Abstract
With the same method as used previously, we investigate neutrino-driven explosions of a larger sample of blue supergiant models. The blue supergiants were evolved as single-star progenitors. The larger sample includes three new presupernova stars. The results are compared with light-curve observations of the peculiar type IIP supernova 1987A (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, starting at a stage of nearly homologous expansion. Our results confirm the basic findings of the previous work: 3D neutrino-driven explosions with SN 1987A-like energies synthesize an amount of 56Ni that is consistent with the radioactive tail of the light curve. Moreover, the models mix hydrogen inward to minimum velocities below 400 km s−1 as required by spectral observations and a 3D analysis of molecular hydrogen in SN 1987A. 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 56Ni 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−1 for the bulk of ejected 56Ni, but failed to reproduce the helium-core mass of 6 M⊙ 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.
Highlights
The explosion of the blue supergiant (BSG) Sanduleak −69◦202 in the Large Magellanic Cloud (LMC) as the peculiar type II plateau supernova (SN) 1987A stimulated activity in its observation from radio wavelengths to gamma rays, and the further development in the theory of the evolution of massive stars, the simulation of explosion mechanisms, and the modeling of light curves and spectra
Performing 3D neutrino-driven explosion simulations and subsequent light curve modeling, we compared the results with the observations of SN 1987A and draw the following main conclusions:
– The initial 56Ni masses required to match the observations of the radioactive tail of SN 1987A fall in between the minimum and maximum estimates obtained in our 3D explosion models, implying that all 3D neutrino-driven simulations under study are able to synthesize the ejected amount of radioactive 56Ni for explosion energies in the general range of what is needed to explain the observed light curve
Summary
The explosion of the blue supergiant (BSG) Sanduleak −69◦202 in the Large Magellanic Cloud (LMC) as the peculiar type II plateau supernova (SN) 1987A stimulated activity in its observation from radio wavelengths to gamma rays, and the further development in the theory of the evolution of massive stars, the simulation of explosion mechanisms, and the modeling of light curves and spectra. Kifonidis et al (2006) and Wongwathanarat et al (2015) found that the amount of outward 56Ni mixing and inward hydrogen mixing is sensitive to the structure of the helium core and the He/H composition interface Using this sensitivity, Utrobin et al (2015) studied the dependence of explosion properties on the structure of four BSG progenitors for the first time in the framework of the neutrinodriven explosion mechanism. In Appendix A we discuss the role of 3D macroscopic mixing in light-curve modeling of ordinary and peculiar type IIP SNe
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