Speaker
Description
Supercooled cosmological phase transitions typically yield a strong gravitational-wave background, potentially detectable, e.g. in LISA. The scenario of supercooling is naturally realised in models with classical scale invariance, where symmetry is broken radiatively. I will review the phenomenology of the supercooled phase transition and explain how to properly compute the bubble nucleation rate. One can wonder whether introducing mass scales through the on-shell renormalisation could break scale invariance and significantly alter phenomenological predictions of this class of models. In this talk, working with a simple model, I will explain how to renormalise classically scale-invariant models in the on-shell scheme. Understanding the correspondence between various mass scales will shed some light on the naturalness of classically scale-invariant scenarios.
