End of multi-field inflation and the perturbation spectrum
Abstract
Description
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.
(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
(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