Roche Limits and Tidal Disruption Bounds for Exomoons of Varied Composition

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 jupiter_density_kg_m3 = 1326; fluid_roche_ice_Rp = 2.78; fluid_roche_rock_Rp = 1.86; rigid_roche_rock_Rp = 0.96; synchronous_orbit_note_Rp = 2.24. A moon that ventures too close to its planet is pulled apart by the difference in gravitational attraction across its own diameter. The Roche limit marks that boundary, and it is the inner counterpart of the Hill stability limit: together they bracket the annulus in which a moon can exist at all. Because the limit depends on the density ratio of planet and moon, it is also a composition diagnostic 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.