3D天炉座模拟揭示的核塌缩超新星爆发的总体框架
The Overarching Framework of Core-Collapse Supernova Explosions as Revealed by 3D Fornax Simulations
摘要：
我们已经进行了十九个国家的最先进的3D核心坍缩超新星模拟跨越广泛的祖质量。这是有史以来最大的复杂3D超新星模拟集合。我们已经发现，虽然这些模型中的大多数都爆炸了，但并不是所有的模型都爆炸了，即使是在可用的原始质量范围中间的模型也可能不太容易爆炸。这并不意味着那些我们没有看到爆炸的模型在自然界中不会爆炸，而是它们比其他模型更不容易爆炸。一个结果是，“紧凑性”的措施是不是一个度量的可爆炸性。我们发现，质量较低的大质量恒星祖先可能经历较低能量的爆炸，而质量较高的大质量恒星可能经历较高能量的爆炸。此外，大多数3D爆炸都有一个占主导地位的偶极子形态，有一个捏，蜂腰结构，并同时经历吸积和爆炸。我们再现的一般范围内的剩余中子星质量推断银河系中子星人口。然而，最大质量的祖先模型，特别是相对于爆炸能量，需要持续更长的物理时间才能渐近线到它们的最终状态。我们发现，虽然大多数的内部喷出物有Y $_e = 0.5$，有一个实质性的质子丰富的尾巴。这一结果具有重要意义的核合成产率作为一个功能的祖。最后，我们发现，非爆炸模型最终演变成紧凑的内部配置，经历一个准周期的螺旋SASI模式。除此之外，我们在爆炸模型中几乎看不到SASI的证据。
英文摘要：
We have conducted nineteen state-of-the-art 3D core-collapse supernova simulations spanning a broad range of progenitor masses. This is the largest collection of sophisticated 3D supernova simulations ever performed. We have found that while the majority of these models explode, not all do, and that even models in the middle of the available progenitor mass range may be less explodable. This does not mean that those models for which we did not witness explosion would not explode in Nature, but that they are less prone to explosion than others. One consequence is that the "compactness" measure is not a metric for explodability. We find that lower-mass massive star progenitors likely experience lower-energy explosions, while the higher-mass massive stars likely experience higher-energy explosions. Moreover, most 3D explosions have a dominant dipole morphology, have a pinched, wasp-waist structure, and experience simultaneous accretion and explosion. We reproduce the general range of residual neutron-star masses inferred for the galactic neutron-star population. The most massive progenitor models, however, in particular vis à vis explosion energy, need to be continued for longer physical times to asymptote to their final states. We find that while the majority of the inner ejecta have Y$_e = 0.5$, there is a substantial proton-rich tail. This result has important implications for the nucleosynthetic yields as a function of progenitor. Finally, we find that the non-exploding models eventually evolve into compact inner configurations that experience a quasi-periodic spiral SASI mode. We otherwise see little evidence of the SASI in the exploding models.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
