications

References 69 publications

Model-independent features of gravitational waves from bubble collisions

Model-independent features of gravitational waves from bubble collisions

Particle shells from relativistic bubble walls

Searching for heavy leptophilic Z′: from lepton colliders to gravitational waves

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