Scaling solutions in quintessential inflation

Abstract

In quintessence scalar field theories, the presence of scaling solutions are important during the radiation and matter epoch due to having their attractor character. Usually, it is assumed that the initial conditions of the quintessence field are in the basin of attraction of the scaling solutions. However, in order to reproduce the current cosmic acceleration, at late times, a mechanism to exit this behavior is needed. In the present work we show that the quintessential inflation models could be an excellent candidate to exhibit the above behavior. However, the crucial point of quintessential inflation is that the initial conditions has to be taken during the inflation, and at the beginning of the radiation era, the scalar field does not belong to the basin of attraction of the scaling solution. This means that, in the case where quintessence is depicted via exponential potentials, only a single exponential in the tail of the { quintessential inflation} potential is enough to depict the evolution of our universe.

arXiv comment17 pages, 6 figures. Version accepted for publication in EPJC

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• Quintessential Inflation from Lorentzian Slow Roll
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• What is needed of a scalar field if it is to unify inflation and late time acceleration ?
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• Particle Production Scenario in an Algebraically Coupled Quintessence Field with a Dark Matter Fluid
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• Reheating constraints and the $H_0$ tension in Quintessential Inflation