Abstract
Recently a new progenitor model for SN 1987A has been constructed. This progenitor model is based on a slow-merger of 14 M⊙ and 9 M⊙ stars and it satisfies most of the observational constraints such as red-toblue evolution, lifetime, total mass and position in the Hertzsprung-Russell diagram at collapse, and chemical anomalies. We perform a three-dimensional self-consistent core-collapse supernova simulation using this new progenitor model and find that it successfully presents an explosion and leaves a 1.53 M⊙ neutron star. Assuming a detector sensitivity of Kamiokande-II and the distance to the supernova of 51 kpc, we obtain 16 neutrino detection events in one second. Some characteristic modes in its gravitational wave signal are also discussed in this article.
Highlights
SN 1987A emerged in the Large Magellanic Cloud located at a distance of 51.4 ± 1.2 kpc
A blue hot surface of the progenitor star Sk-69◦202 found in the pre-explosion images, as well as the light curve without the typical plateau phase of type II-P SNe and the relatively short period of time delay between the neutrino burst detection and the shock breakout emission, suggest that the progenitor was a blue-supergiant (BSG)
We report the results of our self-consistent 3D simulations for core-collapse SN employing this new progenitor model
Summary
SN 1987A emerged in the Large Magellanic Cloud located at a distance of 51.4 ± 1.2 kpc. A blue hot surface of the progenitor star Sk-69◦202 found in the pre-explosion images, as well as the light curve without the typical plateau phase of type II-P SNe and the relatively short period of time delay (three hours) between the neutrino burst detection and the shock breakout emission, suggest that the progenitor was a blue-supergiant (BSG) This BSG star is considered that it used to be a RSG at ∼ 2 × 104 yr since three ring-like nebulae are surrounding the supernova remnant with the high He the CNO abundance ratios and the expansion velocity comparable to the RSG wind velocity. For neutrino transfer calculation we use the state-of-the-art neutrino opacity [5] and solve the neutrino transport taking 20 energy bins with an upper bound of 300 MeV for electron, anti-electron, and heavy-lepton neutrinos
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