On the Maximal Strength of a First-Order Electroweak Phase Transition and its Gravitational Wave Signal

TL;DR

This paper investigates the maximum strength of a first-order electroweak phase transition and its gravitational wave signals, considering supercooling effects and the conditions for successful transition completion in beyond Standard Model theories.

Contribution

It provides a general framework for bubble nucleation and percolation during strong supercooling, establishing bounds on transition temperature and analyzing GW signal characteristics.

Findings

Peak GW frequency is typically above 10^{-4} Hz.

Sound wave GW signals may be shorter-lived than previously assumed.

Turbulence could dominate GW production, reducing overall signal strength.

Abstract

What is the maximum possible strength of a first-order electroweak phase transition and the resulting gravitational wave (GW) signal? While naively one might expect that supercooling could increase the strength of the transition to very high values, for strong supercooling the Universe is no longer radiation-dominated and the vacuum energy of the unstable minimum of the potential dominates the expansion, which can jeopardize the successful completion of the phase transition. After providing a general treatment for the nucleation, growth and percolation of broken phase bubbles during a first-order phase transition that encompasses the case of significant supercooling, we study the conditions for successful bubble percolation and completion of the electroweak phase transition in theories beyond the Standard Model featuring polynominal potentials. For such theories, these conditions set a lower bound on the temperature of the transition. Since the plasma cannot be significantly diluted, the resulting GW signal originates mostly from sound waves and turbulence in the plasma, rather than bubble collisions. We find the peak frequency of the GW signal from the phase transition to be generically $f \gtrsim 10^{-4}$ Hz. We also study the condition for GW production by sound waves to be long-lasting (GW source active for approximately a Hubble time), showing it is generally not fulfilled in concrete scenarios. Because of this the sound wave GW signal could be weakened, with turbulence setting in earlier, resulting in a smaller overall GW signal as compared to current literature predictions.