天体辐射不透明度的实验室研究

天体辐射不透明是天体物理中一个非常重要的基本物理量，其理论计算结果的验证以往只能借助天文观测，激光技术的重大突破，使得天体物理学家可以在实验室里模拟天体等离子体中的辐射输运过程，这为更加深入地了解辐射不透明度提供了极好的实验手段。     

物质辐射不透明度对恒星结构与演化的影响及其计算

简要介绍了恒星结构与演化的理论模型，回顾了物质辐射不透明度计算的发展过程，详细讨论了物质辐射不透明度对恒星物理理论方面许多重要问题的影响以及发展现状。并介绍了利用改进的平均原子模型来进行恒星物质辐射不透明度的计算结果。     

Density Dependence of the Detailed Spectral Line Effects on the Opacity of Astrophysical Abundant Elements： oxygen

A full relativistic detailed-level-accounting approach has been developed independently to deal with the detailed spectral line effects on the opacity of the third most abundant element in stars: oxygen. The atomic energy levels and the oscillator strengths of the radiative transitions between the energy levels are obtained by carrying out the full relativistic one-configuration Dirac-Fock calculations. The photoionization cross sections are obtained via an average atom scheme with a consideration for the splitting of the ionization threshold due to the ionization stages and the term-couplings. As an example, the spectra resolved opacities and the mean opacities of oxygen are calculated to show the importance of the detailed spectral line profiles with the density of the matter.     

物质辐射不透明度对恒星结构与演化的影响及其计算

简要介绍了恒星结构与演化的理论模型,回顾了物质辐射不透明度计算的发展过程,详细讨论了物质辐射不透明度对恒星物理理论方面许多重要问题的影响以及发展现状.并介绍了利用改进的平均原子模型来进行恒星物质辐射不透明度的计算结果.     

Opacity of Hot and Dense Stellar Material： Flexible for Changes in Composition and Abundance

Opacity of stellar materials with the composition and relative abundance specified according to sun has been calculated by using an average-atom scheme, which is designed to treat electronic structures of atoms and ions in a mixture. Different relative abundances of the metallic elements are considered. Oomparisons between the present results and those of OPAL are made for the opacity to show that the difference is less than 10% for mostcases and less than 30% for the largest point with the density of 1.0g/cm^3 and temperatures from 50 to 6000eV. In view of the simplicity of the present approach, it is quite flexible to apply the method to different models of the stellar materials with changes in composition as well as in relative abundance.