Abstract
The intermediate, logamediate and exponential inflationary models in the context of Galileon inflation or G-inflation are studied. By assuming a coupling of the form G(phi ,X)propto phi ^{nu },X^{n} in the action, we obtain different analytical solutions from the background cosmological perturbations assuming the slow-roll approximation. General conditions required for these models of G-inflation to be realizable are determined and discussed. In general, we analyze the condition of inflation and also we use recent astronomical and cosmological observations for constraining the parameters appearing in these G-inflationary models.
Highlights
On the other hand, in the context of exact inflationary solutions, one of the more interesting are found by using an exponential potential for the inflaton, yielding a power-law evolution of the scale factor in cosmic time, i.e., a(t) ∝ t p, where p > 1 [23]
From BICEP2/Keck-Array results data that the ratio r < 0.07, we find a lower bound for the power n given by n > 61912(1 − f )2(1 − ns)2/(2 − 3 f
From BICEP2/Keck-Array data, we have that r < 0.07, we find a lower bound for the power n, given by n > 15480(1 − ns
Summary
In the context of exact inflationary solutions, one of the more interesting are found by using an exponential potential for the inflaton, yielding a power-law evolution of the scale factor in cosmic time, i.e., a(t) ∝ t p, where p > 1 [23]. Note that for the special case λ = 1 and B = p, the logamediate inflation model reduces to powerlaw inflation with an exponential potential [23] These inflationary models were studied as exact solutions of background evolution. [64], the authors explored the viability of considering the intermediate inflation model in the framework of G-inflation, with a cubic Galileon term of the form G(φ, X ) φ ∝ X n φ It was found the compatibility of this model with Planck 2015 data. The main goal of the present article is to explore the observational consequences of studying the intermediate, logamediate and exponential Hubble inflation models in the framework of the cubic Galileon and how these models are modified with the coupling G(φ, X ).
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