Accurate abundance analysis of late-type stars: advances in atomic physics

被引:87
作者
Barklem, Paul S. [1 ]
机构
[1] Uppsala Univ, Dept Phys & Astron, Theoret Astrophys, Box 516, S-75120 Uppsala, Sweden
基金
瑞典研究理事会;
关键词
Abundances; Chemical composition; Stellar atmospheres; Atomic processes and interactions; Atomic and molecular data; SODIUM-D-LINES; ELECTRON-IMPACT EXCITATION; PHOTOIONIZATION CROSS-SECTIONS; SPHERICALLY SYMMETRIC STATES; CLOSE-COUPLING CALCULATIONS; SOLAR FOURIER-TRANSFORM; HIGHLY-EXCITED LEVELS; SPECTRAL-LINES; NEUTRAL HYDROGEN; COLLISIONAL DEPOLARIZATION;
D O I
10.1007/s00159-016-0095-9
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
The measurement of stellar properties such as chemical compositions, masses and ages, through stellar spectra, is a fundamental problem in astrophysics. Progress in the understanding, calculation and measurement of atomic properties and processes relevant to the high-accuracy analysis of F-, G-, and K-type stellar spectra is reviewed, with particular emphasis on abundance analysis. This includes fundamental atomic data such as energy levels, wavelengths, and transition probabilities, as well as processes of photoionisation, collisional broadening and inelastic collisions. A recurring theme throughout the review is the interplay between theoretical atomic physics, laboratory measurements, and astrophysical modelling, all of which contribute to our understanding of atoms and atomic processes, as well as to modelling stellar spectra.
引用
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页数:54
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