在星团中填充黑洞质量间隙：一般关系和上限
Populating the Black Hole Mass Gaps In Stellar Clusters: General Relations and Upper Limits
摘要：
理论和观测表明，单星演化不能产生质量在$3-5M_{\odot}$和$\sim 45M_{\odot}$以上的黑洞，分别称为下质量隙（LMG）和上质量隙（UMG）。然而，通过致密星团中致密天体的合并，有可能在这些间隙中形成BH，例如LMG和UMG可以分别通过双星中子星和BBH合并来填充。这意味着，如果在引力波（GW）中观察到至少有一个质量间隙物体的双星合并，那么要么星团在组装双星合并中是有效的，要么我们的单星模型必须修改。因此，了解星团如何有效地填充两个质量间隙对恒星和GW天体物理学都有重大意义。在本文中，我们提出了一个系统的研究如何有效的星团在人口的质量差距，通过集群GW合并。为此，我们推导出一组封闭形式的关系，用于描述紧凑的对象二进制的动态相互作用和GW合并集群内的演变。通过考虑静态和时间演变的人口，我们发现特别是球状星团显然是低效的人口的LMG相比，UMG。我们进一步描述了这些结果与特征质量，时间和长度尺度与问题。
英文摘要：
Theory and observations suggest that single-star evolution is not able to produce black holes (BHs) with masses in the range $3-5M_{\odot}$ and above $\sim 45M_{\odot}$, referred to as the lower mass gap (LMG) and the upper mas gap (UMG), respectively. However, it is possible to form BHs in these gaps through merger of compact objects in dense clusters, e.g. the LMG and the UMG can be populated through binary neutron star- and BBH mergers, respectively. This implies that if binary mergers are observed in gravitational waves (GWs) with at least one mass gap object, then either clusters are effective in assembling binary mergers, or our single-star models have to be revised. Understanding how effective clusters are at populating both mass gaps have therefore major implications for both stellar- and GW astrophysics. In this paper we present a systematic study on how efficient stellar clusters are at populating both mass gaps through in-cluster GW mergers. For this, we derive a set of closed form relations for describing the evolution of compact object binaries undergoing dynamical interactions and GW merger inside their cluster. By considering both static and time evolving populations, we find in particular that globular clusters are clearly inefficient at populating the LMG in contrast to the UMG. We further describe how these results relate to the characteristic mass, time, and length scales associated with the problem.
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