切伦科夫线辐射的基本公式

THE BASIC FORMULAE OF CERENKOV LINE RADIATION

在８０ 年代初，尤峻汉和程富华从理论上证实，当相对论电子在稠密气体中运动时，切伦科夫效应将产生宽的、轮廓明显不对称的原子或分子发射线．此后这一新的谱线发射机制被一系列实验所确证．尤峻汉等人又进一步给出了有关切伦科夫辐射的系列解析公式，但其有关谱轮廓和红移的结论只适用于极稠密的气体．由于这一线辐射机制在天体物理中的潜在重要性，在他们工作的基础上，进一步简化、推广、改进了原有的公式体系。

Early in 1980, You and Cheng argued that, when relativistic electrons move through a dense gas, the Cerenkov effect will produce peculiar emission lines. They presented a series of formulae to describe this new line radiation. Then an elegant experimental confirmation has been performed by Xu et al. Owing to the potential importance of this radiation mechanism in astrophysics, the authors of this paper try to examine and improve the previous formula system in a form, which is more convenient for astrophysical applications. In particular, the extended formulae may be applied to other species of atoms and/or ions rather than hydrogen as in previous papers, and used in calculations for the nonuniform plane parallel slabs of the emissive gas.