The Evolution of Compact Binary Star Systems

Konstantin A Postnov,Lev R Yungelson

doi:10.12942/lrr-2006-6

Abstract

We review the formation and evolution of compact binary stars consisting of white dwarfs (WDs), neutron stars (NSs), and black holes (BHs). Binary NSs and BHs are thought to be the primary astrophysical sources of gravitational waves (GWs) within the frequency band of ground-based detectors, while compact binaries of WDs are important sources of GWs at lower frequencies to be covered by space interferometers (LISA). Major uncertainties in the current understanding of properties of NSs and BHs most relevant to the GW studies are discussed, including the treatment of the natal kicks which compact stellar remnants acquire during the core collapse of massive stars and the common envelope phase of binary evolution. We discuss the coalescence rates of binary NSs and BHs and prospects for their detections, the formation and evolution of binary WDs and their observational manifestations. Special attention is given to AM CVn-stars — compact binaries in which the Roche lobe is filled by another WD or a low-mass partially degenerate helium-star, as these stars are thought to be the best LISA verification binary GW sources.

Highlights

The date given as uniquely identifies the version of the article you are referring to
By virtue of Equations (63, 64) this means that for a given orbital period they have higher M. This effect is illustrated in the left panel of Figure 18. (The period–mass relation is not single-valued, since the M –R relation has two branches: a branch where the object is thermally supported and a branch where degenerate electrons provide the dominant pressure support.) The right panel of Figure 18 compares a model of the population of AM CVn-stars computed under assumptions that the donor white dwarfs have T = 0 and a model which takes into account cooling of the prospective donors between formation and Roche-lobe overflow (RLOF)
The current understanding of the evolution of binary stars is firmly based on observations of many types of binary systems, from wide non-interacting pairs to very close compact binaries consisting of remnants of stellar evolution

Summary

Introduction

The date given as uniquely identifies the version of the article you are referring to. Living Reviews supports two different ways to keep its articles up-to-date: Fast-track revision A fast-track revision provides the author with the opportunity to add short notices of current research results, trends and developments, or important publications to the article. A fast-track revision is refereed by the responsible subject editor. If an article has undergone a fast-track revision, a summary of changes will be listed here. Major update A major update will include substantial changes and additions and is subject to full external refereeing. It is published with a new publication number. For detailed documentation of an article’s evolution, please refer always to the history document of the article’s online version at http://www.livingreviews.org/lrr-2006-6

Objectives

Results

Conclusion