Reconstructing warm inflation

TL;DR

This paper reconstructs warm inflation models from observable spectral indices and tensor ratios, deriving potential and dissipation functions under different dissipative regimes using a general formalism.

Contribution

It introduces a method to reconstruct warm inflation models from $n_S(N)$ and $r(N)$, providing explicit expressions for potential and dissipation coefficient.

Findings

Reconstructed effective potential $V(\,phi)$ for warm inflation.

Derived dissipation coefficient $\,Gamma(\,phi)$ in different regimes.

Analyzed specific attractor models with $n_S-1 \,propto N^{-1}$ and $r \,propto N^{-2}$.

Abstract

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.