Numerically determine perturbation effects beyond the analytic approximation

Determine numerically the cosmological-perturbation dynamics and inflationary observables for the non-minimally coupled warm-inflation model when temperature-dependent dissipation coefficients and higher-order slow-roll effects are included, thereby characterizing the resulting running of spectral indices and non-Gaussianity.

Background

The analytic scalar power spectrum derived in the paper assumes a temperature-independent dissipation coefficient, negligible metric perturbations, and zeroth order in the slow-roll parameters. For temperature-dependent dissipation, the perturbation equations become coupled and generally require numerical treatment.

The authors note that the modified-gravity factor in the effective dissipation coefficient can produce field dependence not captured by standard power-law parametrizations. A more complete numerical analysis is therefore needed to determine the associated corrections and to compute higher-order observables, including the running of spectral indices and non-Gaussianity.