Gravitational Waves from Core-Collapse Supernovae
Gravitational Waves from Core-Collapse Supernovae
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DOI：
10.1007/978-981-15-4702-7_21-1
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发表时间：
2020-10
期刊：
影响因子：
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通讯作者：
E. Abdikamalov;G. Pagliaroli;D. Radice
中科院分区：
文献类型：
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作者：
E. Abdikamalov;G. Pagliaroli;D. Radice
总结了我们目前对核心塌缩超新星引力波发射的认识。我们回顾了多维模拟的既定结果，并尽可能提供粗略的计算，以强调潜在的物理原理。引力波主要是由质子中子星振荡发出的。在代表最常见的超新星类型的缓慢旋转的情况下，振荡是由多维流体动力学不稳定激发的，而在罕见的快速旋转的情况下，质子中子星由于离心力而出生时是扁平的。对于我们银河系内的一个源，引力波信号可能会被电流探测器略微看到，而未来的第三代仪器将能够进行更强大和更详细的观测。产生非轴对称不稳定性的快速旋转模型可能与第三代探测器相距百万秒可见。最后，我们讨论了超新星多信使观测的策略。
We summarize our current understanding of gravitational wave emission from core-collapse supernovae. We review the established results from multi-dimensional simulations and, wherever possible, provide back-of-the-envelope calculations to highlight the underlying physical principles. The gravitational waves are predominantly emitted by protoneutron star oscillations. In slowly rotating cases, which represent the most common type of the supernovae, the oscillations are excited by multi-dimensional hydrodynamic instabilities, while in rare rapidly rotating cases, the protoneutron star is born with an oblate deformation due to the centrifugal force. The gravitational wave signal may be marginally visible with current detectors for a source within our galaxy, while future third-generation instruments will enable more robust and detailed observations. The rapidly rotating models that develop non-axisymmetric instabilities may be visible up to a megaparsec distance with the third-generation detectors. Finally, we discuss strategies for multi-messenger observations of supernovae.