Gravitational waves from cosmic bubble collisions

Kim, Dong-Hoon; Lee, Bum-Hoon; Lee, Wonwoo; Yang, J.; Yeom, Dong-han

doi:10.1140/epjc/s10052-015-3348-2

Cited by 11 publications

(4 citation statements)

References 25 publications

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“…This one provides a distinguishable difference in the exponential suppression factor B between two models, one corresponds to the event without gravitation, and the other corresponds to the event with gravitation. The inverse time duration of the phase transition corresponding to the nucleation rate of an -symmetric bubble is given by [12,77]…”

Section: S O ρmentioning

confidence: 99%

Gravitational waves from the vacuum decay with LISA *

Yin¹,

Lee²,

Lee³

et al. 2022

Chinese Phys. C

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We investigate the gravitational wave spectrum resulted from the cosmological first-order phase transition. We compare two models; one is a scalar field model without gravitation, while the other is a scalar field model with gravitation. Based on the sensitivity curves of the LISA space-based interferometer on the stochastic gravitational-wave background, we compare the difference between the gravitational wave spectra of the former and the latter cases resulted from the bubble collision process. Especially, we calculated the speed of the bubble wall before collision for the two models numerically. We show that the difference between the amplitudes of those spectra can clearly distinguish between the two models. We expect that the LISA with Signal to Noise Ratio =10 could observe the spectrum as the fast first-order phase transition.

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Section: S O ρmentioning

confidence: 99%

Gravitational waves from the vacuum decay with LISA *

Yin¹,

Lee²,

Lee³

et al. 2022

Chinese Phys. C

Self Cite

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“…Collisions between vacuum bubbles have also been considered, beginning with the work of Hawking, Moss and Stewart [11]. Early studies were motivated JCAP09(2015)004 by the dynamics of early phase transitions within our horizon, with much of the focus on the production of gravitational waves [12][13][14][15][16][17][18][19]. Recent studies are more often motivated by bubble nucleation in false vacuum inflation [20][21][22][23][24][25].…”

Section: Jcap09(2015)004mentioning

confidence: 99%

Cosmic bubble and domain wall instabilities III: the role of oscillons in three-dimensional bubble collisions

Bond

Braden

Mersini-Houghton

2015

J. Cosmol. Astropart. Phys.

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Abstract. We study collisions between pairs of bubbles nucleated in an ambient false vacuum. For the first time, we include the effects of small initial (quantum) fluctuations around the instanton profiles describing the most likely initial bubble profile. Past studies of this problem neglect these fluctuations and work under the assumption that the collisions posess an exact SO(2,1) symmetry. We use three-dimensional lattice simulations to demonstrate that for double-well potentials, small initial perturbations to this symmetry can be amplified as the system evolves. Initially the amplification is well-described by linear perturbation theory around the SO(2,1) background, but the onset of strong nonlinearities amongst the fluctuations quickly leads to a drastic breaking of the original SO(2,1) symmetry and the production of oscillons in the collision region. We explore several single-field models, and we find it is hard to both realize inflation inside of a bubble and produce oscillons in a collision. Finally, we extend our results to a simple two-field model. The additional freedom allowed by the second field allows us to construct viable inflationary models that allow oscillon production in collisions. The breaking of the SO(2,1) symmetry allows for a new class of observational signatures from bubble collisions that do not posess azimuthal symmetry, including the production of gravitational waves which cannot be supported by an SO(2,1) spacetime.

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“…For both cases, inside is a true-vacuum region, and after the nucleation, the bubble should expand over the spacetime; otherwise, the scalar field combination is, in general, unstable. Such a bubble may explain the phase transition of the early universe cosmology [21][22][23][24][25][26]; also, some interactions between bubbles may be a source of gravitational waves [27][28][29].…”

Section: Introductionmentioning

confidence: 99%

Properties of Scalar Hairy Black Holes and Scalarons with Asymmetric Potential

Chew¹,

Yeom²,

Blázquez-Salcedo³

2022

Preprint

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In this paper we study the properties of black holes and scalarons in Einstein gravity when it is minimally coupled to a scalar field φ with an asymmetric potential V (φ), constructed in [Phys. Rev. D 73 (2006), 084002] a few decades ago. V (φ) has been applied in the cosmology to describe the quantum tunneling process from the false vacuum to the true vacuum and contains a local maximum, a local minimum (false vacuum) and a global minimum (true vacuum). In particular we focus on the asymptotically flat solutions, which can be constructed by fixing appropriately the local minimum of V . A branch of hairy black holes solutions emerge from the Schwarzschild black hole, and we study the domain of existence of such configurations. They can reach to a particle-like solution in the small horizon limit, i.e. the scalarons. We study the stability of black holes and scalarons, showing that all of them are unstable under radial perturbations.

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Gravitational waves from cosmic bubble collisions

Cited by 11 publications

References 25 publications

Gravitational waves from the vacuum decay with LISA *

Gravitational waves from the vacuum decay with LISA *

Cosmic bubble and domain wall instabilities III: the role of oscillons in three-dimensional bubble collisions

Properties of Scalar Hairy Black Holes and Scalarons with Asymmetric Potential

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