單星的結構與演化--導論(英文版)/國外優秀物理著作原版系列
內容大鋼
本書是一部版權引進的天文學英文原版教材，是作者過去15年在特拉華大學定期教授的恆星天體物理學課程筆記的補充，它面向的讀者為高年級的本科生和剛剛開始天文研究的研究生，本書讀者熟悉經典力學、量子力學、統計物理學和熱力學的相關知識。
作者介紹
(美)詹姆斯·麥克唐納|責編:聶兆慈//李蘭靜
本書作者為詹姆斯·麥克唐納（JamesMacDonald），他于1979年在劍橋大學獲得天文學博士學位，之後成為薩塞克斯大學、伊利諾伊大學和亞利桑那州立大學的博士后，于1985年加入特拉華大學，現在是物理學和天文學教授，他的研究方向是恆星的結構和演化，最近的工作集中在低質量主序星和褐矮星上，並在同行評審期刊上發表了80多篇論文。
目錄
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
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