  The well-studied type IIP SN 1987A, produced by the explosion of a blue
supergiant (BSG) star, is a touchstone for massive-star evolution, simulations
of neutrino-driven explosions, and modeling of light curves and spectra. In the
framework of the neutrino-driven mechanism, we study the dependence of
explosion properties on the structure of four different BSGs and compare the
corresponding light curves with observations of SN 1987A. We perform 3D
simulations with the PROMETHEUS code until about one day and map the results to
the 1D code CRAB for the light curve calculations. All of our 3D models with
explosion energies compatible with SN 1987A produce 56Ni in rough agreement
with the amount deduced from fitting the radioactively powered light-curve
tail. One of the progenitors yields maximum velocities of ~3000 km/s for the
bulk of ejected 56Ni, consistent with observations. In all of our models inward
mixing of hydrogen during the 3D evolution leads to minimum H-velocities below
100 km/s, in good agreement with spectral observations. The considered BSG
models, 3D explosion simulations, and light-curve calculations can thus explain
basic observational features of SN 1987A. However, all progenitors have too
large pre-SN radii to reproduce the narrow initial luminosity peak, and the
structure of their outer layers is not suitable to match the observed light
curve during the first 30-40 days. Only one stellar model has a structure of
the He core and the He/H composition interface that enables sufficient outward
mixing of 56Ni and inward mixing of hydrogen to produce a good match of the
dome-like shape of the observed light-curve maximum. But this model falls short
of the He-core mass of 6 Msun inferred from the absolute luminosity of the
pre-SN star. The lack of an adequate pre-SN model for SN 1987A is a pressing
challenge for the theory of massive-star evolution. (Abridged)
