On the thermodynamic origin of the initial radiation energy density in warm inflation

Abstract

In warm inflation scenarios, radiation always exists, so that the radiation energy density is also assumed to be finite when inflation starts. To find out the origin of the non-vanishing initial radiation energy density, we revisit thermodynamic analysis for a warm inflation model and then derive an effective Stefan-Boltzmann law which is commensurate with the temperature-dependent effective potential by taking into account the non-vanishing trace of the total energy-momentum tensors. The effective Stefan-Boltzmann law shows that the zero energy density for radiation at the Grand Unification epoch increases until the inflation starts and it becomes eventually finite at the initial stage of warm inflation. By using the above effective Stefan-Boltzmann law, we also study the cosmological scalar perturbation, and obtain the sufficient radiation energy density in order for GUT baryogenesis at the end of inflation.

arXiv comment17 pages, 1 figure, version to appear in JCAP

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• Gravitational wave from warm inflation
• Observational constraints on warm quasi-exponential inflation
• Proper temperature of Schwarzschild AdS black hole revisited
• Gravitational baryogenesis in non-minimal kinetic coupling model
• Spectra and entropy of multi-field warm inflation
• The effective Tolman temperature in curved spacetimes
• On thermal radiation of de Sitter space in the semiclassical Jackiw-Teitelboim model
• Warm inflation in Weyl geometric gravity