Based on the work of Menon and Heger ( 2017 ) , we present the bolometric light curves and 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 Kepler and 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 \mathrm { R } _ { \odot } , an ejecta mass of 20.6 \mathrm { M } _ { \odot } , an explosion energy of 1.7 \times 10 ^ { 51 } erg , a nickel mass of 0.073 \mathrm { M } _ { \odot } , and a nickel mixing velocity of 3 , 000 { \mathrm { km } \mathrm { s } ^ { -1 } } .
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 \mathrm { R } _ { \odot } and ejecta mass of 19.1 \mathrm { M } _ { \odot } matches the light curve .
These parameters are significantly higher than predictions from semi-analytic models for the progenitor of this supernova .