  Based on the work of Menon & Heger (2017), we present the bolometric light
curvesand spectra of the explosions of blue supergiant progenitors from binary
mergers. We study SN 1987A and two other peculiar Type IIP supernovae: SN 1998A
and SN 2006V. The progenitor models were produced using the stellar evolution
code Keplerand then exploded using the 1D radiation hydrodynamic code Crab. The
explosions of binary merger models exhibit an overall better fit to the light
curve of SN 1987A than previous single star models, because of their lower
helium-core masses, larger envelope masses, and smaller radii. The merger model
that best matches the observational constraints of the progenitor of SN 1987A
and the light curve is a model with a radius of 37 solar radii, an ejecta mass
of 20.6 solar masses, an explosion energy of 1.7 Bethe, a nickel mass of 0.073
solar masses, and a nickel mixing velocity of 3,000 km/s. This model also works
for SN 1998A and is comparable with earlier estimates from semi-analytic
models. In the case of SN 2006V, however, a model with a radius of 150 solar
radii and ejecta mass of 19.1 solar masses matches the light curve. These
parameters are significantly higher than predictions from semi-analytic models
for the progenitor of this supernova.
