Towards a theory of warm inflation of the Universe

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Abstract
The warm inflation scenario is an alternative mechanism which can explain the isotropic and homogeneous Universe in which we are living. In this work I extend a previously introduced formalism, without the restriction of the slow-roll regime. Quantum to classical transition of the fluctuations is studied by means of the `transition function' here introduced. I found that the fluctuations of radiation energy density decrease with time and the thermal equilibrium at the end of inflation holds.
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