Supercooled first-order phase transition
A cosmological first-order phase transition is said supercooled when the nucleation temperature is much smaller than the critical temperature (defined when the two minima coincide). This can happen when the tunnelling rate varies very slowly, e.g. logarithmically, with the temperature. Typical scenarios are phase transitions in nearly-conformal sectors in which the scalar field dynamics is dominated by logarithmic loop corrections. Bubble wall expands in diluted plasma, reach ultra-relativistic velocities and cosmological size. They produce a large gravitational waves signal and present interesting wall-particle dynamics.
Published in: JHEP 04 (2021) 278 e-Print: 2007.08440 [hep-ph]
We point out novel effects in supercooled confinement: flux tube formation, string fragmentation, deep-inelastic-scattering
e-Print: 2110.13926 [hep-ph]
We present particle physics model leading to a large amount of supercooling. We derive the O3 and O4 bounce actions in great details (numerically and analytically)
Published in: JHEP 05 (2022) 004 e-Print: 2112.07686 [hep-ph]
During a cosmological first-order phase transition, particles of the plasma crossing the bubble walls can radiate a gauge boson. We resum the real and virtual emissions at all leading-log orders, both analytically and numerically using a Monte-Carlo simulation. We find that radiated bosons are dominantly soft and that the resulting retarding pressure on relativistic bubble walls is linear both in the Lorentz boost and in the order parameter, up to a log.
Accepted by Scipost (2023) e-Print: 2207.05096 [hep-ph]
Upon acquiring a mass inside a bubble, a particle is put off-shell. In the previous paragraph we saw that it can return on-shell by radiating Bremsstrahlung radiation. Another possibility is by decaying into a pair of heavy particles. Hence, bubble wall motion during a 1stOPT can lead to non-adiabatic production of heavy DM. In the present work, we show that DM is produced with a large momentum and therefore it can give signature in large scale structure observables.
