An atlas of line profile studies for SU UMa type cataclysmic variables
An atlas of line profile studies for SU UMa type cataclysmic variables
复制标题
SU UMa型灾变变量线剖面研究图集
DOI：
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发表时间：
2003
期刊：
影响因子：
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通讯作者：
R. Hanuschik
中科院分区：
文献类型：
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作者：
C. Tappert;R. Mennickent;J. Arenas;K. Matsumoto;R. Hanuschik
我们目前的H线剖面分析的七个SU UMa型矮新星AK Cnc，WX Cet，AQ Eri，VW Hyi，RZ狮子座，TU男人，和HS Vir。所有数据集都以相同的方式处理，对每个系统应用一系列技术。这个序列的基本组成部分是诊断图，以确定轨道相位的零点，多普勒层析成像，以可视化的发射分布。此外，我们引入了一种新的定性方法来评估多普勒拟合，通过比较重建的线轮廓与原始频谱的V=R图的形式。我们提出的分析结果的紧凑形式的图集，允许直接比较的排放分布在我们的目标。尽管大多数数据集并不是为了进行谱线分析而采集的，但我们获得了显着的结果，并能够表明这些系统中额外排放的类型。原则上，我们的物体应该具有非常相似的物理性质，也就是说，它们在轨道周期、质量比和质量转移率方面只覆盖很小的范围。然而，我们发现了大量的各种各样的现象，无论是相对于个别系统，也在同一对象的个别数据集。这包括来自次级星星和亮点的“典型”额外发射成分，也包括来自吸积盘前端的发射。
We present H line-profile analyses for the seven SU UMa type dwarf novae AK Cnc, WX Cet, AQ Eri, VW Hyi, RZ Leo, TU Men, and HS Vir. All data sets are treated in the same manner, applying a sequence of techniques for each system. The basic ingredients of this sequence are the diagnostic diagram to determine the zero point of the orbital phase, and Doppler tomography to visualise the emission distribution. We furthermore introduce a new qualitative way of to evaluate the Doppler fit, by comparing the line profile of the reconstructed with the original spectrum in the form of the V=R plot. We present the results of the analysis in the compact form of an atlas, allowing a direct comparison of the emission distribution in our targets. Although most of the data sets were not taken with the intention of a line-profile analysis, we obtain significant results and are able to indicate the type of the additional emission in these systems. Our objects should have in principle very similar physical properties, i.e. they cover only a small range in orbital periods, mass ratios, and mass-transfer rates. Nevertheless, we find a large variety of phenomena both with respect to the individual systems and also within individual data sets of the same object. This includes "canonical" additional emission components from the secondary star and the bright spot, but also emission from the leading side of the accretion disc.