Eternal Inflation, Bubble Collisions, and the Disintegration of the Persistence of Memory

TL;DR

This paper calculates the probability and distribution of bubble collisions in an inflating universe, revealing that such collisions are more common than previously thought and could impact observable cosmic microwave background features.

Contribution

It generalizes previous models by including cosmological evolution and domain wall dynamics, providing a more accurate estimate of bubble collision probabilities and their observable signatures.

Findings

Expected number of bubble collisions is proportional to decay rate and vacuum energies.

Collision distribution on the CMB sky is nearly isotropic.

Number of observable collisions scales with universe curvature.

Abstract

We compute the probability distribution for bubble collisions in an inflating false vacuum which decays by bubble nucleation. Our analysis generalizes previous work of Guth, Garriga, and Vilenkin to the case of general cosmological evolution inside the bubble, and takes into account the dynamics of the domain walls that form between the colliding bubbles. We find that incorporating these effects changes the results dramatically: the total expected number of bubble collisions in the past lightcone of a typical observer is N ~ \gamma V_f / V_i, where \gamma is the fastest decay rate of the false vacuum, V_f is its vacuum energy, and V_i is the vacuum energy during inflation inside the bubble. This number can be large in realistic models without tuning. In addition, we calculate the angular position and size distribution of the collisions on the cosmic microwave background sky, and demonstrate that the number of bubbles of observable angular size is N_{LS} \sim \sqrt{\Omega_k} N, where \Omega_k is the curvature contribution to the total density at the time of observation. The distribution is almost exactly isotropic.