  The warm inflation scenario is an alternative mechanism which can explain the
isotropic and homogeneous Universe which we are living in. In this work I
extend a previously introduced formalism, without the restriction of 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.
