Black Hole Evaporation Driven by Non-Thermal Squeezing Through SNS and CSNS Dynamics

TL;DR

This paper develops a semiclassical gravity framework to study Hawking radiation in a spatially flat FRW universe with quantized inflaton fields prepared in nonclassical SNS and CSNS states. By embedding SNS/CSNS into the SCTG formalism, the authors derive state-resolved expressions for the Hawking temperature, entropy variation, and black hole mass loss, explicitly showing how the squeezing parameter $\rho$, number state $n$, and displacement $\varUpsilon$ control the radiation. Key results include monotonic increases of $T_{\mathbb{H}}$ with $\rho$ and $n$, nonlinear growth of entropy variations, and enhanced mass loss, with CSNS producing stronger effects due to coherent displacement. These findings extend thermal squeezed-state analyses to a fully nonthermal, number-state-resolved description of gravitational particle creation, offering new insights into black hole thermodynamics in cosmological settings.

Abstract

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.

Figures (12)

• Figure 1: 3D plot for Hawking temperature ${\mathbb{T}}_{{\mathbb{H}}_{SNS}}$ with $n$ and $\rho$
• Figure 2: 2D plot for Hawking temperature ${\mathbb{T}}_{{\mathbb{H}}_{SNS}}$ with $\rho$, for different values of $n$.
• Figure 3: 3D plot for Hawking temperature ${\mathbb{T}}_{{\mathbb{H}}_{CSNS}}$ with $n$ and $\rho$
• Figure 4: 2D plot for Hawking temperature ${\mathbb{T}}_{{\mathbb{H}}_{CSNS}}$ with $\rho$, for different values of $n$.
• Figure 5: 3D Plot for $\Delta {\mathbb{S}}_{SNS}$ with number state parameter ($n$) and squeezing parameter ($\rho$).