Following the collapse of their cores, some of the massive binary stars that populate our Universe are expected to form merging binaries composed of black holes and neutron stars. Gravitational-wave observations of the resulting compact binaries can reveal precious details on the inner workings of the supernova mechanism and the subsequent formation of compact objects. Within the framework of the population-synthesis code mobse, we present the implementation of a new supernova model that relies on the compactness of the collapsing star. The model has two free parameters, namely the compactness threshold that separates the formation of black holes and that of neutron stars, and the fraction of the envelope that falls back onto the newly formed black holes. We compare this model extensively against other prescriptions that are commonly used in binary population synthesis. We find that the cleanest signatures of the role of the pre-supernova stellar compactness are (1) the relative formation rates of the different kinds of compact binaries, which mainly depend on the compactness threshold parameter, and (2) the location of the upper edge of the mass gap between the lightest black holes and the heaviest neutron stars, which mainly depends on the fallback fraction.

随着它们的核心坍缩，我们宇宙中的一些大质量双星预计会形成由黑洞和中子星组成的合并双星。对由此产生的致密双星的引力波观测可以揭示有关超新星机制内部运作和致密天体随后形成的宝贵细节。在人口合成代码mobse的框架内，我们介绍了一种新的超新星模型的实现，该模型依赖于坍缩恒星的紧凑性。该模型有两个自由参数，即区分黑洞形成和中子星形成的致密性阈值，以及回落到新形成的黑洞上的包络部分。我们将该模型与二元总体合成中常用的其他处方进行了广泛的比较。我们发现超新星前恒星致密性作用的最清晰特征是（1）不同类型致密双星的相对形成率，主要取决于致密性阈值参数，以及（2）上部的位置最轻的黑洞和最重的中子星之间质量差距的边缘，这主要取决于后备分数。