Numerical simulations of gravitational waves from early-universe turbulence

Pol, Alberto Roper; Mandal, Sayan; Brandenburg, Axel; Kahniashvili, Tina; Kosowsky, Arthur

doi:10.1103/physrevd.102.083512

Cited by 128 publications

(214 citation statements)

References 45 publications

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“…For more recent work on the dynamics of cosmological phase transitions and the shape of the resulting GW signal, we refer to refs. [139][140][141][142][143][144][145][146][147][148][149][150][151][152][153][154][155].…”

Section: Gravitational-wave Signal From a Cosmological Phase Transitionmentioning

confidence: 99%

New sensitivity curves for gravitational-wave signals from cosmological phase transitions

Schmitz

2021

J. High Energ. Phys.

216

149

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Gravitational waves (GWs) from strong first-order phase transitions (SFOPTs) in the early Universe are a prime target for upcoming GW experiments. In this paper, I construct novel peak-integrated sensitivity curves (PISCs) for these experiments, which faithfully represent their projected sensitivities to the GW signal from a cosmological SFOPT by explicitly taking into account the expected shape of the signal. Designed to be a handy tool for phenomenologists and model builders, PISCs allow for a quick and systematic comparison of theoretical predictions with experimental sensitivities, as I illustrate by a large range of examples. PISCs also offer several advantages over the conventional power-law-integrated sensitivity curves (PLISCs); in particular, they directly encode information on the expected signal-to-noise ratio for the GW signal from a SFOPT. I provide semianalytical fit functions for the exact numerical PISCs of LISA, DECIGO, and BBO. In an appendix, I moreover present a detailed review of the strain noise power spectra of a large number of GW experiments. The numerical results for all PISCs, PLISCs, and strain noise power spectra presented in this paper can be downloaded from the Zenodo online repository [1]. In a companion paper [2], the concept of PISCs is used to perform an in-depth study of the GW signal from the cosmological phase transition in the real-scalar-singlet extension of the standard model. The PISCs presented in this paper will need to be updated whenever new theoretical results on the expected shape of the signal become available. The PISC approach is therefore suited to be used as a bookkeeping tool to keep track of the theoretical progress in the field.

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Section: Gravitational-wave Signal From a Cosmological Phase Transitionmentioning

confidence: 99%

New sensitivity curves for gravitational-wave signals from cosmological phase transitions

Schmitz

2021

J. High Energ. Phys.

216

149

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“…While study of production of GWs in such a transition is a daunting task usually approached through lattice simulations [1011,1012,1013,1014,1015,1016] or through simplified analytical modelling [1017,1018,1019,1020,1021,1022,234], typically the results are parametrised by just a few crucial parameters [1023,1024,457]. These are, firstly, strength of the phase transition,…”

Section: First Order Phase Transitionsmentioning

confidence: 99%

“…All the quantities marked with a * are evaluated at the transition temperature. There are three main sources of GWs in a phase transition: collisions of bubble walls [1011,1014], sound waves produced by bubbles in the plasma [1012,1020,1013] and turbulence ensuing after the transition [1017,1018,1019,1016]. All the expressions necessary to calculate the signal can be found for example in [235].…”

Section: First Order Phase Transitionsmentioning

confidence: 99%

The First Three Seconds: a Review of Possible Expansion Histories of the Early Universe

Allahverdi¹,

Amin²,

Berlin³

et al. 2021

TheOJA

194

140

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It is commonly assumed that the energy density of the Universe was dominated by radiation between reheating after inflation and the onset of matter domination 54,000 years later. While the abundance of light elements indicates that the Universe was radiation dominated during Big Bang Nucleosynthesis (BBN), there is scant evidence that the Universe was radiation dominated prior to BBN. It is therefore possible that the cosmological history was more complicated, with deviations from the standard radiation domination during the earliest epochs. Indeed, several interesting proposals regarding various topics such as the generation of dark matter, matter-antimatter asymmetry, gravitational waves, primordial black holes, or microhalos during a nonstandard expansion phase have been recently made. In this paper, we review various possible causes and consequences of deviations from radiation domination in the early Universe -taking place either before or after BBN -and the constraints on them, as they have been discussed in the literature during the recent years.

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“…Only dedicated numerical simulations can resolve these issue. The simulations of turbulent vortical flow [107] seem to disagree with all the predictions, having a slow rise of around k 1 to the peak, and a k −8/3 decay at high wavenumber.…”

Section: Initially the Bubbles Of The Stable Phase Collide And Mergementioning

confidence: 68%

“…The turbulent stage, however, is far less well understood, as simulations of turbulent flows are very challenging [97,107], and consequently the modelling [102,105,106] relies on untested assumptions. The main assumptions that go into the modelling are how the flow autocorrelation time depends on wavenumber, and also how the global quantities such as kinetic energy and correlation length evolve with time.…”

Section: Initially the Bubbles Of The Stable Phase Collide And Mergementioning

confidence: 99%

Phase transitions in the early universe

Hindmarsh

Lüben

Lumma

et al. 2021

SciPost Phys. Lect. Notes

158

169

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These lecture notes are based on a course given by Mark Hindmarsh at the 24th Saalburg Summer School 2018 and written up by Marvin Lüben, Johannes Lumma and Martin Pauly. The aim is to provide the necessary basics to understand first-order phase transitions in the early universe, to outline how they leave imprints in gravitational waves, and advertise how those gravitational waves could be detected in the future. A first-order phase transition at the electroweak scale is a prediction of many theories beyond the Standard Model, and is also motivated as an ingredient of some theories attempting to provide an explanation for the matter-antimatter asymmetry in our Universe. Starting from bosonic and fermionic statistics, we derive Boltzmann's equation and generalise to a fluid of particles with field dependent mass. We introduce the thermal effective potential for the field in its lowest order approximation, discuss the transition to the Higgs phase in the Standard Model and beyond, and compute the probability for the field to cross a potential barrier. After these preliminaries, we provide a hydrodynamical description of first-order phase transitions as it is appropriate for describing the early Universe. We thereby discuss the key quantities characterising a phase transition, and how they are imprinted in the gravitational wave power spectrum that might be detectable by the space-based gravitational wave detector LISA in the 2030s.

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Numerical simulations of gravitational waves from early-universe turbulence

Cited by 128 publications

References 45 publications

New sensitivity curves for gravitational-wave signals from cosmological phase transitions

New sensitivity curves for gravitational-wave signals from cosmological phase transitions

The First Three Seconds: a Review of Possible Expansion Histories of the Early Universe

Phase transitions in the early universe

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