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 Introduc
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