Numerical Predictions for Inflation in the Order Parameter Spacetime Theory — Spectral Index, Tensor-to-Scalar Ratio, and Reheating

Based on the exact cosmological solution of the Order Parameter Spacetime Theory — the critical condition (1-c₁)·3H²=0 — this paper presents systematic numerical predictions for inflationary observables. By coupling the dissipative geodesic equation with the modified Friedmann equation, the evolution equation for the feedback coefficient c₁(t) is derived. On this basis, the modified Mukhanov-Sasaki equation is solved, and the spectral index n_s and its running α_s of the primordial scalar power spectrum are computed. The evolution of tensor perturbations in the critical phase is derived, yielding the information-dissipation correction to the tensor-to-scalar ratio r. The contribution to the non-Gaussianity parameter f_NL is analyzed. Furthermore, a unified scaling relation between the reheating temperature T_reheat and the number of e-folds N_e is established, unifying both under the relaxation time τ of the Type-B singularity. Within a reasonable parameter range, we obtain n_s ≈ 0.965, r ∼ 10⁻³, f_NL ∼ O(10⁻⁴), and T_reheat ∼ 10¹⁵ GeV, all consistent with current observations. The numerical framework depends only on the ratio of the relaxation time of the order-parameter field to the Hubble time, without requiring an inflaton field or a finely tuned potential form.