Bolometric light curves of models B15-2 (blue line), N20-P (green line), W18 (magenta line), and W20 (red line) for the late-time 1D simulations compared with the observations of SN 1987A obtained by Catchpole et al. (1987, 1988) (open circles) and Hamuy et al. (1988) (open triangles). In all models the total ⁵⁶Ni mass is scaled to fit the observed luminosity in the radioactive tail (see Table 4). In contrast, the black line shows the bolometric light curve of an optimal model with a nonevolutionary pre-SN (Utrobin 2005, see also Fig. 1).