论文标题
扔黑洞旋转轴
Tossing Black Hole Spin Axes
论文作者
论文摘要
双黑洞（BH+BH）合并的检测提供了了解其物理特性和起源的独特可能性。迄今为止，高频引力波观测站的Ligo-Virgo-Kagra网络宣布检测超过85 BH+BH合并事件（Abbott等，2022a）。可以从数据中提取的重要诊断功能是BHS有效的灵感旋转的分布。 This distribution is in clear tension with theoretical expectations from both an isolated binary star origin, which traditionally predicts close-to aligned BH component spins (Kalogera 2000; Farr et al. 2017), and formation via dynamical interactions in dense stellar environments that predicts a symmetric distribution of effective inspiral spins (Mandel & O'Shaughnessy 2010; Rodriguez et al. 2016b).这里证明，如果BHS在巨大恒星的核心崩溃中抛弃其旋转轴，则可以令人信服地解释观察到的数据，这与显然在新生儿中子恒星中作用的过程类似。然而，即使在第二个核心崩溃之前对旋转的比对，也很难再现了无自旋轴的形成。基于仅具有最低假设的模拟，可以根据经验数据的约束对第一和第二胎BHS的自旋幅度进行限制，从而在形成BHS之前可以更好地理解大量的二进制恒星进化。
The detection of double black hole (BH+BH) mergers provides a unique possibility to understand their physical properties and origin. To date, the LIGO-Virgo-KAGRA network of high-frequency gravitational wave observatories have announced the detection of more than 85 BH+BH merger events (Abbott et al. 2022a). An important diagnostic feature that can be extracted from the data is the distribution of effective inspiral spins of the BHs. This distribution is in clear tension with theoretical expectations from both an isolated binary star origin, which traditionally predicts close-to aligned BH component spins (Kalogera 2000; Farr et al. 2017), and formation via dynamical interactions in dense stellar environments that predicts a symmetric distribution of effective inspiral spins (Mandel & O'Shaughnessy 2010; Rodriguez et al. 2016b). Here it is demonstrated that isolated binary evolution can convincingly explain the observed data if BHs have their spin axis tossed during their formation process in the core collapse of a massive star, similarly to the process evidently acting in newborn neutron stars. BH formation without spin-axis tossing, however, has difficulties reproducing the observed data - even if alignment of spins prior to the second core collapse is disregarded. Based on simulations with only a minimum of assumptions, constrains from empirical data can be made on the spin magnitudes of the first- and second-born BHs, thereby serving to better understand massive binary star evolution prior to the formation of BHs.
