Spacetime Rigidity and the Resolution of Black Hole Singularities

We apply the principle of spacetime rigidity, formulated as an upper bound on curvature invariants, to the physics of black holes. In the standard Schwarzschild solution, curvature invariants diverge at r=0, signaling the classical singularity. Rigidity prevents such divergences: the Kretschmann scalar saturates at the Planck scale, replacing the singularity with a finite core. We analyze the implications for horizon structure, entropy scaling, and the possible universality of the suppression factor ~10−123. The comparison with cosmology shows both similarities and differences: while the number 10−123 is universal in cosmology, for black holes it emerges only in the extreme case where the horizon radius is comparable to the Hubble scale. We show that the core of a black hole and the core of the Big Bang are structurally equivalent: when the informational capacity of the core is saturated, Heisenberg’s uncertainty principle forbids static confinement, enforcing a bounce into a white hole phase. This perspective unifies black hole physics with cosmogenesis.