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.

17 pages, 1 figure, version to appear in JCAP

References in corpus (6)

• Reheating in Inflationary Cosmology: Theory and Applications
• Nonperturbative Dynamics Of Reheating After Inflation: A Review
• Warm Inflation and its Microphysical Basis
• Reheating temperature from the CMB
• Tachyon warm inflationary universe models
• Observational implications of mattergenesis during inflation

Cited by in corpus (6)

• The warm inflation story
• Gravitational baryogenesis in non-minimal kinetic coupling model
• Spectra and entropy of multi-field warm inflation
• The effective Tolman temperature in curved spacetimes
• Warm inflation in Weyl geometric gravity
• On thermal radiation of de Sitter space in the semiclassical Jackiw-Teitelboim model