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Cosmological Inflation and Large-Scale Structure
TLDR
This textbook is the first to provide a modern and unified overview of inflationary cosmology and carefully compares predictions with the latest observations, including those of the cosmic microwave background, the clustering and velocities of galaxies and the epoch of structure formation.
What Would We Learn by Detecting a Gravitational Wave Signal in the Cosmic Microwave Background Anisotropy
Inflation generates gravitational waves, which may be observable in the low multipoles of the cosmic microwave background anisotropy but only if the inflaton field variation is at least of order the
The Primordial Density Perturbation: Cosmology, Inflation and the Origin of Structure
1. Overview Part I. Relativity: 2. Special relativity 3. General relativity Part II. The Universe after the First Second: 4. The unperturbed Universe 5. The primordial density perturbation 6.
A general proof of the conservation of the curvature perturbation
Without invoking a perturbative expansion, we define the cosmological curvature perturbation, and consider its behaviour assuming that the universe is smooth over a sufficiently large comoving scale.
The Primordial Density Perturbation
The origin and evolution of the primordial perturbation is the key to understanding structure formation in the earliest stages of the Universe. It carries clues to the types of physical phenomena
Inflationary prediction for primordial non-gaussianity.
We extend the deltaN formalism so that it gives all of the stochastic properties of the primordial curvature perturbation zeta if the initial field perturbations are Gaussian. The calculation
A New approach to the evolution of cosmological perturbations on large scales
We discuss the evolution of linear perturbations about a Friedmann-Robertson-Walker background metric, using only the local conservation of energy-momentum. We show that on sufficiently large scales
Primordial density perturbation in the curvaton scenario
We analyze the primordial density perturbation when it is generated by a “curvaton” field different from the inflaton. In some cases this perturbation may have large isocurvature components, fully
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