通常来说，大质量恒星都会以中心核塌缩超新星爆发结束自己的生命，形成致密天体（中子星或黑洞）。然而，最新的理论模拟显示，许多中心核塌缩可能会经历失败的超新星爆发（FSN）,直接塌缩成黑洞，并且在观测上已经发现可能的候选体。FSN的发生依赖于中心核塌缩前恒星的结构和化学丰度。众所周知，70%以上的大质量恒星处在双星系统中，而且双星的相互作用对恒星的结构与演化有着重要的影响。借助双星演化模型和中微子机制，本项目将重点研究大质量双星系统中FSN发生的物理条件，分析由FSN通道形成的黑洞质量的分布特点，给出‘重’黑洞的形成条件。最后利用星族合成方法，研究由FSN通道形成大样本双黑洞系统的统计特性，借助引力波辐射模型讨论这些双黑洞系统并合时产生的引力波，给出引力波GW150914可能的前身星系统。

Massive stars usually end their lives as central core-collapse supernova explosions, and leave compact objects (neutron stars or black holes). However, based on the recent theoretical simulation, many of them can undergo failed supernova explosions (FSNs), and directly collapse into black holes. Furthermore, possible candidates for FSNs had been observed. FSNs depend on the stellar structures and chemical abundances of the core-collapse progenitors. It is well known that more than 70% of massive stars are in binary systems, and binary interactions have great effects on the stellar structures and evolutions. Using the models of binary evolutions and neutrino mechanism, this project focuses on studying the physical conditions of FSNs in massive binaries, discussing the mass distribution of the black holes formed via FSN channel, and finding out the formation channel for ‘heavy’ black holes. With help of the method of population synthesis, the project investigates the statistical properties of a large sample for black-hole binaries via FSN channel, discusses the gravitational waves released by them, and gives possible progenitors for GW150914.