Tidal Disruption
Compare tidal radius, flyby and idealised stellar fallback around a black hole.
About this tool
Choose a stellar example or custom values and Calculate. M☉ and R☉ mean solar masses and radii. r_p/R_t sets closest approach relative to the tidal radius; β = R_t/r_p is penetration. Both axes in the radii view use the same scale. The enlarged yellow marker shows pericentre, not the star at its true size. Reset restores the solar example and radii view, and clears results without calculating again.
Estimate, not a destruction simulation: R_t = R★(M_BH/M★)¹ᐟ³ uses the standard TDE convention. Its coefficient actually depends on stellar structure, spin and encounter duration. It is neither a guaranteed full-disruption boundary nor a circular-orbit Roche limit. The blue reference orbit is Newtonian and parabolic; it is hidden for r_p ≤ 10 r_s. This conservative model limit is not an exact capture boundary. The hole is nonrotating.
Fallback: Only r_p ≤ R_t and r_p > 10 r_s show estimates assuming full disruption. Δε = GM_BH R★/R_t², t_min = 2πGM_BH/(2Δε)³ᐟ² and Ṁ = M★/(3t_min)(t/t_min)⁻⁵ᐟ³ assume a parabolic encounter and uniform debris-energy distribution. Energy freezes at R_t, so pericentre does not change this idealised curve. It predicts neither accretion rate nor light curve, debris hydrodynamics or certain survival.
Mass at R_t = r_s is a rough Schwarzschild radius equality, not an exact Hills/capture threshold; relativistic effects and hole spin are absent. Independent stellar inputs are not validated as a realistic stellar-evolution model. Hole mass must exceed stellar mass by at least 1000. 3D shows the same radii without arbitrary particle motion; calculations and charts work without WebGL.