Exploring the impact of the dissipation coefficient in warm Higgs inflation

In this study, we conduct a detailed analysis of the dissipation coefficient (Q) of warm Higgs inflation (WHI), which exerts important influences on the entire warm inflation process. By deriving the relationships between various quantities and Q, one can avoid a priori assumptions, i.e., strong dissipation (Q >> 1) or weak dissipation (Q << 1). Taking into account the constraints imposed by the cosmic microwave background, the dissipation the coefficient Q remains at extremely low levels throughout the entire warm inflation process, i.e., Q << 1. This observation indicates that WHI falls under the category of weak dissipation warm inflation. Despite being weak dissipation, Q still plays a non-negligible role in the evolution of temperature, energy, and other quantities. We delve into the impact of the primordial power spectrum on the dissipation coefficient Q during the warm inflation process, discovering that the dependency is not significant. Consequently, this results in a weak sensitivity of the gravitational wave spectrum (Omega(GW,0)h(2)) to changes in Q. In addition, the variation of tensor-to-scalar ratio r has a significant effect on the Omega(GW,0)h(2) of cold inflation and a small effect on WHI. Finally, gravitational waves generated by WHI hold the potential for verification in future observational experiments, especially through the SKA100 experiment.