2018/06/30 by Athira Menon, В. П. Утробин, Victor Utrobin +1
Physics and Astronomy · #Astrophysical Phenomena and Observations #Astrophysics #Binary number #Ejecta #Gamma-ray bursts and supernovae #Light curve #Physics #Pulsars and Gravitational Waves Research #RADIUS #Red supergiant #Star (game theory) #Stars #Stellar evolution #Supergiant #Supernova #Type (biology) #astro-ph.HE #astro-ph.SR
paper · pdf · doi:10.1093/mnras/sty2647
17 pages, 11 figures, 3 tables, accepted by MNRAS
arxiv created 2018/09/24 · openalex publication_date 2018/10/01 · arxiv updated 2018/10/17 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Based on the work of Menon & Heger, 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 R_\odot |, an ejecta mass of |20.6 M_\odot |, an explosion energy of |1.7× 1051 | erg, a nickel mass of |0.073 M_\odot |, and a nickel mixing velocity of |3 000 km 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 R_\odot | and ejecta mass of |19.1 M_\odot | matches the light curve. These parameters are significantly higher than predictions from semi-analytic models for the progenitor of this supernova.