Reconstructing warm inflation
  The reconstruction of a warm inflationary universe model from the scalar
spectral index $n_S(N)$ and the tensor to scalar ratio $r(N)$ as a function of
the number of e-folds $N$ is studied. Under a general formalism we find the
effective potential and the dissipative coefficient in terms of the
cosmological parameters $n_S$ and $r$ considering the weak and strong
dissipative stages under the slow roll approximation. As a specific example, we
study the attractors for the index $n_S$ given by $n_{S}-1\propto N^{-1}$ and
for the ratio $r\propto N^{-2}$, in order to reconstruct the model of warm
inflation. Here, expressions for the effective potential $V(\phi)$ and the
dissipation coefficient $\Gamma(\phi)$ are obtained.
