Luminosities of full disruptions with stellar masses M_* = 0.1, 0.3, 0.5, 1, 3, 10, 30 M_⊙ as functions of M_BH. Solid lines are calculated using the single power-law mass–radius relation, and dashed lines are calculated from the modified one. Also shown are the curves of luminosity our model would predict for R_T = 6r_g and R_T = 4r_g; extreme TDEs occur when 4r_g < r_p < 6r_g (T. Ryu et al. 2023a); direct capture ensues when r_p < 4r_g (an exact result for Schwarzschild spacetime, the angle-averaged result for Kerr; J. Krolik et al. 2020). The luminosities of partial disruptions of a given M_* form a family lying below the curve for a full disruption of such a star.