共生星双星的星风物质损失率的测定

Determination of Mass Loss Rates of Symboitic Binaries

共生星双星是一颗有强大星风物质损失的红巨星与一颗早型热星组成的特殊双星系统。由于早型热星在充满红巨星的星风物质的空间中环绕运行，可以产生Ｐ—Ｃｙｇｎｉ型谱线，通过对Ｐ—Ｃｙｇｎｉ型谱线的理论分析可以精确测定共生星双星的星风物质损失率。文章介绍了国际上比较有代表意义的一些共生星双星的工作，其中的方法几乎都是近十年中发展起来的。同时，文章还介绍了作者的一些工作。在谱线形成计算中考虑了较多的因素，如氢—氦混合气体的多能级跃迁问题、轨道运动引起的密度非径向分布问题等，并在轨道形状方面做了一些简化。反映了共生星双星谱线形成关键的周期性相位变化的特征，取得了比较满意的结果，对这个方法存在的问题和改进方向进行了一些简要讨论，此外，还介绍了作者在线性化分离法求解Ｎｏｎ－ＬＴＥ大气模型中所做的工作。

The symbiotic binary is a special system, consisting of a hot early type star and a cool late type supergiant with strong stellar wind, which forms an expanding envelope. In the expanding envelope, the orbital motion of the hot star produces P-Cygni type lines which have periodic variation profiles. The mass loss rate from the stellar wind of the supergiant can be determined by analysis of these lines. In this paper, we discuss the use of the theory of moving atthospheres to determine the mass loss rate by caculating the line formations of symbiotic binaries. We develope a method to calculate the multiple transitions in the hydrogen and helium mixture gases and treat the distribution of the density as non-radial distribution resulting from the orbital motions. The results show the key characteristics of periodic variations of the line profile of symbiotic binaries. In iddition, we have made an improvement of the linearization -separation technique, a method used in the carculation of the Non-LTE atmosphere models.