Warm inflation in loop quantum cosmology: a model with a general dissipative coefficient

TL;DR

This paper investigates warm inflation within loop quantum cosmology using a generalized dissipative coefficient, analyzing stability conditions and the impact of temperature dependence on inflationary dynamics and cosmic microwave background signatures.

Contribution

It introduces a generalized form of the dissipative coefficient in warm inflation within loop quantum cosmology and analyzes stability and observational implications.

Findings

Thermal effects are enhanced when the dissipative coefficient depends on temperature.

Quantum effects leave a tiny imprint on the CMB.

Conditions for warm inflation attractors are derived in this framework.

Abstract

A general form of warm inflation with the dissipative coefficient $\Gamma=\Gamma_0(\phi /\phi_0) ^n(T/\tau_0) ^m$ in loop quantum cosmology is studied. In this case, we obtain conditions for the existence of a warm inflationary attractor in the context of loop quantum cosmology by using the method of stability analysis. The two cases when the dissipative coefficient is independent $(m=0)$ and dependent $(m\neq0)$ on temperature are analyzed specifically. In the latter case, we use the new power spectrum which should be used when considering temperature dependence in the dissipative coefficient. We find that the thermal effect is enhanced in the case $m>0$. As in the standard inflation in loop quantum cosmology, we also reach the conclusion that quantum effect leaves a tiny imprint on the cosmic microwave background (CMB) sky.