Efnisyfirlit

• Cover
• Half Title
• Title Page
• Copyright
• Dedication
• Contents
• Preface
• Acknowledgements
• Part I: Astronomical background
• 1. High energy astrophysics – an introduction
• 1.1 High energy astrophysics and modern physics and astronomy
• 1.2 The sky in different astronomical wavebands
• 1.3 Optical waveband
• 1.4 Infrared waveband
• 1.5 Millimetre and submillimetre waveband
• 1.6 Radio waveband
• 1.7 Ultraviolet waveband
• 1.8 X-ray waveband
• 1.9 γ-ray waveband
• 1.10 Cosmic ray astrophysics
• 1.11 Other non-electromagnetic astronomies
• 1.12 Concluding remarks
• 2. The stars and stellar evolution
• 2.1 Introduction
• 2.2 Basic observations
• 2.3 Stellar structure
• 2.4 The equations of energy generation and energy transport
• 2.5 The equations of stellar structure
• 2.6 The Sun as a star
• 2.7 Evolution of high and low mass stars
• 2.8 Stellar evolution on the colour–magnitude diagram
• 2.9 Mass loss
• 2.10 Conclusion
• 3. The galaxies
• 3.1 Introduction
• 3.2 The Hubble sequence
• 3.3 The red and blue sequences
• 3.4 Further correlations among the properties of galaxies
• 3.5 The masses of galaxies
• 3.6 The luminosity function of galaxies
• 4. Clusters of galaxies
• 4.1 The morphologies of rich clusters of galaxies
• 4.2 Clusters of galaxies and isothermal gas spheres
• 4.3 The Coma Cluster of galaxies
• 4.4 Mass distribution of hot gas and dark matter in clusters
• 4.5 Cooling flows in clusters of galaxies
• 4.6 The Sunyaev–Zeldovich effect in hot intracluster gas
• 4.7 Gravitational lensing by galaxies and clusters of galaxies
• 4.8 Dark matter in galaxies and clusters of galaxies
• Part II: Physical processes
• 5. Ionisation losses
• 5.1 Introduction
• 5.2 Ionisation losses – non-relativistic treatment
• 5.3 The relativistic case
• 5.4 Practical forms of the ionisation loss formulae
• 5.5 Ionisation losses of electrons
• 5.6 Nuclear emulsions, plastics and meteorites
• 5.7 Dynamical friction
• 6. Radiation of accelerated charged particles and bremsstrahlung of electrons
• 6.1 Introduction
• 6.2 The radiation of accelerated charged particles
• 6.3 Bremsstrahlung
• 6.4 Non-relativistic bremsstrahlung energy loss rate
• 6.5 Thermal bremsstrahlung
• 6.6 Relativistic bremsstrahlung
• 7. The dynamics of charged particles in magnetic fields
• 7.1 A uniform static magnetic field
• 7.2 A time-varying magnetic field
• 7.3 The scattering of charged particles by irregularities in the magnetic field
• 7.4 The scattering of high energy particles by Alfvén and hydromagnetic waves
• 7.5 The diffusion-loss equation for high energy particles
• 8. Synchrotron radiation
• 8.1 The total energy loss rate
• 8.2 Non-relativistic gyroradiation and cyclotron radiation
• 8.3 The spectrum of synchrotron radiation – physical arguments
• 8.4 The spectrum of synchrotron radiation – a fuller version
• 8.5 The synchrotron radiation of a power-law distribution of electron energies
• 8.6 The polarisation of synchrotron radiation
• 8.7 Synchrotron self-absorption
• 8.8 Useful numerical results
• 8.9 The radio emission of the Galaxy
• 9. Interactions of high energy photons
• 9.1 Photoelectric absorption
• 9.2 Thomson and Compton scattering
• 9.3 Inverse Compton scattering
• 9.4 Comptonisation
• 9.5 The Sunyaev–Zeldovich effect
• 9.6 Synchrotron–self-Compton radiation
• 9.7 Cherenkov radiation
• 9.8 Electron–positron pair production
• 9.9 Electron–photon cascades, electromagnetic showers and the detection of ultra-high energy γ-rays
• 9.10 Electron–positron annihilation and positron production mechanisms
• 10. Nuclear interactions
• 10.1 Nuclear interactions and high energy astrophysics
• 10.2 Spallation cross-sections
• 10.3 Nuclear emission lines
• 10.4 Cosmic rays in the atmosphere
• 11. Aspects of plasma physics and magnetohydrodynamics
• 11.1 Elementary concepts in plasma physics
• 11.2 Magnetic flux freezing
• 11.3 Shock waves
• 11.4 The Earth’s magnetosphere
• 11.5 Magnetic buoyancy
• 11.6 Reconnection of magnetic lines of force
• Part III: High energy astrophysics in our Galaxy
• 12. Interstellar gas and magnetic fields
• 12.1 The interstellar medium in the life cycle of stars
• 12.2 Diagnostic tools – neutral interstellar gas
• 12.3 Ionised interstellar gas
• 12.4 Interstellar dust
• 12.5 An overall picture of the interstellar gas
• 12.6 Star formation
• 12.7 The Galactic magnetic field
• 13. Dead stars
• 13.1 Supernovae
• 13.2 White dwarfs, neutron stars and the Chandrasekhar limit
• 13.3 White dwarfs
• 13.4 Neutron stars
• 13.5 The discovery of neutron stars
• 13.6 The Galactic population of neutron stars
