Orbital Adreses and Velocity Predictions for Exoplanet Candidates

AbstractSpace-based transit surveys such as NASA's Transiting Exoplanet Survey Satellite (TESS) detect thousands of periodic photometric dips embedded in stellar light-curve noise, initially yielding only the orbital period (P) without direct radial-velocity measurements of orbital speed (v) or semi-major axis distance (R). Using discrete elastic lattice mechanics, this paper replaces Newtonian mass (M) and the gravitational constant (G) with a single geometric star parameter—the Stellar Passport (P_star = (Rs / 2) * c^2 = 132.716 * 10^9 * k km^3/s^2, scaled from the solar indentation caliber Rs_sun = 2,953.335 m). From the transit period alone, orbital vortex velocity is extracted directly via v = (2 * Pi * P_star / T)^(1/3), and the exact radial cell address is determined via R = P_star / v^2. Step-by-step predictions are presented for eight prominent unconfirmed TESS Objects of Interest (TOI-715.02, L 98-59 f, TOI-270.04, TOI-1452.02, TOI-2095.03, TOI-1266.03, TOI-216.03, and TOI-561.04) alongside three predicted unobserved planets occupying empty resonant lattice cells in the Kepler-11, TRAPPIST-1, and TOI-700 systems.