Abstract
A warm intermediate inflationary model in the context of Generalized Chaplygin Gas is investigated. We study this model in the weak and strong dissipative regimes, considering a generalized form of the dissipative coefficient $\Gamma=\Gamma(T,\phi)$, and we describe the inflationary dynamics in the slow-roll approximation. We find constraints on the parameters in our model considering the Planck 2015 data, together with the condition for warm inflation $T>H$, and the conditions for the weak and strong dissipative regimes.
Highlights
It is well known that in modern cosmology in our understanding of the early Universe there has been introduced a new stage of the Universe, described by the inflationary scenario [1,2,3,4,5,6]
The most important feature of the inflationary scenario is that it provides a novel mechanism to account for the large-scale structure [7,8,9,10,11,12] and it explains the origin of the observed anisotropy of the cosmic microwave background (CMB) radiation [13,14,15]
From the essential condition for warm inflation to occur, T > H, we obtain a lower bound for Cφ, given by Cφ > 3.6 × 10−5, and numerically we find that the values A = 2995, and β = −1.4 correspond to Cφ = 3.6 × 10−5
Summary
It is well known that in modern cosmology in our understanding of the early Universe there has been introduced a new stage of the Universe, described by the inflationary scenario [1,2,3,4,5,6] This early phase solves some of the problems of the standard big bang model, like the flatness, horizon, density of monopoles, etc. A fundamental condition for warm inflation to occur is that the temperature of the thermal bath must satisfy T > H , where H is the Hubble rate Under this condition, the thermal fluctuations play a fundamental role in producing the primordial density fluctuations, indispensable for large-scale structure formation.
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