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"The Evolution of Compact Binary Star Systems"

Konstantin A. Postnov and Lev R. Yungelson

	Abstract
1	Introduction
	1.1	Formation of stars and end products of their evolution
	1.2	Binary stars
2	Observations of Double Compact Stars
	2.1	Compact binaries with neutron stars
	2.2	How frequent are NS binary coalescences?
	2.3	Black holes in binary systems
	2.4	A model-independent upper limit on the BH-BH/BH-NS coalescence rate
3	Basic Principles of the Evolution of Binary Stars
	3.1	Keplerian binary system and radiation back reaction
	3.2	Mass exchange in close binaries
	3.3	Mass transfer modes and mass and angular momentum loss in binary systems
	3.4	Supernova explosion
	3.5	Kick velocity of neutron stars
	3.6	Common envelope stage
	3.7	Other notes on the CE problem
4	Evolutionary Scenario for Compact Binaries with Neutron Star or Black Hole Components
	4.1	Compact binaries with neutron stars
	4.2	Black-hole–formation parameters
5	Formation of Double Compact Binaries
	5.1	Analytical estimates
	5.2	Population synthesis results
6	Detection Rates
7	Short-Period Binaries with White-Dwarf Components
	7.1	Formation of compact binaries with white dwarfs
	7.2	White-dwarf binaries
	7.3	Type Ia supernovae
	7.4	Ultra-compact X-ray binaries
8	Observations of Double-Degenerate Systems
	8.1	Detached white dwarf and subdwarf binaries
9	Evolution of Interacting Double-Degenerate Systems
	9.1	“Double-degenerate family” of AM CVn stars
	9.2	“Helium-star family” of AM CVn stars
	9.3	Final stages of evolution of interacting double-degenerate systems
10	Gravitational Waves from Compact Binaries with White-Dwarf Components
11	AM CVn-Type Stars as Sources of Optical and X-Ray Emission
12	Conclusions
	Acknowledgments
	References
	Footnotes
	Updates
	Figures
	Tables

List of Tables

Table 1:
Types of compact remnants of single stars (the ranges of progenitor mass are shown for solar composition stars).

Table 2:
Observed parameters of neutron star binaries.

Table 3:
Derived parameters of neutron star binaries.

Table 4:
Observed parameters of HMXB with black holes.

Table 5:
Comparison of Fe-Core Collapse and e-Capture Supernovae. Table reproduced with permission from [685], copyright by AAS.

Table 6:
Examples of the estimates for Galactic merger rates of relativistic binaries calculated under different assumptions on the parameters entering population synthesis.

Table 7:
Properties of companions to exploding WD. After [679].

Table 8:
Current birth rates and merger rates per year for Galactic disk binaries containing two compact objects and their total number in the Galactic disk [518].

Table 9:
Detectable sources (5 Mkm detector – two upper rows, 1 Mkm detector – two lower rows). Values are shown for $SNR = 5 thr$ , one interferometric observable, and one year of observation, with approximate scalings as a function of $−1∕2 −1∕2 ρeff = SNRthr (Tobs∕yr) (Nobs)$ [531].