Low-scale Quintessential Inflation

Abstract

In quintessential inflationary model, the same master field that drives inflation becomes, later on, the dynamical source of the (present) accelerated expansion. Quintessential inflationary models require a curvature scale at the end of inflation around $10^{-6}{M}_{\mathrm{P}}$ in order to explain the large scale fluctuations observed in the microwave sky. If the curvature scale at the end of inflation is much smaller than $10^{-6}{M}_{\mathrm{P}}$, the large scale adiabatic mode may be produced thanks to the relaxation of a scalar degree of freedom, which will be generically denoted, according to the recent terminology, as the curvaton field. The production of the adiabatic mode is analysed in detail in the case of the minimal quintessential inflationary model originally proposed by Peebles and Vilenkin.

25 pages; 5 figures

References in corpus (2)

• Large Scale Structure from the Higgs fields of the Supersymmetric Standard Model
• Constraints on pre-big bang parameter space from CMBR anisotropies

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