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Primordial non-Gaussianities from multiple-field inflation
We calculate the three-point correlation function evaluated at horizon crossing for a set of interacting scalar fields coupled to gravity during inflation. This provides the initial condition for the
Primordial non-Gaussianities in single-field inflation
We calculate the three-point function for primordial scalar fluctuations in a single-field inflationary scenario where the scalar field Lagrangian is a completely general function of the field and
Reconstructing the inflaton potential—an overview
The authors review the relation between the inflationary potential and the spectra of density waves (scalar perturbations) and gravitational waves (tensor perturbations) produced, with particular
The inflationary trispectrum
We calculate the trispectrum of the primordial curvature perturbation generated by an epoch of slow-roll in. ation in the early universe, and demonstrate that the non-Gaussian signature imprinted at
Cosmic dynamics of Bose–Einstein condensates
A dynamical correspondence is established between positively curved, isotropic, perfect fluid cosmologies and quasi-two-dimensional, harmonically trapped Bose–Einstein condensates by mapping the
Ermakov-Pinney equation in scalar field cosmologies
It is shown that the dynamics of cosmologies sourced by a mixture of perfect fluids and self-interacting scalar fields are described by the non-linear, Ermakov-Pinney equation. The general solution
Stretching the inflaton potential with kinetic energy
Inflation near a maximum of the potential is studied when nonlocal derivative operators are included in the inflaton Lagrangian. Such terms can impose additional sources of friction on the field. For
Non-Gaussianity from the inflationary trispectrum
We present an estimate for the non-linear parameter τNL, which measures the non-Gaussianity imprinted in the trispectrum of the comoving curvature perturbation, ζ. Our estimate is valid throughout
An Emergent Universe from a loop
Closed, singularity-free, inflationary cosmological models have recently been studied in the context of general relativity. Despite their appeal, these so called emergent models suffer from a number