Solve the modified Friedmann equation with the local i\rho_i and entangled interlayer terms,
Extract H(r)H(r), a(r)a(r), and corresponding deceleration parameter q(r)q(r),
Perform comparative runs with and without the topological interference term to isolate its effect.
4. Results: Profile of H(r)H(r)
Key simulation outputs:
H(r)H(r) shows oscillatory modulation around a baseline Hubble expansion curve. These modulations arise naturally from topological phase coupling.
The outer layers (void-dominated) exhibit slower expansion rates, consistent with underdense shell slowing, while denser interior layers evolve more rapidly.
The effective H0H_0 extracted from inner regions (e.g., SN Ia-like observers) is higher than the average expansion inferred from outer layers (e.g., CMB), offering a natural resolution to the Hubble tension.
5. Comparison with Observations
Thus, the model's emergent radial-dependence in H(r)H(r) may help reconcile disparate cosmological distance ladders without introducing new scalar fields or dark sector components.
6. Next Steps
