Hawking Radiation as an Indirect Consequence of Absorbed Photons
Abstract
Abstract This paper explores whether the energy deposited by previously absorbed photons can leave a weak, state-dependent imprint on Hawking emission. While infalling photons do not re-emerge, their absorbed energy changes the black hole parameters and can transiently perturb near-horizon quantum correlations that govern semiclassical particle creation. Using a quantum optics–inspired open-system framework, we parameterize this history dependence through small modifications of mode mixing (Bogoliubov coefficients) and introduce an additional vacuum-mediated entropy contribution ΔS vac that supplements the standard Bekenstein–Hawking term in an effective description. We find that, in this parameterization, the resulting occupation numbers can deviate slightly from an exactly thermal spectrum, with the size of the effect controlled by the absorbed energy scale relative to M and the assumed correlation/relaxation timescale. We discuss limiting cases in which the correction is negligible (rapid Markovian relaxation) versus potentially long lived (non-Markovian correlations or squeezing near the horizon), and we outline how analogous correlation signatures could be sought in laboratory analogue-horizon systems. The aim is not to introduce a new microscopic theory of black-hole evaporation, but to construct a mathematically explicit phenomenological bridge between semiclassical Hawking radiation, quantum-optical open system methods, and non-Markovian correlation dynamics.
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