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