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With the same method as used previously, we investigate neutrino-drivenexplosions of a larger sample of blue supergiant models. The larger sampleincludes three new presupernova stars. The results are compared withlight-curve observations of the peculiar type IIP SN 1987A. The explosions weremodeled in 3D with the neutrino-hydrodynamics code PROMETHEUS-HOTB, andlight-curve calculations were performed in spherical symmetry with theradiation-hydrodynamics code CRAB. Our results confirm the basic findings ofthe previous work: 3D neutrino-driven explosions with SN 1987A-like energiessynthesize an amount of Ni-56 that is consistent with the radioactive tail ofthe light curve. Moreover, the models mix hydrogen inward to minimum velocitiesbelow 400 km/s as required by spectral observations. Hydrodynamic simulationswith the new progenitor models, which possess smaller radii than the olderones, show much better agreement between calculated and observed light curvesin the initial luminosity peak and during the first 20 days. A set ofexplosions with similar energies demonstrated that a high growth factor ofRayleigh-Taylor instabilities at the (C+O)/He composition interface combinedwith a weak interaction of fast Rayleigh-Taylor plumes, where the reverse shockoccurs below the He/H interface, provides a sufficient condition for efficientoutward mixing of Ni-56 into the hydrogen envelope. This condition is realizedto the required extent only in one of the older stellar models, which yielded amaximum velocity of around 3000 km/s for the bulk of ejected Ni-56, but failedto reproduce the helium-core mass of 6 Msun inferred from the absoluteluminosity of the presupernova star. We conclude that none of the single-starprogenitor models proposed for SN 1987A to date satisfies all constraints setby observations. (Abridged)

Three-dimensional mixing and light curves: constraints on the progenitor of supernova 1987A