The stream impact region in the disc of WZ Sge
The stream impact region in the disc of WZ Sge
复制标题
WZ Sge盘中的流冲击区域
DOI：
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发表时间：
1998
期刊：
影响因子：
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通讯作者：
R. Rutten
中科院分区：
文献类型：
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作者：
H. Spruit;R. Rutten
我们报告的观测新功能的光谱的激变变量WZ Sge。盘食被认为是Hα线上一个定义明确的结构。从相位0.25到0.5，在这条谱线上可以看到与发射S波形状相同的吸收特征，但红移了200 km s−1。两种可能的解释这个功能，这两个都意味着它起源于光盘边缘上的流的冲击点。此外，在光斑的速度图中发现了亚结构的证据。从连续谱热点下游延伸到约60°处的线发射激波后物质的发射，在多普勒图中以从热点延伸的尾部的形式出现。理论估计表明，这种尾翼是撞击后气流流体动力学的结果。对系统参数进行了新的确定。他们同意Gilliland等人的观点;特别是，这些数据支持一个高的原始质量。在内部区域，Hα表面亮度随离主星距离的变化比霍恩发现的其他激变变星在静止时的r−1.5变化要平缓。
We report the observation of new features in the spectrum of the cataclysmic variable WZ Sge. The disc eclipse is seen as a well-defined structure in the Hα line. From phases 0.25 to 0.5 an absorption feature of the same shape as the emission S wave is seen in this line, but redshifted by ∼ 200 km s−1. Two possible interpretations of this feature are given, both of which imply that it originates at the impact point of the stream on the disc edge. In addition, evidence is found for substructure in the velocity map of the spot. Emission from line-emitting post-shock material, extending to about 60° downstream from the continuum hotspot, is seen in the Doppler map in the form of a tail extending from the hotspot. A theoretical estimate shows that such a tail is to be expected as a consequence of the post-impact hydrodynamics of the stream. A new determination of the system parameters is made. They agree with those of Gilliland et al.; in particular, the data support a high primary mass. The variation of Hα surface brightness with distance from the primary is flatter, in the inner regions, than the r−1.5 dependence found by Horne for other cataclysmic variables in quiescence.