Fallback in core-collapse supernovae (CCSNe) plays an important role in determining the properties of the central compact remnants, which might produce a black hole (BH) hyperaccretion system in the centre of a massive CCSN. When the accretion rate is extremely high and neutrino cooling is dominant, the hyperaccretion should be in the phase of the neutrino-dominated accretion flows (NDAFs), and thus a large number of anisotropic MeV neutrinos will be launched from the disc along with the strong gravitational waves (GWs). In this paper, we perform a series of one-dimensional CCSN simulations with the initial explosion energy in the range of 2−8 B (1 B = 1051 erg) to investigate the fallback processes. By considering the evolution of the central BH mass and spin in the fallback accretion, we present the effects of the initial explosion energies, masses, and metallicities of the massive progenitor stars on the spectra of anisotropic MeV neutrinos and the waveform of GWs from NDAFs. These neutrino or GW signals might be detected by operational or future detectors, and the multimessenger joint detections could constrain the properties of CCSNe and progenitor stars.

中文翻译：

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后退核心坍缩超新星中黑洞中微子主导吸积流的各向异性中微子和引力波

核心坍缩超新星（CCSNe）的回退在确定中心致密残余物的性质方面起着重要作用，这可能会在巨大的CCSN中心产生黑洞（BH）超吸积系统。当吸积率极高且中微子冷却占主导地位时，超吸积应该处于中微子主导的吸积流（NDAFs）阶段，因此大量各向异性的 MeV 中微子会随着强引力波（GW）。在本文中，我们执行了一系列一维 CCSN 模拟，初始爆炸能量在 2-8 B（1 B = 1051 erg）范围内，以研究回退过程。通过考虑后备吸积中中心 BH 质量和自旋的演变，我们提出了初始爆炸能量的影响，各向异性 MeV 中微子光谱和来自 NDAF 的 GW 波形上大质量前身星的质量和金属丰度。这些中微子或引力波信号可能会被正在运行的或未来的探测器探测到，而多信使联合探测可能会限制 CCSNe 和前身星的特性。