Speaker
Eemeli Tomberg
Description
Primordial black holes can arise from strong fluctuations produced during cosmic inflation. Stochastic inflation is a method to compute the fluctuation statistics non-perturbatively. It approximates the complicated, full quantum field theory computation and is needed for accurate black hole predictions. I discuss recent progress in the numerical implementation of the method and highlight the role of a constant-roll phase and the resulting non-Gaussian curvature distribution. As a new result, I present numerically solved profiles of the compaction function, the correct quantity to characterize the black hole collapse process.
