论文标题
孤立的黑孔二进制旋转进动和营养的签名
Signatures of spin precession and nutation in isolated black-hole binaries
论文作者
论文摘要
来自孤立的高质量二进制恒星的二进制黑洞（BBHS）的自旋进动取决于现象的相互作用，例如潮汐，风，积聚，公共 - 内玻璃式演化，纳塔尔踢和恒星核心孔 - 启动式耦合。在先前的工作中，我们确定了参数空间的区域，这些区域可能会产生来自鼻踢和高旋转幅度的BBH，并从三种机制（潮汐，积聚或遗传）通过最小的核心核能耦合而产生较高的自旋幅度。在这里，我们使用五个参数探索了此类BBH的自旋进动，这些参数描述了轨道角动量进攻和刺激的幅度和频率，并在总角度动量上进行了刺激，从而调节了重力波发射。通常可以为至少一个黑洞旋转的足够强大的出生踢而进行进一步。营养是自旋旋转耦合的结果，取决于三种自旋机制。潮汐同步可以在对齐的有效自旋和螺旋频率之间留下明显的相关性，但不会产生大型的脂肪。当一个黑洞积聚$ \ gtrsim 20 \％$的信封时，进动频率和振幅很大。当吸积是狼射线（WR）恒星时，需要少量的积聚，例如$ \约2 \％$。 The inheritance of high natal WR spins ($\gtrsim 5\%$ of their maximum breakup value) via minimal core-envelope coupling is the most promising mechanism for producing nutating BBHs, implying that a measurement of nutation from gravitational-wave observations may suggest isolated-binary origin with minimal core-envelope coupling.
The spin precession of binary black holes (BBHs) that originate from isolated high-mass binary stars is determined by the interplay of phenomena such as tides, winds, accretion, common-envelope evolution, natal kicks, and stellar core-envelope coupling. In previous work, we identified regions of the parameter space that may produce BBHs with large misalignments from natal kicks and high spin magnitudes from three mechanisms - tides, accretion, or inheritance via minimal core-envelope coupling. Here, we explore the spin precession of such BBHs using five parameters that describe the amplitude and frequency with which the orbital angular momentum precesses and nutates about the total angular momentum, modulating the gravitational-wave emission. Precession is generally possible for sufficiently strong natal kicks provided at least one of the black holes is spinning. Nutation is a consequence of spin-spin coupling and depends on the three spin-up mechanisms. Tidal synchronization can leave a distinct correlation between the aligned effective spin and the nutation frequency, but does not produce large nutations. When a black hole accretes $\gtrsim 20\%$ of its companion's envelope, the precession frequency and amplitude are large. A much smaller amount of accretion, e.g., $\approx 2\%$, is needed to provide a large precession frequency and amplitude when the accretor is a Wolf-Rayet (WR) star. The inheritance of high natal WR spins ($\gtrsim 5\%$ of their maximum breakup value) via minimal core-envelope coupling is the most promising mechanism for producing nutating BBHs, implying that a measurement of nutation from gravitational-wave observations may suggest isolated-binary origin with minimal core-envelope coupling.
