Explosions of blue supergiants from binary mergers for SN 1987A

Athira Menon, Victor Utrobin, Alexander Heger

Research output: Contribution to journalArticleResearchpeer-review

Abstract

Based on thework 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 heliumcore 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 37R, an ejecta mass of 20.6M, an explosion energy of 1.7 × 1051 erg, a nickel mass of 0.073M, and a nickel mixing velocity of 3000 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 150R and ejecta mass of 19.1M matches the light curve. These parameters are significantly higher than predictions from semi-analytic models for the progenitor of this supernova.

Original languageEnglish
Pages (from-to)438-452
Number of pages15
JournalMonthly Notices of the Royal Astronomical Society
Volume482
Issue number1
DOIs
Publication statusPublished - 1 Jan 2019

Keywords

  • Binaries: general
  • Methods: numerical
  • SN 1998A
  • SN 2006V
  • Stars: evolution
  • Supergiants
  • Supernovae: general
  • Supernovae: individual: SN 1987A

Cite this

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title = "Explosions of blue supergiants from binary mergers for SN 1987A",
abstract = "Based on thework 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 heliumcore 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 37R⊙, an ejecta mass of 20.6M⊙, an explosion energy of 1.7 × 1051 erg, a nickel mass of 0.073M⊙, and a nickel mixing velocity of 3000 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 150R⊙ and ejecta mass of 19.1M⊙ matches the light curve. These parameters are significantly higher than predictions from semi-analytic models for the progenitor of this supernova.",
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Explosions of blue supergiants from binary mergers for SN 1987A. / Menon, Athira; Utrobin, Victor; Heger, Alexander.

In: Monthly Notices of the Royal Astronomical Society, Vol. 482, No. 1, 01.01.2019, p. 438-452.

Research output: Contribution to journalArticleResearchpeer-review

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AB - Based on thework 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 heliumcore 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 37R⊙, an ejecta mass of 20.6M⊙, an explosion energy of 1.7 × 1051 erg, a nickel mass of 0.073M⊙, and a nickel mixing velocity of 3000 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 150R⊙ and ejecta mass of 19.1M⊙ matches the light curve. These parameters are significantly higher than predictions from semi-analytic models for the progenitor of this supernova.

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