Transition rate and gravitational wave spectrum from first-order QCD phase transitions

TL;DR

This paper studies gravitational waves from first-order QCD phase transitions, analyzing their spectra across different models and conditions, and discusses their detectability and implications for early universe phenomena.

Contribution

It provides a comprehensive analysis of gravitational wave spectra from various QCD phase transition models, including effects of baryon density and chemical potential, with implications for detection.

Findings

Gravitational waves peak at 10^{-4}-0.01 Hz, detectable by LISA and Taiji.

High baryon density reduces phase transition rate, producing nanohertz gravitational waves.

Existence of a critical chemical potential where phase transition rate is zero, supporting primordial quark nugget formation.

Abstract

We investigate the gravitational wave spectrum induced by first-order QCD phase transitions including the deconfinement phase transition in the pure gluon system and Friedberg-Lee model, and chiral phase transition in the quark-meson model and Polyakov quark-meson model. The gravitational wave power spectra are sensitive to the phase transition rate $\beta/H$. All QCD models predict a rather large phase transition rate in the order of $\beta/H\sim10^4$ at high temperature region, and the produced gravitational waves lie in the peak frequency region of $10^{-4}-0.01 {\rm Hz}$, corresponding to an energy spectrum in the range of $10^{-8}-10^{-7}$, which can be detected by LISA and Taiji. If a high baryon density is generated through Affleck-Dine baryogenesis or other mechanisms, the baryon chemical potential significantly reduces the phase transition rate, potentially dropping it to the order of $\beta/H\sim 10^1$, leading to the production of nanohertz gravitational waves. Furthermore, a critical quark chemical potential exists with a zero phase transition rate $\beta/H=0$, indicating that the false vacuum will not decay, thus supporting the formation of primordial quark nuggets in the early universe.