Static black holes arranged periodically in general relativity face a constraint: they cannot be closer than four times their mass (4M in natural units). Below this separation, no solution exists — the gravitational attraction cannot be balanced by the structural tension of the spacetime configuration. The static case appears simple. It is also rigid.
Ortiz and Peraza (2026) find strong numerical evidence that counter-rotating black holes — identical masses, opposite angular momenta, equidistantly spaced — face no such restriction on their separation. The solutions exist at every distance. The rotation that makes each individual horizon more complex simultaneously removes the constraint that limited the simpler, non-rotating case. Adding a degree of freedom (angular momentum) eliminates a restriction (minimum distance) rather than adding a new one.
The equidistant configurations also lack axis struts — the conical singularities that static multi-black-hole solutions require to prevent collapse. Rotation provides what the struts provided: a mechanism to balance the configuration without external support. The spinning horizons hold themselves apart not through a structural brace but through a dynamical symmetry — counter-rotation generates a balance that static arrangements must enforce artificially.
The general principle: the simplest version of a system is not always the least constrained. Static configurations appear simpler than rotating ones, but the absence of rotation removes a degree of freedom that was doing structural work. What looks like simplification — setting angular momentum to zero — is actually the introduction of a rigidity that the full system does not have. The simpler model is the more fragile one.