Formation of P Cygni line profiles in relativistically expanding atmospheres
Formation of P Cygni line profiles in relativistically expanding atmospheres
复制标题
相对论膨胀大气中天鹅座 P 线剖面的形成
DOI：
10.1086/169203
复制
发表时间：
1990
期刊：
影响因子：
--
通讯作者：
J. Surdej
中科院分区：
文献类型：
--
作者：
D. Hutsemékers;J. Surdej
为了精确解释宽吸收线类星体和超新星光谱中观测到的天鹅座P线轮廓，我们采用Surdej（1979）的概率方法将Sobolev（1958）的形式推广到狭义相对论的情形。导出了源函数和谱线轮廓的表达式，结果表明，相对论性天鹅座P线轮廓与经典理论框架下的计算结果有很大的不同。因此，随着终端风速值的增加，红色发射翼肯定会变得比蓝色的更窄，而线中心发射会增加。根据多普勒效应的相对论表达式，这不再是对称的。参考文献29篇。
The probabilistic approach of Surdej (1979) is followed to generalize the Sobolev (1958) formalism to the case of special relativity, in order to interpret accurately the P Cygni line profiles observed in the spectrum of broad absorption-line quasars and supernovae. The expressions of the source function and of the line profile are derived, and it is shown that the relativistic P Cygni line profiles are significantly different from those computed in the framework of the classical theory. Thus, for increasing values of the terminal wind velocity, the red emission wing becomes definitely narrower than the blue one, while the line center emission increases. This is no longer symmetrical in accordance with the relativistic expression of the Doppler effect. 29 refs.