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Six binary-merger progenitors of Supernova 1987A (SN 1987A) with propertiesclose to those of the blue supergiant Sanduleak -69 202 are exploded byneutrino heating and evolved until long after shock breakout in threedimensions (3D), and continued for light-curve calculations in sphericalsymmetry. Our results confirm previous findings for single-star progenitors:(1) 3D neutrino-driven explosions with SN 1987A-like energies synthesize Ni-56masses consistent with the radioactive light-curve tail; (2) hydrodynamicmodels mix hydrogen inward to minimum velocities below 40 km/s compatible withspectral observations of SN 1987A; and (3) for given explosion energy theefficiency of outward radioactive Ni-56 mixing depends mainly on high growthfactors of Rayleigh-Taylor instabilities at the (C+O)/He and He/H compositioninterfaces and a weak interaction of fast plumes with the reverse shockoccurring below the He/H interface. All binary-merger models possesspresupernova radii matching the photometric radius of Sanduleak -69 202 and astructure of the outer layers allowing them to reproduce the observed initialluminosity peak in the first about 7 days. Models that mix about 0.5 Msun ofhydrogen into the He-shell and exhibit strong outward mixing of Ni-56 withmaximum velocities exceeding the 3000 km/s observed for the bulk of ejectedNi-56 have light-curve shapes in good agreement with the dome of the SN 1987Alight curve. A comparative analysis of the best representatives of our 3Dneutrino-driven explosion models of SN 1987A based on single-star andbinary-merger progenitors reveals that only one binary model fulfills allobservational constraints, except one.

Supernova 1987A: 3D Mixing and light curves for explosion models based on binary-merger progenitors