Supernova simulations from a 3D progenitor model - Impact of perturbations and evolution of explosion properties
Supernova simulations from a 3D progenitor model - Impact of perturbations and evolution of explosion properties
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DOI：
10.1093/mnras/stx1962
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发表时间：
2017-05
影响因子：
4.8
通讯作者：
B. Muller;T. Melson;A. Heger;Hideko Nomura Queen's University Belfast;Monash University;M. F. Astrophysics;U. Minnesota;S. University
中科院分区：
文献类型：
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作者：
B. Muller;T. Melson;A. Heger;Hideko Nomura Queen's University Belfast;Monash University;M. F. Astrophysics;U. Minnesota;S. University
我们研究了对流壳燃烧的大尺度扰动对核心坍缩超新星爆炸机制的影响，使用三维（3D）多群中微子流体动力学模拟的18太阳质量的祖。从最近的一个O壳燃烧的3D模型中获得的O壳中的种子非球面性，有助于在反弹后330 ms触发中微子驱动的爆炸，而在基于球对称祖先的模型中，冲击波至少在另外300 ms内不会复活。我们初步推断，由于预坍缩扰动的冲击波复兴的临界光度减少约20%。这表明对流种子扰动在某些祖细胞的爆炸机制中起着重要的作用。我们跟踪了18太阳质量模型进入爆发阶段超过2s的演化过程，发现在这个阶段吸积和物质抛射的循环仍然在进行。初步的诊断爆炸能量值为0.77贝特，重子中子星星的质量为1.85太阳质量，中子星星的反冲速度约为600 km/s，中子星星的自旋周期约为20 ms，爆炸和残余物的性质略有不典型，但仍然在观测到的分布范围内。虽然仍然需要更精细的模拟和更大规模的祖先调查，但这表明在观测范围内解决冲击波复兴和爆炸能量问题的方法是可以实现的中微子驱动的3D爆炸。
We study the impact of large-scale perturbations from convective shell burning on the core-collapse supernova explosion mechanism using three-dimensional (3D) multi-group neutrino hydrodynamics simulations of an 18 solar mass progenitor. Seed asphericities in the O shell, obtained from a recent 3D model of O shell burning, help trigger a neutrino-driven explosion 330ms after bounce whereas the shock is not revived in a model based on a spherically symmetric progenitor for at least another 300ms. We tentatively infer a reduction of the critical luminosity for shock revival by ~20% due to pre-collapse perturbations. This indicates that convective seed perturbations play an important role in the explosion mechanism in some progenitors. We follow the evolution of the 18 solar mass model into the explosion phase for more than 2s and find that the cycle of accretion and mass ejection is still ongoing at this stage. With a preliminary value of 0.77 Bethe for the diagnostic explosion energy, a baryonic neutron star mass of 1.85 solar masses, a neutron star kick of ~600km/s and a neutron star spin period of ~20ms at the end of the simulation, the explosion and remnant properties are slightly atypical, but still lie comfortably within the observed distribution. Although more refined simulations and a larger survey of progenitors are still called for, this suggests that a solution to the problem of shock revival and explosion energies in the ballpark of observations are within reach for neutrino-driven explosions in 3D.