Towards a theory of warm inflation of the Universe

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.