The coalescence of compact binaries containing neutron stars or black holes is one of the most promising signals for advanced ground-based laser interferometer gravitational-wave detectors, with the first direct detections expected over the next few years. The rate of binary coalescences and the distribution of component masses is highly uncertain, and population synthesis models predict a wide range of plausible values. Poorly constrained parameters in population synthesis models correspond to poorly understood astrophysics at various stages in the evolution of massive binary stars, the progenitors of binary neutron star and binary black hole systems. These include effects such as supernova kick velocities, parameters governing the energetics of common envelope evolution and the strength of stellar winds. Observing multiple binary black hole systems through gravitational waves will allow us to infer details of the astrophysical mechanisms that lead to their formation. Here we simulate gravitational-wave observations from a series of population synthesis models including the effects of known selection biases, measurement errors and cosmology. We compare the predictions arising from different models and show that we will be able to distinguish between them with observations (or the lack of them) from the early runs of the advanced LIGO and Virgo detectors. This will allow us to narrow down the large parameter space for binary evolution models.
Reassessing the Spin of Second-born Black Holes in Coalescing Binary Black Holes and Its Connection to the chi_eff-q Correlation
Anhui Normal University（安徽师范大学）；University of Nevada, Las Vegas（内华达大学拉斯维加斯分校）；Zhejiang University of Technology（浙江工业大学）；Université de Genève（日内瓦大学）；Guizhou University（贵州大学）
在LIGO O 1和O2科学运行中发现的能够在哈勃时间内合并并产生强大引力波爆发的大质量近距离双星黑洞的可能形成机制包括场低金属丰度大质量双星的演化、致密星团中的动力学形成和原始黑洞。不同的形成通道产生不同的源分布的总质量${M_\mathrm{tot}}$和有效自旋$χ_\mathrm{eff}$的合并的二元BH。利用改进的\textsc{bse}程序，我们对标准场质量双星形成通道中不同金属丰度的BH先驱体的有效自旋和总质量分布进行了广泛的布居合成计算（从零金属第三族恒星到太阳金属丰度），不同的初始旋转的二进制组件，恒星风质量损失处方，不同的BH形成模型和一系列常见的包络效率。在两区（核-包）近似下，利用有效的核-包耦合时间，并考虑了双星演化过程中恒星包旋转的潮汐同步，讨论了恒星的自转。我们的模拟结果与金属度相关的恒星形成历史进行卷积，表明LIGO O O 1-O2运行期间检测到的合并双黑洞的总质量和有效自旋，但最重的一个（GW 170729）可以由所采用的BH形成模型同时再现。GW 170729的显著有效自旋需要从旋转的恒星包层额外的回落。
The detection rate of Inspiral and Quasi-normal modes of Pop III binary black holes which can confirm or refute the General Relativity in the strong gravity region
Linking high-mass X-ray binaries to binary compact object mergers in Milky Way-like galaxies
Universidad Andres Bello（安德烈斯贝略大学）；INAF - Osservatorio di Astrofisica e Scienza dello Spazio（意大利国家天体物理研究所空间科学与天体物理观测站）；Instituto de Astrofísica de Canarias（加那利群岛天体物理研究所）；Universidad de La Laguna（拉拉克鲁纳大学）；Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona (UB)（巴塞罗那宇宙科学研究所）；Universität Heidelberg, Zentrum für Astronomie (ZAH), Institut für Theoretische Astrophysik（海德堡大学天文学中心理论天体物理研究所）
