单星的结构与演化：导论（英文）

作者: [美] 詹姆斯·麦克唐纳著

出版社: 哈尔滨工业大学出版社

出版时间: 2021-06

版次: 1

ISBN: 9787560394305

定价: 108.00

装帧: 平装

开本: 16开

页数: 220页

分类: 自然科学

本书是一部版权引进的天文学英文原版教材。本书是作者过去15年在特拉华大学定期教授的恒星天体物理学课程笔记的补充，书中大量使用了被称为埃格尔顿( Eggleton)代码的基于恒星结构和演化的计算得出的数据。本书作者为詹姆斯・麦克唐纳（JamesMacDonald），他于1979年在剑桥大学获得天文学博士学位，之后成为萨塞克斯大学、伊利诺伊大学和亚利桑那州立大学的博士后，于1985年加入特拉华大学，现在是物理学和天文学教授，他的研究方向是恒星的结构和演化，最近的工作集中在低质量主序星和褐矮星上，并在同行评审期刊上发表了80多篇论文。 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
内容简介:
本书是一部版权引进的天文学英文原版教材。本书是作者过去15年在特拉华大学定期教授的恒星天体物理学课程笔记的补充，书中大量使用了被称为埃格尔顿( Eggleton)代码的基于恒星结构和演化的计算得出的数据。
作者简介:
本书作者为詹姆斯・麦克唐纳（JamesMacDonald），他于1979年在剑桥大学获得天文学博士学位，之后成为萨塞克斯大学、伊利诺伊大学和亚利桑那州立大学的博士后，于1985年加入特拉华大学，现在是物理学和天文学教授，他的研究方向是恒星的结构和演化，最近的工作集中在低质量主序星和褐矮星上，并在同行评审期刊上发表了80多篇论文。
目录:
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