Black Hole Evaporation Driven by Non-Thermal Squeezing Through SNS and CSNS Dynamics
In this work, we present a comprehensive semiclassical analysis of black hole radiation in a spatially flat FRW Universe for two fundamental nonclassical states: the Squeezed Number State (SNS) and the Coherent Squeezed Number State (CSNS). Unlike thermally modified earlier studies, SNS and CSNS constitute fully non-thermal, number-state-dependent quantum configurations. By embedding these states within the framework of semiclassical theory of gravity, we derive state-resolved expressions for the Hawking temperature, entropy variation, and corresponding mass loss of an evaporating black hole. The influence of the squeezing parameter $ρ$ and number state parameter $n$ on Hawking emission is examined through a series of analytical results supported by twelve detailed plots. The analysis reveals that the Hawking temperature exhibits monotonic growth with increasing $ρ$ and $n$, thereby elevating the effective temperature experienced at the black hole horizon. The entropy variations $Δ\mathbb{S}_{\mathrm{SNS}}$ and $Δ\mathbb{S}_{\mathrm{CSNS}}$ show strong nonlinear enhancement, especially at moderate and large squeezing values. Overall, the study extends earlier thermal squeezed-state approaches to a fully number-state-resolved framework, highlighting the sensitivity of Hawking emission to nonclassical quantum configurations. These findings contribute a new perspective on gravitational particle creation in cosmological settings.