Six binary-merger progenitors of supernova 1987A (SN 1987A) with properties close to those of the blue supergiant Sanduleak −69202 are exploded by neutrino heating and evolved until long after shock breakout in 3D and continued for light-curve calculations in spherical symmetry. Our results confirm previous findings for single-star progenitors: (1) 3D neutrino-driven explosions with SN 1987A-like energies synthesize ⁵⁶Ni masses consistent with the radioactive light-curve tail; (2) hydrodynamic models mix hydrogen inward to minimum velocities below 40 km s⁻¹ compatible with spectral observations of SN 1987A; and (3) for given explosion energy the efficiency of outward radioactive ⁵⁶Ni mixing depends mainly on high growth factors of Rayleigh–Taylor instabilities at the (C+O)/He and He/H composition interfaces and a weak interaction of fast plumes with the reverse shock occurring below the He/H interface. All binary-merger models possess presupernova radii matching the photometric radius of Sanduleak −69202 and a structure of the outer layers allowing them to reproduce the observed initial luminosity peak in the first ∼7 days. Models that mix about 0.5 M _⊙ of hydrogen into the He-shell and exhibit strong outward mixing of ⁵⁶Ni with maximum velocities exceeding the 3000 km s⁻¹ observed for the bulk of ejected ⁵⁶Ni have light-curve shapes in good agreement with the dome of the SN 1987A light curve. A comparative analysis of the best representatives of our 3D neutrino-driven explosion models of SN 1987A based on single-star and binary-merger progenitors reveals that only one binary model fulfills all observational constraints, except one.

超新星 1987A (SN 1987A) 的六颗双星合并前身星，其特性与蓝色超巨星 Sanduleak −69202 的特性接近，在中微子加热的作用下发生爆炸，并演化至 3D 冲击爆发后很久，并继续进行球对称光曲线计算。我们的结果证实了之前对单星祖细胞的发现：（1）具有类似 SN 1987A 能量的 3D 中微子驱动爆炸合成了^{56 个}与放射性光曲线尾部一致的 Ni 质量；(2) 流体动力学模型将氢向内混合到低于 40 km s ^{-1 的}最小速度，与 SN 1987A 的光谱观测相符；(3) 对于给定的爆炸能量，外向放射性⁵⁶的效率Ni 混合主要取决于 (C+O)/He 和 He/H 组成界面处瑞利-泰勒不稳定性的高增长因子，以及快速羽流与 He/H 界面下方发生的反向冲击的弱相互作用。所有二元合并模型都具有与 Sanduleak -69202 的光度半径相匹配的超新星前半径和外层结构，允许它们在前 7 天重现观察到的初始光度峰值。将大约 0.5 M _⊙的氢混合到 He 壳中并表现出⁵⁶ Ni 的强烈向外混合的模型，其最大速度超过了对大部分喷射出的⁵⁶观察到的 3000 km s ^-1Ni 的光曲线形状与 SN 1987A 光曲线的圆顶非常吻合。对我们基于单星和双星合并祖先的 SN 1987A 3D 中微子驱动爆炸模型的最佳代表的比较分析表明，只有一个双星模型满足所有观测约束，除了一个。