Preface Acknowledgements Author biography 1 Observational background 1.1 Distances 1.2 Stellar brightness and luminosity 1.3 Colors 1.4 Spectroscopy 1.5 Color-magnitude diagrams 1.6 Stellar masses 1.7 The mass-luminosity relation for main sequence stars 1.8 The mass-radius relation for main sequence stars Bibliography 2 The equations of stellar structure: mass conservation and hydrostatic equilibrium 2.1 Introduction 2.2 The mass conservation equation 2.3 The hydrostatic equilibriu m equation for a spherical star 2.4 The dynamical time scale 2.5 The central temperature of the Sun 2.6 The central temperatures of main sequence stars 2.7 Radiation pressure 3 Energy considerations, the source of the Sun's energy, and energy transport 3.1 Introduction 3.2 The virial theorem 3.3 The virial theorem for stars in hydrostatic equilibrium 3.4 The conservation of energy equation for a star in hydrostatic equilibrium 3.5 Stars in thermal equilibrium 3.6 Energy transport 3.7 The equation of radiative transfer 3.8 Optical depth and effective temperature 3.9 Validity of the diffusion approximation Bibliography 4 Convective energy transport 4.1 Introduction 4.2 The Schwarzschild criterion for convective instability 4.3 Including convective energy transport in stellar models Bibliography 5 The equations of stellar evolution and how to solve them 5.1 Introduction 5.2 The equations of stellar structure 5.3 The physical significance of the Eddington luminosity 5.4 Equations for composition changes 5.5 Solving the equations of stellar evolution 5.6 The Newton-Raphson method 5.7 Sets of non-linear equations Bibliography 6 Physics of gas and radiation 6.1 Introduction
6.2 The ideal gas equation of state 6.3 The radiation equation of state 6.4 The equation of state for a mixture of ideal gas and radiation 6.5 The Eddington standard model of stellar structure Bibliography 7 Ionization and recombination 7.1 Introduction 7.2 The Boltzmann excitation equation 7.3 The Saha ionization equation 7.4 A difficulty and its resolution 7.5 Ionization of hydrogen 7.6 The effect of ionization on the adiabatic gradient 7.7 The effect of ionization on the specific heat 7.8 Pressure ionization 7.9 Free energy approach to ionization 7.10 A crude model for inclusion of pressure ionization in a thermodynamically consistent way Bibliography 8 The degenerate electron gas 8.1 Introduction 8.2 Complete electron degeneracy 8.3 Limiting forms 8.4 The contribution from nuclei at zero temperature 8.5 Transition from non-degeneracy to degeneracy 8.6 Effects of degeneracy on the adiabatic gradient and the first adiabatic exponent 「 ua 「 9 Polytropes and the Chandrasekhar mass 9.1 Introduction 9.2 The Lane-Emden equation 9.3 Application to white dwarf stars Bibliography 10 Opacity 10.1 Introduction 10.2 The Rosseland mean opacity 10.3 Opacity mechanisms 10.4 Electron scattering opacity 10.5 Free-free opacity 10.6 Bound-free opacity 10.7 Bound-bound opacity 10.8 The Rosseland mean opacity for solar composition material Bibliography 11 Nuclear reactions 11.1 Introduction 11.2 Occurrence of thermonuclear reactions 11.3 Cross sections and nuclear reaction rates 11.4 The cross section 11.5 Evaluation of the reaction rate 11.6 Major nuclear burning stages in stars: H burning 11.7 Energy generation in the pp-chains and the CNO-cycles 11.8 Major nuclear burning stages in stars: He burning
11.9 Advanced nuclear burning phases Bibliography 12 Neutrino energy loss processes 12.1 Pair annihilation neutrino process (e++e- →v + ) 12.2 Plasma neutrino process (/plamon→v +i) 12.3 Photo-neutrino process (y + e→e +v +D) 12.4 Bremsstrahlung neutrino process Bibiography 13 Homology relations 13.1 Introduction 13.2 Homology of zero age main sequence stars 13.3 Sensitivity of stellar structure to nuclear reaction rate 13.4 Sensitivity of stellar properties to composition 13.5 Stars with convective cores 13.6 Stars with convective envelopes 14 Hydrogen main sequence stars 14.I Masses of main sequence stars 14.2 Lifetimes of main sequence stars 14.3 Convection in main sequence stars 14.4 Variation of surface properties with mass 14.5 Variation of central properties with mass 14.6 The theoretical Hertzsprung-Russell diagram Bibliography 15 Helium main sequence stars 15.1 Why consider helium main sequence stars? 15.2 Homology analysis of helium zero age main sequence stars 15.3 Convection in helium main sequence stars 15.4 Variation of surface properties with mass 15.5 Variation of central properties with mass 15.6 The theoretical Hertzsprung-Russell diagram Bibliography 16 The Hayashi line 16.1 Introduction 16.2 The Hayashi phase Bibiography 17 Star formation 17.1 Introduction 17.2 The Jeans mass 17.3 Fragmentation Bibliography 18 Evolution on the main sequence and beyond 18.1 Introduction 18.2 Change in luminosity on the main sequence 18.3 Evolution of the hydrogen profile 18.4 Evolution after hydrogen exhaustion in the core 18.5 The Hertzsprung gap Bibliography 19 Evolution on the red giant branch 19.1 Introduction 19.2 Change in luminosity on the red giant branch
19.3 The globular cluster luminosity function bump 19.4 The helium core flash 19.5 Stability considerations Bibliography 20 Evolution from red giant to white dwarf 20.1 Introduction 20.2 The horizontal branch 20.3 The asymptotic giant branch 20.4 The formation of planetary nebulae 20.5 The cooling of white dwarfs 20.6 The luminosity function of white dwarfs 20.7 Masses of white dwarf stars: observational material Bibliography 21 Evolution of massive stars 21.1 Introduction 21.2 Composition changes in the core 21.3 Evolution after the end of core helium burning 21.4 Evolution of stars more massive than 8 Mo Bibliography 編輯手記
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