论文标题
质量间隙，自旋差距和合并二进制黑洞的起源
The mass gap, the spin gap, and the origin of merging binary black holes
论文作者
论文摘要
据信，Ligo和处女座观察到的两个主要通道是产生黑洞二进制合并的，被认为是田间中恒星二进制的孤立演化，而星形簇中的动态形成。它们的相对效率可以以“混合分数”为特征。配对的不稳定性可防止出色的崩溃产生比$ 45 m_ \ odot $更大的黑洞。此“质量差距”仅适用于场的形成场景，可以通过簇中的重复合并来填充。类似的推理也适用于二进制的有效旋转。如果黑孔诞生缓慢旋转，则只能由动态组装的黑洞二进制组填充参数空间的高旋转部分（“自旋差距”）。使用半分析群集模型，我们表明可以利用质量间隙，自旋隙或两者的未来重力波事件，以推断田间和群集形成通道之间的混合分数。
Two of the dominant channels to produce the black-hole binary mergers observed by LIGO and Virgo are believed to be the isolated evolution of stellar binaries in the field and dynamical formation in star clusters. Their relative efficiency can be characterized by a "mixing fraction." Pair instabilities prevent stellar collapse from generating black holes more massive than about $45 M_\odot$. This "mass gap" only applies to the field formation scenario, and it can be filled by repeated mergers in clusters. A similar reasoning applies to the binary's effective spin. If black holes are born slowly rotating, the high-spin portion of the parameter space (the "spin gap") can only be populated by black hole binaries that were assembled dynamically. Using a semianalytical cluster model, we show that future gravitational-wave events in either the mass gap, the spin gap, or both can be leveraged to infer the mixing fraction between the field and cluster formation channels.
