Population Synthesis of Massive Close Binary Evolution

TL;DR

This paper reviews binary population synthesis, detailing physical processes, uncertainties, and predictions for supernovae, stellar populations, and gravitational wave sources, emphasizing the impact of binary interactions on stellar evolution outcomes.

Contribution

It provides a comprehensive overview of binary population synthesis methods, uncertainties, and their implications for supernovae, stellar populations, and gravitational wave event predictions.

Findings

Predictions for core-collapse supernovae rates and progenitors.

Impact of supernova kicks on binary evolution outcomes.

Estimates of compact remnant merger rates for gravitational waves.

Abstract

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.