Merger-Induced Cosmogenesis: A Binary Black Hole Bounce as a Mechanism for Cosmological Initial Conditions

Within the framework of black hole cosmology, a number of authors have proposed that the singular interior of a gravitationally collapsed object may be replaced, under appropriate non-classical physics, by a non-singular bounce into a new expanding cosmological phase. Existing proposals (Pathria–Good, Smolin, Popławski, Brandenberger et al.) treat this bounce as a feature of single-body gravitational collapse. We propose a modification of this picture in which the trigger for a successful cosmogenic bounce is not isolated collapse but the merger of two black holes. We argue heuristically that the transient curvature and torsion densities reached during the coalescence of a binary black hole system, particularly in the presence of fermionic matter or vacuum spinor condensates inside one or both horizons, exceed those of a quiescent Kerr interior by several orders of magnitude and may satisfy bounce conditions that single-body collapse cannot generically meet. We sketch the geometry of a merger-interior FLRW patch glued to the external Kerr remnant via an S-brane-like junction surface, identify the parameter regime in which the interior daughter universe acquires near-homogeneity and inflation-compatible expansion, and outline observational signatures (gravitational-wave ringdown anomalies, a preferred axis correlated with parent-merger spin, and shifts in the merger rate of primordial black holes) that distinguish merger-induced cosmogenesis (MIC) from single-collapse variants of black hole cosmology. The proposal is speculative and several derivations are deferred; its purpose is to determine whether a research program along these lines is well-posed.