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  Matter Mixing in Aspherical Core-collapse Supernovae: Three-dimensional Simulations with Single Star and Binary Merger Progenitor Models for SN 1987A

Ono, M., Nagataki, S., Ferrand, G., Takahashi, K., Umeda, H., Yoshida, T., et al. (2020). Matter Mixing in Aspherical Core-collapse Supernovae: Three-dimensional Simulations with Single Star and Binary Merger Progenitor Models for SN 1987A. Astrophysical Journal, 888(2): 111. doi:10.3847/1538-4357/ab5dba.

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Item Permalink: http://hdl.handle.net/21.11116/0000-0005-D847-8 Version Permalink: http://hdl.handle.net/21.11116/0000-0005-D84B-4
Genre: Journal Article

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 Creators:
Ono, Masaomi, Author
Nagataki, Shigehiro, Author
Ferrand, Gilles, Author
Takahashi, Koh1, Author              
Umeda, Hideyuki, Author
Yoshida, Takashi, Author
Orlando, Salvatore, Author
Miceli, Marco, Author
Affiliations:
1Computational Relativistic Astrophysics, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, ou_2541714              

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Free keywords: Astrophysics, High Energy Astrophysical Phenomena, astro-ph.HE, Astrophysics, Solar and Stellar Astrophysics, astro-ph.SR
 Abstract: We perform three-dimensional hydrodynamic simulations of aspherical core-collapse supernovae focusing on the matter mixing in SN 1987A. The impacts of four progenitor (pre-supernova) models and parameterized aspherical explosions are investigated. The four pre-supernova models include a blue supergiant (BSG) model based on a slow merger scenario developed recently for the progenitor of SN 1987A (Urushibata et al. 2018). The others are a BSG model based on a single star evolution and two red supergiant (RSG) models. Among the investigated explosion (simulation) models, a model with the binary merger progenitor model and with an asymmetric bipolar-like explosion, which invokes a jetlike explosion, best reproduces constraints on the mass of high velocity $^{56}$Ni, as inferred from the observed [Fe II] line profiles. The advantage of the binary merger progenitor model for the matter mixing is the flat and less extended $\rho \,r^3$ profile of the C+O core and the helium layer, which may be characterized by the small helium core mass. From the best explosion model, the direction of the bipolar explosion axis (the strongest explosion direction), the neutron star (NS) kick velocity, and its direction are predicted. Other related implications and future prospects are also given.

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 Dates: 2019-12-042020
 Publication Status: Published in print
 Pages: Accepted for publication in The Astrophysical Journal, 62 pages, 26 figures, 3 tables
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 Rev. Method: -
 Identifiers: arXiv: 1912.02234
DOI: 10.3847/1538-4357/ab5dba
URI: http://arxiv.org/abs/1912.02234
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Title: Astrophysical Journal
Source Genre: Journal
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Pages: - Volume / Issue: 888 (2) Sequence Number: 111 Start / End Page: - Identifier: -