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Black holes in the era of gravitational-wave astronomy /

This comprehensive volume explores the formation, evolution, and observational aspects of black holes in various astronomical contexts. Edited by leading researchers, it covers topics such as stellar and binary black hole systems, black holes in star clusters and dwarf galaxies, and massive black ho...

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Bibliographic Details
Corporate Author: ScienceDirect (Online service)
Other Authors: Sedda, Manuel Arca, Bortolas, Elisa, Spera, Mario
Format: eBook
Language:English
Published: Amsterdam : Elsevier, 2024.
Subjects:
Black holes (Astronomy)
Celestial mechanics.
Trous noirs (Astronomie)
Mécanique céleste.
Electronic books.
Online Access:Connect to the full text of this electronic book
Table of Contents:
  • Front Cover
  • Black Holes in the Era of Gravitational-Wave Astronomy
  • Copyright
  • Contents
  • Contributors
  • About the editors
  • Preface
  • 1 Stellar black holes and compact stellar remnants
  • 1.1 Stellar evolution: single stars
  • 1.1.1 Introduction
  • 1.1.2 Overview on stellar evolution
  • 1.1.2.1 Historical background
  • 1.1.2.2 Mass ranges and stellar remnants
  • 1.1.2.3 The HR diagram
  • 1.1.3 Main physical processes that affect life and death of massive stars
  • 1.1.3.1 Convection and overshooting
  • 1.1.3.1.1 Defining the convective borders
  • 1.1.3.1.2 Convective boundary mixing or overshooting
  • 1.1.3.2 Mass loss through stellar winds
  • 1.1.3.3 Rotation and magnetic fields
  • 1.1.3.3.1 Stellar rotation
  • 1.1.3.3.2 Magnetic fields
  • 1.1.3.4 Final phases: supernovæ, core collapse, and pair instability
  • 1.1.3.4.1 Core collapse and supernova engines
  • 1.1.3.4.2 Electron-capture and pair-instability supernovæ
  • 1.1.4 Summary
  • 1.2 Stellar evolution: binaries
  • 1.2.1 Introduction
  • 1.2.2 Mass exchange
  • 1.2.2.1 When: evolution of stellar radii
  • 1.2.2.2 How: stability of mass transfer
  • 1.2.2.2.1 Roche lobe radius
  • 1.2.2.2.2 Donor radius and its response to mass loss
  • 1.2.2.2.3 Combining the two: stability criteria and the mass transfer timescales
  • 1.2.2.3 Mass transfer: effect on the evolution
  • 1.2.2.3.1 Impact on the orbit: stable mass transfer case
  • 1.2.2.3.2 Impact on the orbit: unstable (CE) case
  • 1.2.2.3.3 Impact on the donor star
  • 1.2.2.3.3.1 Early mass transfer maximizes the differences with respect to single star evolution
  • 1.2.2.3.3.2 Fully or partially stripped (and why it matters)
  • 1.2.2.3.4 Impact on the accretor: stellar accretors
  • 1.2.2.3.4.1 Rejuvenation and core growth (or lack thereof)
  • 1.2.2.3.4.2 Spin-up (followed by the likely spin-down).
  • 1.2.2.3.5 Impact on the accretor: BH accretors
  • 1.2.2.3.5.1 How much mass can a BH accrete?
  • 1.2.2.3.5.2 Is Eddington accretion the limit?
  • 1.2.2.3.5.3 How much can a BH spin up?
  • 1.2.2.3.5.4 Can BHs accrete non-negligible mass (and spin up) during the CE?
  • 1.2.3 Other relevant binary processes
  • 1.2.3.1 Tidal forces: effect on spins and orbit
  • 1.2.3.1.1 Chemically homogeneous evolution
  • 1.2.3.1.2 Tidal spin up of the immediate BH progenitor
  • 1.2.3.2 Orbital evolution due to gravitational wave emission
  • 1.2.3.3 Magnetic braking
  • 1.2.4 Summary
  • 1.3 Black holes in binaries: formation channels
  • isolated
  • 1.3.1 Introduction: the new frontier of GW paleontology
  • 1.3.2 Formation pathways to GW sources
  • 1.3.2.1 The separation challenge
  • 1.3.2.2 Formation channels
  • 1.3.2.2.1 Isolated binary evolution formation channel (N=2)
  • 1.3.2.3 Other formation channels
  • 1.4 Black holes in binaries: formation channels
  • dynamical
  • 1.4.1 N=3
  • triples and three-body encounters
  • 1.4.1.1 Hierarchical triples
  • 1.4.1.2 Democratic triples
  • 1.4.2 N=O(103−105)
  • open clusters
  • 1.4.3 N=O(104−107)
  • globular clusters
  • 1.4.3.1 Observational signatures of purely dynamical formation
  • 1.4.4 N=O(105−108)
  • nuclear star clusters
  • 1.4.4.1 GN without SMBHs
  • 1.4.4.2 GN with SMBHs
  • 1.5 Black holes in binaries through observations: X-ray, detached, lensing, LIGO
  • 1.5.1 Introduction
  • 1.5.2 Isolated black holes
  • 1.5.3 Black holes in binary systems with luminous companions
  • 1.5.3.1 Black holes in interacting systems
  • 1.5.3.1.1 Development of electromagnetic detection methods for X-ray binaries
  • 1.5.3.1.2 Types of X-ray binaries
  • 1.5.3.1.2.1 High mass X-ray binaries
  • 1.5.3.1.2.2 Low mass X-ray binaries
  • 1.5.3.1.2.3 IMXBs
  • 1.5.3.1.2.4 ULXs
  • 1.5.3.1.2.5 Finding black hole X-ray binaries.
  • 1.5.3.1.3 Accretion physics in X-ray binaries
  • 1.5.3.1.3.1 The accretion disk
  • 1.5.3.1.3.2 Properties of the accretion disk
  • 1.5.3.1.3.3 The multicolor disk model
  • 1.5.3.1.3.4 Deviation from the standard accretion disk model
  • 1.5.3.1.3.5 The disk instability model
  • 1.5.3.1.4 Electromagnetic observational signatures of black hole binaries
  • 1.5.3.1.4.1 Black hole binary X-ray emission states
  • 1.5.3.1.4.2 Black hole binary timing signatures
  • 1.5.3.2 Black holes in non-interacting systems
  • 1.5.3.2.1 Spectroscopic detection of quiescent black holes
  • 1.5.3.2.1.1 Quiescent black holes in low-density fields
  • 1.5.3.2.1.2 Quiescent black holes in high-density fields
  • 1.5.3.2.2 Astrometric detection of quiescent black holes
  • 1.5.4 Black holes in binaries with compact objects
  • 1.5.4.1 Gravitational waves
  • 1.5.4.1.1 What are gravitational waves?
  • 1.5.4.1.2 Types of gravitational waves
  • 1.5.4.1.3 Gravitational wave sources
  • 1.5.4.2 Gravitational waves detectors
  • 1.5.4.2.1 Indirect detection methods
  • 1.5.4.2.2 Direct detection methods
  • 1.5.4.2.2.1 Resonant mass detectors
  • 1.5.4.2.2.2 Laser interferometers
  • 1.5.4.2.2.3 Other detector designs
  • 1.5.4.3 Gravitational wave detections
  • 1.5.4.3.1 Indirect detections
  • 1.5.4.3.2 Direct detections
  • Acknowledgments
  • References
  • 2 Intermediate-mass black holes in star clusters and dwarf galaxies
  • 2.1 Intermediate-mass black holes in star clusters and dwarf galaxies: formation and growth
  • 2.1.1 Introduction
  • 2.1.1.1 Context and definition
  • 2.1.1.2 Relevance
  • 2.1.2 Formation pathways of IMBHs
  • 2.1.2.1 Evolutionary remnants of massive metal-free and metal-poor stars
  • 2.1.2.1.1 Accretion driven growth of stellar-mass BHs that formed from pop III and metal-poor stars
  • 2.1.2.2 IMBH formation in dense stellar environments.
  • 2.1.2.2.1 Dynamical evolution of star clusters
  • 2.1.2.2.2 Modelling the evolution of star clusters
  • 2.1.2.2.3 Formation and retention of stellar-mass BHs in star clusters: natal kicks and dynamics
  • 2.1.2.2.4 Overview of IMBH formation pathways in star clusters
  • 2.1.2.2.5 Repeated or hierarchical mergers of stellar-mass BHs
  • 2.1.2.2.5.1 Segregation of stellar-mass BHs due to dynamical friction
  • 2.1.2.2.5.2 Dynamical BBH formation and hardening
  • 2.1.2.2.5.3 BBHs from binary evolution and their hardening
  • 2.1.2.2.5.4 Gravitational wave recoil kick and merged BH retention
  • 2.1.2.2.6 Fast runaway: stellar collisions resulting in IMBH formation
  • 2.1.2.2.6.1 Segregation of massive stars and collisional formation of a very massive star
  • 2.1.2.2.6.2 Evolution of a very massive star and IMBH formation
  • 2.1.2.2.7 Slow runaway: gradual growth of a stellar-mass BH
  • 2.1.2.2.7.1 Collision between BHs and stars
  • 2.1.2.2.7.2 Tidal disruption and capture events
  • 2.1.2.2.8 Rapid stellar mergers leading to low-mass IMBH formation
  • 2.1.2.2.9 Gas accretion by stellar-mass BHs
  • 2.1.2.2.10 IMBH formation in AGN disks
  • 2.1.3 Gravitational waves from IMBH mergers with other BHs
  • 2.1.3.1 Light IMRIs: mergers between IMBH and sBHs
  • 2.1.3.2 Binary IMBHs
  • 2.1.3.3 Heavy IMRIs: mergers between IMBH and SMBHs
  • 2.1.4 Summary
  • 2.2 Intermediate-mass black holes in star clusters and dwarf galaxies: observations
  • 2.2.1 Introduction
  • 2.2.2 Globular clusters
  • 2.2.2.1 Dynamical BH mass measurements
  • 2.2.2.2 Signatures of BH accretion
  • 2.2.3 Dwarf galaxies
  • 2.2.3.1 Dynamical BH masses
  • 2.2.3.2 Optical spectroscopy
  • 2.2.3.3 Optical variability
  • 2.2.3.4 Infrared spectroscopy
  • 2.2.3.5 Mid-infrared colors
  • 2.2.3.6 Radio observations
  • 2.2.3.7 X-ray observations
  • 2.2.4 Gravitational waves
  • 2.2.4.1 LIGO detections.
  • 2.2.4.2 LIGO-LISA predictions
  • Acknowledgments
  • References
  • 3 Massive black holes in galactic nuclei
  • 3.1 Supermassive black holes and their environments
  • 3.1.1 Introduction
  • 3.1.2 Historical overview
  • 3.1.3 The coupled evolution of galaxies and SMBHs
  • 3.1.3.1 An observational point of view on the physics behind the scaling relations
  • 3.1.3.1.1 A theoretical point of view on the physics behind the scaling relations
  • 3.1.3.1.2 Processes impacting the coevolution between galaxies and SMBHs: gravitational recoils
  • 3.2 The formation scenarios of SMBHs
  • 3.2.1 Introduction
  • 3.2.1.1 Light seeds
  • 3.2.1.2 Heavy seeds generated in nuclear star clusters
  • 3.2.1.3 Heavy seeds generated from (super-)massive stars
  • 3.2.1.3.1 Lyman-Werner irradiation
  • 3.2.1.3.2 Rapid assembly
  • 3.2.1.3.3 Baryonic streaming motions
  • 3.2.1.4 Exotic formation channels
  • 3.2.1.5 Differentiating seed formation channels through observations
  • 3.3 Massive black hole binaries
  • 3.3.1 Introduction
  • 3.3.1.1 The large-scale inspiral
  • 3.3.1.1.1 The simplest approximation: the collisionless isothermal sphere
  • 3.3.1.1.2 The impact of different density profiles
  • 3.3.1.1.3 Axisymmetric distributions: the effect of discs
  • 3.3.1.1.4 Dynamical friction in gaseous environments
  • 3.3.1.1.5 Time evolution of the main galaxy
  • 3.3.1.1.6 Global asymmetries: galactic bars
  • 3.3.1.1.7 The transition to the small scale inspiral
  • 3.3.1.2 The small-scale inspiral: hardening in stellar backgrounds
  • 3.3.1.2.1 Binary-star interaction: energy and angular momentum exchanges
  • 3.3.1.2.2 Binary hardening: analytical estimates and scattering experiments
  • 3.3.1.2.3 Evolution in realistic galactic environments
  • 3.3.1.3 The small-scale inspiral: triplets and multiplets
  • 3.3.1.3.1 The three-body problem
  • 3.3.1.3.2 The formation of MBH triplets.