The Cosmic Microwave Background (CMB) temperature and polarization anisotropies,
Large-scale structure (LSS) anisotropies and clustering anomalies,
Cosmic parity violations and hemispherical asymmetries.
1. Theoretical Setup
Each cosmological "layer" (see Section II.2) is treated as a quasi-FRW submanifold embedded in a higher-dimensional meta-spacetime. The field interf(x)\Phi_{\text{interf}}(x) governing inter-layer connectivity is given by the generalized interference term:
interf(x)ein(x)d4x\Phi_{\text{interf}}(x) \sim \int e^{i\theta_n(x)} \, d^4x
where n(x)\theta_n(x) represents the topological phase angle of layer nn, defined via boundary conditions arising from the Blink Genesis. These phases are non-trivially coupled due to the layered geometry, such that:
net(x)=nwn(x)n(x),with nwn(x)=1\theta_{\text{net}}(x) = \sum_n w_n(x) \theta_n(x), \quad \text{with } \sum_n w_n(x) = 1
The interference field manifests in observable space as modulations in the energy density and curvature tensor RR_{\mu\nu}, altering photon geodesics and matter power spectra.
2. Numerical Modeling Approach
2.1. Simulating Layered Phase Fields
Each layer nn is assigned a stochastic topological phase field n(x)\theta_n(x), modeled as:
 n(x)=nPerlin(x)+nquant(x)\theta_n(x) = \alpha_n \cdot \text{Perlin}(x) + \beta_n \cdot \phi_{\text{quant}}(x) where Perlin(x) introduces smooth spatial coherence and quant(x)\phi_{\text{quant}}(x) injects quantum noise.
The relative coupling wn(x)w_n(x) is varied to simulate constructive and destructive interference zones, particularly near layer junctions and void boundaries.
2.2. Propagating Photons Through Interfering Fields
Ray-tracing simulations are employed to model the path of CMB photons through layered structures modulated by interf(x)\Phi_{\text{interf}}(x),
Photon path deflection (x)\delta\theta(x) is computed via perturbative corrections to the geodesic equation:
d2xd2+dxddxd=finterf(x)\frac{d^2x^\mu}{d\lambda^2} + \Gamma^\mu_{\alpha\beta} \frac{dx^\alpha}{d\lambda} \frac{dx^\beta}{d\lambda} = f^\mu_{\text{interf}}(x)
where finterfinterf(x)f^\mu_{\text{interf}} \propto \nabla^\mu \Phi_{\text{interf}}(x)
2.3. Statistical Outputs
