Abstract

Classical general relativity presents a profound temporal paradox: black holes form instantly for an infalling observer, yet appear to freeze eternally for a distant one. I propose a semi-classical framework where, from the distant observer's viewpoint, black holes emerge asymptotically over cosmological timescales, driven by quantum effects near the horizon. My model introduces a minimal Planck-scale correction of order $\lp^2/r^2$ into standard black hole metrics, regularising the central singularity and defining a quasi-static horizon boundary. I show that the coordinate time required for a self-gravitating body to collapse to this boundary ($T_\mathrm{form}$) is governed by quantum dissipation, intrinsically linked to Hawking radiation. This yields a formation timescale ($T_\mathrm{form} \propto M^3$) that parametrically matches the Hawking evaporation time ($T_\mathrm{evap}$). Formalising this through a quantum field theory (QFT)-derived interaction Hamiltonian ($H_{\text{int}}$) that couples near-horizon and asymptotic modes, I establish a dynamic temporal entanglement. This framework presents black holes as unitary, singularity-free macroscopic quantum systems, thereby resolving the frozen-star, singularity, and information-loss paradoxes. I demonstrate the model's generality by extending it to Schwarzschild, Kerr, and Reissner-Nordström black holes, and ultimately situate it within the paradigm of gravity as emergent thermodynamics.