Abstract

We have tested some simple quintessential inflation models, imposing the requirement that they match with the recent observational data provided by the BICEP and Planck team and leading to a reheating temperature, which is obtained via gravitational particle production after inflation, supporting the nucleosynthesis success. Moreover, for the models coming from supergravity one needs to demand low temperatures in order to avoid problems such as the gravitino overproduction or the gravitational production of moduli fields, which are obtained only when the reheating temperature is due to the production of massless particles with a coupling constant very close to its conformal value.

Highlights

  • Quintessential inflation [1] is a good candidate to unify the early and late time acceleration of our universe

  • We have tested some simple quintessential inflation models, imposing the requirement that they match with the recent observational data provided by the BICEP and Planck team and leading to a reheating temperature, which is obtained via gravitational particle production after inflation, supporting the nucleosynthesis success

  • The main goal of the present work is to study the viability of some well-known inflationary potentials, some of them coming from supersymmetric theories, adapted to quintessence

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Summary

Introduction

Quintessential inflation [1] is a good candidate to unify the early and late time acceleration of our universe. At very late times, the quintessential potential dominates and the universe starts to accelerate again Having this in mind, the main goal of the present work is to study the viability of some well-known inflationary potentials, some of them coming from supersymmetric theories, adapted to quintessence. We obtain a potential with a phase transition that models an inflationary universe at early times, which reheats the universe via gravitational particle production after inflation and it is dominated by the cosmological constant. Once we have these potentials, we calculate their spectral parameters, the number of e-folds, which has to be in quintessential inflation between 63 and 73.

A non-singular model
Cosmological perturbations
The scalar field
Reheating constraints
Simple quintessential inflation models
He6nd 163π m2
Other quintessential inflation potentials
Conclusions
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