论文标题
在孤立的地层通道中生产具有大型未对准旋转的二进制黑洞的途径
Pathways for producing binary black holes with large misaligned spins in the isolated formation channel
论文作者
论文摘要
二进制黑洞（BBH）可以从孤立的高质量二元星的塌陷芯中形成。这些BBH的质量和旋转取决于现象的复杂相互作用，例如潮汐，风，积聚，公共 - 层状演化（CEE），超新星自然踢球和恒星核心 - 埃纳维洛普偶联。 BBH的合并期间发出的引力波取决于它们的质量和自旋，因此可以限制这些现象。我们提出了一个简化的二进制恒星演化模型，并识别参数空间的区域，该区域与轨道角动量未对准大型旋转的BBH。在我们模型的方案A（B）中，稳定的传质（SMT）发生在较大（较少）的巨星的Roche-Lobe Overflow（RLOF）之后，而CEE遵循较少（更多的）大型恒星的RLOF。每个场景进一步分为途径1和2 2，具体取决于较大的恒星的核心是否分别在较小的恒星的RLOF之前或之后崩溃。如果恒星芯与它们的信封微弱耦合，那么如果出生的旋转超过$ 10 \％的破裂值是从恒星祖细胞继承的，则可以产生高度旋转的BBH。 BBH可以在场景A中的沃尔夫射线阶段通过潮汐同步获得大型旋转。
Binary black holes (BBHs) can form from the collapsed cores of isolated high-mass binary stars. The masses and spins of these BBHs are determined by the complicated interplay of phenomena such as tides, winds, accretion, common-envelope evolution (CEE), supernova natal kicks, and stellar core-envelope coupling. The gravitational waves emitted during the mergers of BBHs depend on their masses and spins and can thus constrain these phenomena. We present a simplified model of binary stellar evolution and identify regions of the parameter space that produce BBHs with large spins misaligned with their orbital angular momentum. In Scenario A (B) of our model, stable mass transfer (SMT) occurs after Roche-lobe overflow (RLOF) of the more (less) massive star, while CEE follows RLOF of the less (more) massive star. Each scenario is further divided into Pathways 1 and 2 depending on whether the core of the more massive star collapses before or after RLOF of the less massive star, respectively. If the stellar cores are coupled weakly to their envelopes, highly spinning BBHs can be produced if natal spins greater than $10\%$ of the breakup value are inherited from the stellar progenitors. BBHs can alternatively acquire large spins by tidal synchronization during the Wolf-Rayet stage in Scenario A or by accretion onto the initially more massive star during SMT in Scenario B. BBH spins can be highly misaligned if the kicks are comparable to the orbital velocity, which is more easily achieved in Pathway A1 where the kick of the more massive star precedes CEE.
