Answers are grounded in this paper and cite their sources.
The dynamics of the scalar field driving inflation can be described as a Brownian motion under the influence of a classical force arising from its self-interactions. Fluctuations of the inflaton on large scales give rise to density perturbations. If the inflaton potential is not too flat, as in models of nonexponential inflation, these perturbations can be non-Gaussian. In a power-law inflation with an exponential potential non-Gaussian scale-invariant adiabatic perturbations are rapidly produced.
No takes yet. Share an insight, caveat, or question.
Ortolan et al. (1988) studied this question.
Synapse has enriched 10 related papers. Consider them for comparative context: