Physics of Binary Star Evolution

Name: Physics of Binary Star Evolution | From Stars to X-ray Binaries and Gravitational Wave Sources
Brand: Princeton University Press
Price: 92.99 EUR
Availability: OnlineOnly

From Stars to X-ray Binaries and Gravitational Wave Sources

Thomas M. Tauris Edward P.J. van den Heuvel(Autor*in)

Princeton University Press

1. Auflage

Erschienen am 28. März 2023

864 Seiten

E-Book

PDF mit Wasserzeichen-DRM

Systemvoraussetzungen

978-0-691-23926-2 (ISBN)

92,99 €inkl. 7% MwSt.

Systemvoraussetzungen

für PDF mit Wasserzeichen-DRM

E-Book Einzellizenz

Als Download verfügbar

Beschreibung

Weitere Details

Weitere Ausgaben

Personen

Inhalt

Cover
Contents
Preface
1. Introduction: The Role of Binary Star Evolution in Astrophysics
2. Historical Notes on Binary Star Discoveries
2.1 Visual Binaries and the Universal Validity of the Laws of Physics
2.2 Astrometric Binaries
2.3 Spectroscopic Binaries
2.4 Eclipsing Binaries
2.5 The Discovery of the Binary Nature of Novae and Other Cataclysmic Variables
2.6 The Discovery of the Binary Nature of the Brightest X-ray Sources in the Sky
2.7 Centaurus X-3: Discovery of the First Neutron Star X-ray Binary
2.8 Cygnus X-1: Discovery of the First Black Hole X-ray Binary
2.9 The Discovery of the Existence of Double NSs and Double BHs
2.10 The Discovery of Millisecond Radio Pulsars: Remnants of LMXBs
2.11 Type Ia, Ib, and Ic SNe: Results of the Evolution of Binary Systems
2.12 Binary Nature of Blue Stragglers, Barium Stars, and Peculiar Post-AGB Stars
Exercises
3. Orbits and Masses of Spectroscopic Binaries
3.1 Some Basics about Binary Orbits
3.2 Orbit Determination
3.3 Determination of Stellar Masses
3.4 Masses of Unevolved Main-sequence Stars
3.5 The Most Massive Stars
3.6 Falsification of Radial Velocity Curves
3.7 The Incidence of Interacting Binaries and Their Orbital Distributions and Masses
Exercises
4. Mass Transfer and Mass Loss in Binary Systems
4.1 Roche Equipotentials
4.2 Limitations in the Concept of Roche Equipotentials
4.3 Orbital Changes due to Mass Transfer and Mass Loss in Binary Systems
4.4 Observational Examples
4.5 Basic Physics of Mass Transfer via L1
4.6 Accretion Disks
4.7 Tidal Evolution in Binary Systems
4.8 Common Envelopes
4.9 Eddington Accretion Limit
Exercises
5. Observed Binaries with Non-degenerate or White Dwarf Components
5.1 Introduction
5.2 Unevolved Systems
5.3 Evolved Systems with Non-degenerative Components
5.4 Systems with One or Two White Dwarfs
Exercises
6. Observed Binaries with Accreting Neutron Stars and Black Holes: X-ray Binaries
6.1 Discovery of NS and BH Character of Bright Galactic X-ray Sources
6.2 Two Types of Persistent Strong X-ray Sources: HMXBs and LMXBs
6.3 HMXBs and LMXBs vs. IMXBs
6.4 Determinations of NS Masses in X-ray Binaries
6.5 BH X-ray Binaries
6.6 Binaries and Triples with Non-interacting BHs
Exercises
7. Observed Properties of X-ray Binaries in More Detail
7.1 High-mass X-ray Binaries in More Detail
7.2 Stellar Wind Accretion in More Detail
7.3 Spin Evolution of Neutron Stars
7.4 The Corbet Diagram for Pulsating HMXBs
7.5 Orbital Changes due to Torques by Stellar Wind Accretion, Mass Loss, and Tides
7.6 Measuring BH Spins in X-ray Binaries
7.7 Ultra-luminous X-ray Binaries
7.8 Low-mass X-ray Binaries in More Detail
Exercises
8. Evolution of Single Stars
8.1 Overview of the Evolution of Single Stars
8.2 Final Evolution and Core Collapse of Stars More Massive than 8 M
8.3 Evolution of Helium Stars
Exercises
9. Stellar Evolution in Binaries
9.1 Historical Introduction: Importance of Mass Transfer
9.2 Evolution of the Stellar Radius and Cases of Mass Transfer
9.3 RLO: Reasons for Large-scale Mass Transfer and Conditions for Stability of the Transfer
9.4 Results of Calculations of Binary Evolution with Conservative Mass Transfer
9.5 Examples of Non-conservative Mass Transfer
9.6 Comparison of Case B Results with Some Observed Types of Systems
9.7 Differences in Final Remnants of Mass-transfer Binaries and Single Stars
9.8 Slowly Rotating Magnetic Main-sequence Stars: The Products of Mergers?
Exercises
10. Formation and Evolution of High-mass X-ray Binaries
10.1 Introduction: HMXBs are Normal Products of Massive Binary Star Evolution
10.2 Formation of Supergiant HMXBs
10.3 Formation of B-emission (Be)/X-ray Binaries
10.4 WR Binaries, HMXBs, and Runaway Stars
10.5 Stability of Mass Transfer in HMXBs
10.6 The X-ray Lifetime and Formation Rate of the Blue Supergiant HMXBs
10.7 Highly Non-conservative Evolution and Formation of Very Close Relativistic Binaries
10.8 Formation Models of HMXBs Different from Conservative Case B Evolution
10.9 The Lower Mass Limit of Binary Stars for Terminating as a BH
10.10 Final Evolution of BH-HMXBs: Two Formation Channels for Double BHs
10.11 Final Evolution of Wide-orbit BH-HMXBs via CE Evolution
10.12 Final Evolution of Relatively Close-orbit BH-HMXBs via Stable RLO
10.13 Refinement of the DNS Formation Model: Case BB RLO in Post-HMXB Systems
Exercises
11. Formation and Evolution of Low-mass X-ray Binaries
11.1 Origin of LMXBs with Neutron Stars
11.2 Origin of LMXBs with Black Holes
11.3 Mechanisms Driving Mass Transfer in Close-orbit LMXBs and CVs
11.4 Formation and Evolution of UCXBs
11.5 Mechanisms Driving Mass Transfer in Wide-orbit LMXBs and Symbiotic Binaries
11.6 Stability of Mass Transfer in Intermediate-Mass and High-Mass X-ray Binaries
Exercises
12. Dynamical Formation of Compact Star Binaries in Dense Star Clusters
12.1 Introduction
12.2 Observed Compact Object Binaries in Globular Clusters: X-ray Binaries and Radio Pulsars
12.3 Possible Formation Processes of NS Binaries in Globular Clusters
12.4 Dynamical Formation of Double BHs
12.5 Compact Objects in Globular Clusters Constrain Birth Kicks
13. Supernovae in Binaries
13.1 Introduction
13.2 Supernovae of Type Ia
13.3 Stripped-Envelope Core-Collapse SNe
13.4 Electron-capture SNe in Single and Binary Stars
13.5 Ultra-Stripped Supernovae
13.6 Comparison between Theory and Observations of SNe Ib and Ic
13.7 Supernova Kicks
13.8 Kinematic Impacts on Post-SN Binaries
Exercises
14. Binary and Millisecond Pulsars
14.1 Introduction to Radio Pulsars
14.2 To Be Recycled or Not to Be Recycled
14.3 MSPs with He WD or Sub-stellar Dwarf Companions-Evolution from LMXBs
14.4 MSPs with CO WD Companions-Evolution from IMXBs
14.5 Formation of MSPs via Accretion-induced Collapse
14.6 Recycling of Pulsars
14.7 Masses of Binary Neutron Stars
14.8 Pulsar Kicks
14.9 Formation of Double Neutron Star Systems
Exercises
15. Gravitational Waves from Binary Compact Objects
15.1 The Evidence of GWs prior to LIGO
15.2 GW Luminosity and Merger Timescale
15.3 Observations of GW Signals from Binaries
15.4 Galactic Merger Rates of Neutron Star/Black Hole Binaries
15.5 Formation of Double Black Hole Binaries
15.6 Properties of GW Sources Detected so Far
15.7 Empirical Merger Rates
15.8 BH Spins-Expectations and Observations
15.9 Anticipated Other Sources to be Detected in the GW Era
15.10 GW Follow-up Multimessenger Astronomy
15.11 Cosmological Implications
15.12 LISA Sources
15.13 LISA Sensitivity Curve and Source Strain
Exercises
16. Binary Population Synthesis and Statistics
16.1 Introduction
16.2 Methodology of Population Synthesis
16.3 Empirical vs. Binary Population Synthesis-Based Estimates of Double Compact Object Merger Rates
16.4 Some History of Early Binary Population Synthesis: Evolution of Open Star Clusters with Binaries
Acknowledgments
Answers to Exercises
List of Acronyms
References
Index

Systemvoraussetzungen

Als PDF speichern Als Link merken