天文光谱学——天文光谱的原子与分子物理学导论（第二版）(英文影印版)

　　Preface
　　1.Why Record Spectra of Astronomical Objects?
　　  1.1  A Historical Introduction
　　  1.2  What One Can Learn from Studying Spectra
　　2.The Nature of Spectra
　　  2.1  Transitions
　　  2.2  Absorption and Emission
　　  2.3  Other Measures of Transition Probabilities
　　  2.4  Stimulated Emission
　　  2.5  Optical Depth
　　  2.6  Critical Density
　　  2.7  Wavelength or Frequency?
　　  2.8  The Electromagnetic Spectrum
　　3.Atomic Hydrogen
　　  3.1  Overview
　　  3.2  The Schrodinger Equation of Hydrogen-Like Atoms
　　  3.3  Reduced Mass
　　  3.4  Atomic Units
　　  3.5  Wavefunctions for Hydrogen
　　  3.6  Energy Levels and Quantum Numbers
　　  3.7  H-Atom Discrete Spectra
　　  3.8  H-Atom Spectra in Different Locations
　　    3.8.1  Balmer series
　　    3.8.2  Lyman series
　　    3.8.3  Infrared lines
　　  3.9  H-Atom Continuum Spectra
　　    3.9.1  Processes
　　    3.9.2  H-atom emission in H II regions
　　  3.10  Radio Recombination Lines
　　  3.11  Radio Recombination Lines for Other Atoms
　　  3.12  Angular Momentum Coupling in the Hydrogen Atom
　　  3.13  The Fine Structure of Hydrogen
　　  3.14  Hyperfine Structure in the H Atom
　　  3.15  Allowed Transitions
　　  3.16  Hydrogen in Nebulae
　　4.Complex Atoms
　　  4.1  General Considerations
　　  4.2  Central Field Model
　　  4.3  Indistinguishable Particles
　　  4.4  Electron Configurations
　　  4.5  The Periodic Table
　　  4.6  Ions
　　  4.7  Angular Momentum in Complex Atoms
　　    4.7.1  L-S or Russell-Saunders coupling
　　    4.7.2  j-j coupling
　　    4.7.3  Why two coupling schemes?
　　  4.8  Spectroscopic Notation
　　  4.9  Parity of the Wavefunction
　　  4.10  Terms and Levels in Complex Atoms
　　5.Helium Spectra
　　  5.1  He I and He II Spectra
　　  5.2  Selection Rules for Complex Atoms
　　  5.3  Observing Forbidden Lines
　　  5.4  Grotrian Diagrams
　　  5.5  Potential Felt by Electrons in Complex Atoms
　　  5.6  Emissions of Helium-Like Ions
　　6.Alkali Atoms
　　  6.1  Sodium
　　  6.2  Spin-Orbit Interactions
　　  6.3  Fine Structure Transitions
　　  6.4  Astronomical Sodium Spectra
　　  6.5  Other Alkali Metal-Like Spectra
　　7.Spectra of Nebulae
　　  7.1  Nebulium
　　  7.2  The Bowen Mechanism
　　  7.3  Two Valence Electrons
　　  7.4  Autoionisation and Recombination
　　8.Spectra in Magnetic Fields
　　  8.1  Uniform Magnetic Field
　　  8.2  Strong Magnetic Field
　　  8.3  Weak Magnetic Field
　　    8.3.1  The normal Zeeman effect
　　    8.3.2  The anomolous Zeeman effect
　　  8.4  Spectra in Magnetic Field
　　9.X-Ray Spectra
　　  9.1  Inner Shell Processes
　　  9.2  The Solar Corona
　　  9.3  The Structure of Highly Ionised Atoms
　　  9.4  Isotope Effects
　　10.Molecular Structure
　　  10.1  The Born-Oppenheimer Approximation
　　  10.2  Electronic Structure of Diatomics
　　    10.2.1  Labelling of electronic states
　　    10.2.2 Symmetry
　　    10.2.3 State labels
　　  10.3  Schrodinger Equation
　　    10.3.1  Nuclear motion in diatomic molecules
　　  10.4  Fractionation
　　  10.5  Vibration-Rotation Energy Levels
　　  10.6  Temperature Effects
　　    10.6.1  Rotational state populations
　　    10.6.2  Vibrational state populations
　　    10.6.3  Electronic state populations
　　11.Rotational Spectra
　　  11.1  Rotational Structure of Polyatomic Molecules
　　  11.2  Selection Rules: Pure Rotational Transitions
　　  11.3  Selection Rules
　　  11.4  Isotope Effects
　　  11.5  Rotational Spectra of Other Molecules
　　  11.6  Rotational Spectra of Molecular Hydrogen
　　  11.7  Maser Emissions
　　12.Vibration-Rotation Spectra
　　  12.1  Vibrations in Polyatomic Molecules
　　  12.2  Vibrational Transitions
　　    12.2.1  Structure of the spectrum
　　    12.2.2  Isotope effects
　　    12.2.3  Hydrogen molecule vibrational spectra
　　  12.3  Astronomical Spectra
　　13.Electronic Spectra of Diatomic Molecules
　　  13.1  Electronic Transitions
　　  13.2  Selection Rules
　　    13.2.1  Vibrational selection rules
　　    13.2.2  Rotational selection rules
　　  13.3  Transition Frequencies
　　  13.4  Astronomical Spectra
　　  13.5  Non-E Electronic States
　　Solutions to Model Problems
　　Further Reading and Bibliography
　　Index

　　（英）坦尼森，伦敦大学学院教授。

　　对于宇宙的观测，其信息几乎都来自于光。观测一方面要把光分解成各种成分，另一方面也要了解原子和分子的性质。《天文光谱学——天文光谱的原子与分子物理学导论（第二版）(英文影印版)》对于这两方面都进行了系统讲述。在天文光谱学的研究中，本书能够提供丰富而实用的知识。
　　《天文光谱学——天文光谱的原子与分子物理学导论（第二版）(英文影印版)》适合天文学领域的研究者和研究生阅读。