• 13.7 Thermal emission of neutron stars
• 13.8 Pulsar glitches
• 13.9 The pulsar magnetosphere
• 13.10 The radio and high energy emission of pulsars
• 13.11 Black holes
• 14. Accretion power in astrophysics
• 14.1 Introduction
• 14.2 Accretion – general considerations
• 14.3 Thin accretion discs
• 14.4 Thick discs and advective flows
• 14.5 Accretion in binary systems
• 14.6 Accreting binary systems
• 14.7 Black holes in X-ray binaries
• 14.8 Final thoughts
• 15. Cosmic rays
• 15.1 The energy spectra of cosmic ray protons and nuclei
• 15.2 The abundances of the elements in the cosmic rays
• 15.3 The isotropy and energy density of cosmic rays
• 15.4 Gamma ray observations of the Galaxy
• 15.5 The origin of the light elements in the cosmic rays
• 15.6 The confinement time of cosmic rays in the Galaxy and cosmic ray clocks
• 15.7 The confinement volume for cosmic rays
• 15.8 The Galactic halo
• 15.9 The highest energy cosmic rays and extensive air-showers
• 15.10 Observations of the highest energy cosmic rays
• 15.11 The isotropy of ultra-high energy cosmic rays
• 15.12 The Greisen–Kuzmin–Zatsepin (GKZ) cut-off
• 16. The origin of cosmic rays in our Galaxy
• 16.1 Introduction
• 16.2 Energy loss processes for high energy electrons
• 16.3 Diffusion-loss equation for high energy electrons
• 16.4 Supernova remnants as sources of high energy particles
• 16.5 The minimum energy requirements for synchrotron radiation
• 16.6 Supernova remnants as sources of high energy electrons
• 16.7 The evolution of supernova remnants
• 16.8 The adiabatic loss problem and the acceleration of high energy particles
• 17. The acceleration of high energy particles
• 17.1 General principles of acceleration
• 17.2 The acceleration of particles in solar flares
• 17.3 Fermi acceleration – original version
• 17.4 Diffusive shock acceleration in strong shock waves
• 17.5 Beyond the standard model
• 17.6 The highest energy cosmic rays
• Part IV: Extragalactic high energy astrophysics
• 18. Active galaxies
• 18.1 Introduction
• 18.2 Radio galaxies and high energy astrophysics
• 18.3 The quasars
• 18.4 Seyfert galaxies
• 18.5 Blazars, superluminal sources and γ-ray sources
• 18.6 Low Ionisation Nuclear Emission Regions – LINERs
• 18.7 Ultra-Luminous InfraRed Galaxies – ULIRGs
• 18.8 X-ray surveys of active galaxies
• 18.9 Unification schemes for active galaxies
• 19. Black holes in the nuclei of galaxies
• 19.1 The properties of black holes
• 19.2 Elementary considerations
• 19.3 Dynamical evidence for supermassive black holes in galactic nuclei
• 19.4 The Soltan argument
• 19.5 Black holes and spheroid masses
• 19.6 X-ray observations of fluorescence lines in active galactic nuclei
• 19.7 The growth of black holes in the nuclei of galaxies
• 20. The vicinity of the black hole
• 20.1 The prime ingredients of active galactic nuclei
• 20.2 The continuum spectrum
• 20.3 The emission line regions – the overall picture
• 20.4 The narrow-line regions – the example of Cygnus A
• 20.5 The broad-line regions and reverberation mapping
• 20.6 The alignment effect and shock excitation of emission line regions
• 20.7 Accretion discs about supermassive black holes
• 21. Extragalactic radio sources
• 21.1 Extended radio sources – Fanaroff–Riley types
• 21.2 The astrophysics of FR2 radio sources
• 21.3 The FR1 radio sources
• 21.4 The microquasars
• 21.5 Jet physics
• 22. Compact extragalactic sources and superluminal motions
• 22.1 Compact radio sources
• 22.2 Superluminal motions
• 22.3 Relativistic beaming
• 22.4 The superluminal source population
• 22.5 Synchro-Compton radiation and the inverse Compton catastrophe
• 22.6 γ-ray sources in active galactic nuclei
• 22.7 γ-ray bursts
• 23. Cosmological aspects of high energy astrophysics
• 23.1 The cosmic evolution of galaxies and active galaxies
• 23.2 The essential theoretical tools
• 23.3 The evolution of non-thermal sources with cosmic epoch
• 23.4 The evolution of thermal sources with cosmic epoch
• 23.5 Mid- and far-infrared number counts
• 23.6 Submillimetre number counts
• 23.7 The global star-formation rate
• 23.8 The old red galaxies
• 23.9 Putting it all together
• Appendix: Astronomical conventions and nomenclature
• A.1 Galactic coordinates and projections of the celestial sphere onto a plane
• A.2 Distances in astronomy
• A.3 Masses in astronomy
• A.4 Flux densities, luminosities, magnitudes and colours
• A.5 Diffraction-limited telescopes
• A.6 Interferometry and synthesis imaging
• A.7 The sensitivities of astronomical detectors
• A.8 Units and relativistic notation
• Bibliography
• Name index
• Object index
• Index