The Flatness Problem Through the Aldred Bounce: Bookkeeping of the Curvature Fraction Across Contraction and Expansion

In standard expanding cosmology the curvature fraction |Omega - 1| grows with time, so the present bound |Omega_0 - 1| <= 0.005 requires the early universe to have been flat to an extreme precision. In Einstein-Cartan spin-torsion gravity the universe instead reaches a maximum density and bounces: the Aldred Limit, rho_A = 9.72e54 g/cm^3, with a companion bound placing spectrum generation at a bounce density rho_b <= 2.77e54 g/cm^3. This paper does the bookkeeping of the curvature fraction through such a bounce, by numerical integration of the Friedmann equations in the variable eps = |Omega - 1|/Omega. The expanding branch alone grows eps by 1.86e40 between a bounce at rho_b = 2.77e54 g/cm^3 and today, so a purely expanding history needs eps = 2.69e-43 at that density (42.6 orders below unity). A radiation-filled contraction from the equality density to the bounce removes 36.6 orders, leaving eps_start <= 1.18e-6; a stiff (w = 1) contraction over the same range removes 48.9 orders and saturates the bookkeeping; a matter-filled contraction removes 24.4. Complete removal requires a density range of 10^85.1 (radiation) or 10^63.9 (stiff). The frame fixes the bounce density but not the duration, starting density, or content of the contracting branch, and those unsupplied quantities decide how much of the flatness problem is removed; the bounce alone does not solve it. AI-use disclosure: this paper was prepared with the assistance of Dave, an AI system built and operated by Aldred Industries. The author reviewed the results and takes responsibility for the content. Version note (correction): The first version of this paper used the bounce-density figure supplied by the spectrum bound (DOI 10.5281/zenodo.24102289) without stating its conditional status. This version labels that figure wherever it is used as conditional on the prescription of the spectrum bound: Deruelle-Mukhanov transfer with the curvature perturbation conserved across the bounce surface, generation of the spectrum at the bounce density, and the single-component density identification used in that paper. The Einstein-Cartan background alone supplies rho_A = 9.72 x 10^54 g/cm^3, not this bound. No result, number, or conclusion has changed.