Orbital and Formation Budget for the Kepler-1708 b Exomoon Candidate and Its Follow-Up Requirements

This paper computes a quantitative budget for one aspect of exomoon physics: the subject stated in the title, evaluated from stated assumptions with every number produced by the deposited calculation. Headline results are hill_radius_Rp = 262; separation_fraction_Hill = 0.046; moon_period_days = 4.17; moon_mass_earth = 12.8; mass_ratio_percent = 4.01; moon_depth_ppm = 452. The candidate satellite of Kepler-1708 b, a cool Jupiter on a two-year orbit, is in several respects the opposite of the warmer, more massive Kepler-1625 system: the proposed moon is a super-Earth-sized body, a few Earth radii across, orbiting close to its planet at roughly a dozen planetary radii. A close, comparatively small moon stresses different parts of the physical budget. Stability is triv The results are compared with published Solar System values and with the constraints attached to reported exomoon candidates where those apply, and the conditions under which the computed budget would change are stated explicitly. Computed from stated assumptions, not measured.