Shallow relic gravitational wave spectrum with acoustic peak

Abstract

We study the gravitational wave (GW) spectrum produced by acoustic waves in the early universe, such as would be produced by a first order phase transition, focusing on the low-frequency side of the peak. We confirm with numerical simulations the Sound Shell model prediction of a steep rise with wave number $k$ of $k^9$ to a peak whose magnitude grows at a rate $(H/k_{\text{p}})H$, where $H$ is the Hubble rate and $k_{\text{p}}$ the peak wave number, set by the peak wave number of the fluid velocity power spectrum. We also show that hitherto neglected terms give a shallower part with amplitude $(H/k_{\text{p}}{)}^2$ in the range $H\lesssim k\lesssim k_{\text{p}}$, which in the limit of small $H/k$ rises as $k$. This linear rise has been seen in other modelling and also in direct numerical simulations. The relative amplitude between the linearly rising part and the peak therefore depends on the peak wave number of the velocity spectrum and the lifetime of the source, which in an expanding background is bounded above by the Hubble time $H^{-1}$. For slow phase transitions, which have the lowest peak wave number and the loudest signals, the acoustic GW peak appears as a localized enhancement of the spectrum, with a rise to the peak less steep than $k^9$. The shape of the peak, absent in vortical turbulence, may help to lift degeneracies in phase transition parameter estimation at future GW observatories.

21 pages, 10 figures, Accepted for publication in JCAP

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• Primordial acoustic turbulence: three-dimensional simulations and gravitational wave predictions
• Gravitational Waves from Phase Transitions
• General bubble expansion at strong coupling
• Fundamental Physics and Cosmology with TianQin
• Detecting Cosmological Phase Transitions with Taiji: Sensitivity Analysis and Parameter Estimation
• General backreaction force of cosmological bubble expansion
• Gravitational waves from vacuum bubbles: Ultraviolet dependence on wall thickness
• LISA and $\gamma$-ray telescopes as multi-messenger probes of a first-order cosmological phase transition