Reconstructing warm inflation

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 $V(\varphi )$ and the dissipation coefficient $\Gamma (\varphi )$ are obtained.

Tensor to scalar ratio was given incorrect in previous version. Update here

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Cited by in corpus (15)

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• Dynamical and observational constraints on the Warm Little Inflaton scenario
• Reconstructing inflation in scalar-torsion $f(T,\varphi )$ gravity
• Identifying Universality in Warm Inflation
• Irreversible thermodynamical description of warm inflationary cosmological models
• Unifying Inflation with early and late Dark Energy in Multi-Fields: Spontaneously broken scale invariant TMT
• Reconstructing G-inflation: From the attractors $n_S(N)$ and $r(N)$
• Reconstructing k-essence: Unifying the attractor $n_S(N)$ and the swampland criteria
• Dynamic analysis of noncanonical warm inflation
• Reconstructing Mimetic Cosmology
• Warm inflation with non-comoving scalar field and radiation fluid
• Observational constraints on warm quasi-exponential inflation
• G-Warm inflation: Intermediate model
• Is warm inflation quasi-stable?