In quintessential inflation, the scalar field misses the scaling-solution attractor during radiation, so a single exponential tail can drive both inflation and dark energy.
The Peebles -- Vilenkin quintessential inflation model revisited
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abstract
We review the well-known Peebles-Vilenkin (PV) quintessential inflation model and discuss its possible improvements in agreement with the recent observations. The improved PV model depends only on two parameters: the inflaton mass $m$, and another smaller mass $M$; where the latter has to be chosen in order to undertake that, at present time, the dark energy density of the universe is approximately about 70\% of the total energy budget of the universe. The value of the inflaton mass $m$ is calculated using the observational value of the power spectrum of the scalar perturbations, and the value of mass $M$, which depends on the reheating temperature, is calculated by solving the corresponding dynamical system whose initial conditions are taken at the matter-radiation equality and are obtained from three observational data: the red shift at the matter-radiation equality, the ratio of the matter energy density to the critical one at the present time and the current value of the Hubble parameter.
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gr-qc 1years
2019 1verdicts
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Scaling solutions in quintessential inflation
In quintessential inflation, the scalar field misses the scaling-solution attractor during radiation, so a single exponential tail can drive both inflation and dark energy.