Disruption tidale (survol de Roche)

A star on a parabolic-like flyby of a black hole is shredded when its periapsis lies inside the Roche (tidal) radius

R_t ≈ R★ (2 M_BH / M★)1/3

(order-of-magnitude fluid estimate). Set black-hole and star masses, stellar radius, and periapsis as a fraction of R_t, then Run. When r < R_t the star is replaced by a particle debris stream: outer material is kicked onto unbound tails, inner material stays more bound and can fall in (counted as accreted). A flare brightens as debris nears the hole.

When to use: intuition for TDEs, comparing R_t to the Schwarzschild radius, and seeing bound vs unbound streams.

Limitations: not hydrodynamics; no relativistic orbits; no self-gravity of the debris; purely educational visualization.