论文标题
大规模近二元进化的种群综合
Population Synthesis of Massive Close Binary Evolution
论文作者
论文摘要
二元种群合成是一种方法，可以通过二进制恒星进化的理论模型对不同观察者的观察力进行预测。与单颗恒星相比，二进制恒星具有更多可能的进化结果，而不同途径的相对速率（例如不同超新星类型的速率）取决于不确定或不良约束的物理学。在本章中，我们描述了种群综合，概述了主要不确定性，并讨论了核心偏离超新星的相关预测。在概述单星发展之后，我们概述了包括Roche-Lobe Overflow，Common-Envelope Evolution和Supernova Kicks（包括Roche-Lobe Overflow）中发生的重要物理过程。我们还讨论了如何构建结合相互作用二进制的合成恒星种群，以及不确定性（例如超新星踢的强度）如何影响任何预测。我们通过比较两个年轻恒星簇中的恒星种群的预测来说明这一过程。然后，我们讨论了人口综合的重要预测，以了解核心折叠超新星，它们的延迟时间分布和祖细胞星。最后，我们讨论如何预测紧凑型残留物的合并速率，从而预测重力波源的初始参数。
Binary population synthesis is the method by which predictions of varied observables of stellar populations can be made from theoretical models of binary stellar evolution. Binary stars have many more possible evolutionary outcomes compared to single stars and the relative rates of the different pathways, such as the rates of different supernova types, depend on uncertain or poorly constrained physics. In this Chapter we describe population synthesis, outline the major uncertainties and discuss the relevant predictions for core-collapse supernovae. After we overview single star evolution we outline the important physical processes that occur in binaries including Roche-lobe overflow, common-envelope evolution and supernova kicks. We also discuss how a synthetic stellar population incorporating interacting binaries can be constructed and how uncertainties, such as the strength of supernova kicks, affect any predictions. We illustrate the process by comparing predictions for the stellar populations in two young star clusters. We then discuss the important predictions from population synthesis for understanding core-collapse supernovae, their delay-time distribution and their progenitor stars. Finally we discuss how we can predict the rate of mergers of compact remnants and thus predict the initial parameters of gravitational wave sources.
