The Peebles–Vilenkin quintessential inflation model revisited

From the assumption that the slow-roll parameter ε has a Lorentzian form as a function of the e-fold number N , a successful model of a quintessential inflation is obtained, as succinctly studied in [1]. The form corresponds to the vacuum energy both in the inflationary and in the dark-energy epochs and satisfies the condition to climb from small values of ε to 1 at the end of the inflationary epoch. We find the corresponding scalar quintessential inflationary potential with two flat regions. Moreover, a reheating mechanism is suggested with numerical estimation for the homogeneous evolution of the universe. The suggested mechanism is consistent with the BBN bound.

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“…From the time duration one can calculate the density of particles in the phase space [96][97][98][99][100][101][102][103][104][105]:…”

Section: Reheatingmentioning

confidence: 99%

Quintessential inflation from Lorentzian slow roll

Benisty

Guendelman

2020

Eur. Phys. J. C

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“…where the sub-index 0 means "at present time" and ρ ϕ =φ 2 /2 + V (ϕ) is the energy density of the inflaton field. Numerical calculations performed in [58] show that the value of M depends on the reheating temperature and for a reheating temperature of the order of 100 TeV, which is the one obtained when the reheating is due to the production of superheavy particles [26], one gets M ∼ 18 GeV. Moreover, as we show in Figure 3 the values of the power spectrum and the ratio of tensor to scalar perturbations stand within 2σ confidence level for some given Planck likelihoods but not if we consider all the ones available in the 2018 Planck results [59].…”

Section: Creation Of Superheavy Particles Conformally Coupled To Gravitymentioning

confidence: 99%

Understanding gravitational particle production in quintessential inflation

Haro

Pan

Saló

2019

J. Cosmol. Astropart. Phys.

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The diagonalization method, introduced by a group of Russian scientists at the beginning of seventies, is used to compute the energy density of superheavy massive particles produced due to a sudden phase transition from inflation to kination in quintessential inflation models, the models unifying inflation with quintessence originally proposed by Peebles-Vilenkin. These superheavy particles must decay in lighter ones to form a relativistic plasma, whose energy density will eventually dominate the one of the inflaton field, in order to have a hot universe after inflation. In the present article we show that, in order that the overproduction of Gravitational Waves (GWs) during this phase transition does not disturb the Big Bang Nucleosynthesis (BBN) success, the decay has to be produced after the end of the kination regime, obtaining a maximum reheating temperature in the TeV regime.

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“…As has been shown in Ref. [21] that for a viable model with an exponential tail described in (15), the value of the model parameter γ should belong to the interval (0, √ 2). It is important to realize that a value of γ leading to a scaling solution does not serve for nothing because the real scalar field never enters the basin of attraction of the scaling solution.…”

Section: A Viable Modelmentioning

confidence: 93%

“…On the contrary, in quintessential inflation [10][11][12][13][14][15][16][17][18][19][20][21], there is only one scalar field driving the evolution of the universe by depicting both the early-and late-acceleration of the universe. Due to the attractor behavior of inflation the initial condition of the scalar field has to be taken belonging to the basin of attraction of the slow roll solution.…”

Section: Introductionmentioning

confidence: 99%

Scaling solutions in quintessential inflation

2020

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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.

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The Peebles–Vilenkin quintessential inflation model revisited

Cited by 21 publications

References 81 publications

Quintessential inflation from Lorentzian slow roll

Quintessential inflation from Lorentzian slow roll

Understanding gravitational particle production in quintessential inflation

Scaling solutions in quintessential inflation

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