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

被引:41
作者
Ono, Masaomi [1 ,2 ]
Nagataki, Shigehiro [1 ,2 ]
Ferrand, Gilles [1 ,2 ]
Takahashi, Koh [3 ]
Umeda, Hideyuki [4 ]
Yoshida, Takashi [4 ]
Orlando, Salvatore [5 ]
Miceli, Marco [5 ,6 ]
机构
[1] RIKEN Cluster Pioneering Res, Astrophys Big Bang Lab, 2-1 Hirosawa, Wako, Saitama 3510198, Japan
[2] RIKEN Interdisciplinary Theoret & Math Sci Progra, 2-1 Hirosawa, Wako, Saitama 3510198, Japan
[3] Albert Einstein Inst, Max Planck Inst Gravitat Phys, Muhlenberg 1, D-14476 Potsdam, Germany
[4] Univ Tokyo, Grad Sch Sci, Dept Astron, Bunkyo Ku, 7-3-1 Hongo, Tokyo 1130033, Japan
[5] INAF Osservatorio Astron Palermo, Piazza Parlamento 1, I-90134 Palermo, Italy
[6] Univ Palermo, Dipartimento Fis & Chim, Piazza Parlamento 1, I-90134 Palermo, Italy
关键词
Core-collapse supernovae; Supernova dynamics; Supergiant stars; Neutron stars; Stellar evolutionary models; Hydrodynamical simulations; Explosive nucleosynthesis; RAYLEIGH-TAYLOR INSTABILITIES; APPROXIMATIVE NEUTRINO TRANSPORT; GAMMA-RAY EMISSION; TURBULENT CONVECTION; MASSIVE STARS; X-RAY; PRESUPERNOVA EVOLUTION; DRIVEN SUPERNOVA; CIRCUMSTELLAR ENVIRONMENT; BLUE SUPERGIANTS;
D O I
10.3847/1538-4357/ab5dba
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
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 an asymmetric bipolar-like explosion, which invokes a jetlike explosion, best reproduces constraints on the mass of high-velocity Ni-56, 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) and the neutron star (NS) kick velocity and direction are predicted. Other related implications and future prospects are also given.
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页数:40
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