天文光谱学-天文光谱的原子分子物理学导论-引进系列.57-第二版-(影印版)_PDF下载[80MB-百度云]坦尼森

本书特色

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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。

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内容简介

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观测宇宙主要靠光。对于光的分析，光谱分析至关重要。另外，对于分子和原子物理学的研究对光谱分析也是必不可少的。《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)》综合了两方面的知识，是相关领域研究不可多得的佳作。

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preface1.why record spectra of astronomical objects? 1.1 a historical introduction 1.2 what one can learn from studying spectra2.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 spectrum3.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 nebulae4.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 atoms5.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 ions6.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 spectra7.spectra of nebulae 7.1 nebulium 7.2 the bowen mechanism 7.3 two valence electrons 7.4 autoionisation and recombination8.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 field9.x-ray spectra 9.1 inner shell processes 9.2 the solar corona 9.3 the structure of highly ionised atoms 9.4 isotope effects10.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 populations11.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 emissions12.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 spectra13.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 statessolutions to model problemsfurther reading and bibliographyindex