End of multi-field inflation and the perturbation spectrum

Abstract

We investigate the dynamics of inflation models driven by multiple, decoupled scalar fields and calculate the Hubble parameter and the amplitude of the lightest field at the end of inflation which may be responsible for interesting, or possibly dangerous cosmological consequences after inflation. The results are very simple and similar to those of the single field inflation, mainly depend on the underlying spectrum of the masses. The mass distribution is heavily constrained by the power spectrum of density perturbations P and the spectral index n. The overall mass scale gives the amplitude of P, and n is affected by the number of fields and the spacing between masses in the distribution. The drop-out effect of the massive fields makes the perturbation spectrum typically redder than the single field inflation spectrum. We illustrate this using two different mass distributions.

arXiv comment(v1) 16 pages, 5 figures, 3 tables; (v2) 17 pages, references added, typos corrected; (v3) references added, typos corrected; (v4) 16 pages, typos corrected, Table 1 expanded and Table 3 removed, Figs. 2 and 3 reduced, to appear in Physical Review D

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Cited by in corpus (18)

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• Energy Transfer in Multi Field Inflation and Cosmological Perturbations
• Non-Gaussianities in N-flation
• Preheating after N-flation
• Systematics of multi-field effects at the end of warped brane inflation
• Nflation: observable predictions from the random matrix mass spectrum
• Evolution of the curvature perturbation during and after multi-field inflation
• Multiple scalar particle decay and perturbation generation
• The lessons from the running of the tensor-to-scalar ratio
• On Number of Nflation Fields
• Spectrum of Curvature Perturbation of Multi-field Inflation with Small-Field Potential
• Generation of perturbation after multi-field inflation
• Inflation with antisymmetric tensor field: new candidates
• Entropy Perturbations in N-flation
• Phase Diagram for Nflation
• Scalar and vector modes in inflation with antisymmetric tensor field
• Minimal gauge inflation
• Sustainability of multi-field inflation and bound on string scale