PhD thesis
Quantum Fluctuations of Vector Fields and the Primordial Curvature Perturbation in the Universe
The successes and fine-tuning problems of the Hot Big Bang theory of the Universe are briefly reviewed and inflation is introduced. It alleviates those problems substantially and give rise to the primordial curvature perturbation with the properties observed in the cosmic microwave background. It is shown how application of the quantum field theory in the exponentially expanding Universe leads to the conversion of quantum fluctuations into the classical field perturbation. The δN formalism is introduced and applied to calculate the primordial curvature perturbation ζ for three examples: single field inflation, the end-of-inflation and the curvaton scenarios.
The δN formalism is extended to include the perturbation of the vector field. The later is quantized in de Sitter space-time and it is found that in general the particle production process of the vector field is anisotropic. This anisotropy is parametrized by introducing two parameters p and q, which are determined by the conformal invariance braking mechanism. If any of them are non-zero, generated ζ is statistically anisotropic. Then the power spectrum of ζ and the non-linearity parameter fNL have an angular modulation.
This formalism is applied for two vector curvaton models and the end-of-inflation scenario. It is found that for p≠0, the magnitude of fNL and the direction of its angular modulation is correlated with the anisotropy in the spectrum. If |p|≥1, the anisotropic part of fNL is dominant over the isotropic one. These are distinct observational signatures; their detection would be a smoking gun for a vector field contribution to ζ.
In the first curvaton model the vector field is non-minimally coupled to gravity and in the second one it has a time varying kinetic function and mass. In the former, only statistically anisotropic ζ can be generated, while in the later, isotropic ζ may be realized too. Parameter spaces for these vector curvaton scenarios are large enough for them to be realized in the particle physics models. In the end-of-inflation scenario fNL have similar properties to the vector curvaton scenario with additional anisotropic term.