Speaker
Description
In this study, we explore the evolution of a system composed of an unstable scalar field ($\phi$), and radiation in the context of non-standard cosmology where initially the Universe is dominated by the energy density of $\phi$. Later, the unstable $\phi$ with decay width $\Gamma_\phi$ decays into radiation and we focus on two relevant quantities: the maximum radiation temperature $T_{max}$ and the temperature when the universe is dominated by the radiation (reheating temperature) $T_{RH}$. For a given universe's initial Hubble scale ($H_I$) we compare our numerical results from the Boltzmann equations with approximate results in two regimes: $H_I > \Gamma_\phi$ and $H_I < \Gamma_\phi$. Building upon our understanding of the system’s evolution during reheating, we further discuss the viability of Baryogenesis in this scenario.
