Solar Perturbations and Closed Vector Tidal Feedback in Retrograde Earth–Moon Spin Reversal

An imposed retrograde Earth satellite can brake terrestrial rotation in an isolated tidal model, but solar perturbations and a consistent vector budget must be assessed before interpreting that model as a physical reversal route. This paper audits the Gate-3C–3F solar-dynamical layer of the Impact-Triggered Lunar Angular-Momentum Reversal programme. A solar–quadrupole secular screen, finite-mass Newtonian three-body windows, an adiabatic path diagnostic and a reset-ensemble vector tidal pilot are reproduced. The observed-quadrupole Laplace scale is 53582.317 km, well inside the approximately 217000 km eccentric reference corridor. Independent IAS15 controls confirm substantial eccentricity excitation near 140 degrees inclination and an osculating Roche-threshold crossing in the 110-degree control. The stitched 145-degree path has a minimum sampled pericenter of 156343.811 km across 72 windows, but these windows do not establish continuous survival. The documented coarse vector pilot reproduces an ecliptic spin-component crossing at 1.053350 Gyr and 217830.928 km. New explicit-grid calculations show that halving the fast timestep changes the crossing time by about 4.8–4.9 percent; further refinement changes it by another 1.08 percent. The spin retains approximately 11 percent of its initial magnitude at these projection crossings. Although the instantaneous terrestrial tidal torque satisfies the full-vector angular-momentum identity, the reset ensemble does not transport conservative solar-plane evolution or close the representative slow-state budget. Its accumulated discrepancy is approximately 0.305–0.310 terrestrial initial-spin units. The release therefore supports finite-window dynamical diagnostics and a falsifiable closure architecture, rather than a converged gigayear Sun–Earth–Moon reversal solution. No collision-generated reservoir, hydrodynamic survival result or reversal of the actual Earth is demonstrated.