Black Hole Entropy Without Singularities

In classical general relativity, black holes are characterized by singularities where curvature diverges, and entropy is described by the Bekenstein-Hawking formula. However, quantum gravity effects are expected to resolve these singularities. This paper presents a ghost-free mechanism for black hole entropy and singularity resolution within the Spectral Nod Gravity (SNG) framework. Spacetime emerges from discrete Planck-scale nod networks, where entropy arises from nod entanglement. Upon reaching maximal nod density, the system undergoes topological reconfiguration via cyclic equivalence operator (\( \ceq \)), capping entropy at \( S_{\rm BH} \fleq \frac{A_{\rm horizon}}{4 \ell_p^2} \langle \hat{\mathcal{F}}(\Omega) \rangle_{\rm BH} \). This recovers the Bekenstein-Hawking formula as an emergent limit while eliminating classical singularities through finite nod density and resets. Black holes function as entropic phase boundaries, with the Cosmic Grinder redistributing infalling matter into spectral layers, preserving information continuity.