Abstract
We present the computation of the full system of Boltzmann equations at second orderdescribing the evolution of the photon, baryon and cold dark matter fluids. These equationsallow one to follow the time evolution of the cosmic microwave background anisotropies atsecond order at all angular scales from the early epoch, when the cosmologicalperturbations were generated, to the present, through the recombination era. Thispaper sets the stage for the computation of the full second-order radiation transferfunction at all scales and for a generic set of initial conditions specifying the level ofprimordial non-Gaussianity. In a companion paper, we will present the computation ofthe three-point correlation function at recombination which is very relevant forthe issue of non-Gaussianity in the cosmic microwave background anisotropies.
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