类新星激变变星RW Sextantis和1 RXS J064434 .5+334451中吸积流的结构
The structure of accretion flows in nova-like cataclysmic variables: RW Sextantis and 1RXS J064434.5+334451
摘要：
对类新星激变变星RW Sextantis进行了新的时间分辨阶梯光栅光谱观测，目的是研究该系统的发射特征。H_α发射谱线的轮廓可以清楚地分为两个（“窄”和“宽”）分量。在另一个类新星系统1 RXS ~J064434.5+33445中也观测到了类似的发射轮廓，我们也重新分析了它的光谱数据，重新确定了系统参数。“窄”低速分量的来源是次级恒星的被照射面。我们从H_α分布中解开并去除了“窄”分量，以研究发射宽分量的区域的起源和结构。我们发现，“宽”分量与白矮星或吸积盘中心的风无关，而是从吸积盘的外侧发出的。对类似系统的文献研究表明，这一特征在其他一些长周期类新星变星中也很常见。我们建议，源的“宽”的组成部分是一个扩展的，低速区域的吸积盘的相对侧的郊区，相对于吸积流和光盘的碰撞点。
英文摘要：
New time-resolved optical spectroscopic echelle observations of the nova-like cataclysmic variable RW Sextantis were obtained, with the aim to study the properties of emission features in the system. The profile of the H_alpha emission line can be clearly divided into two (`narrow' and `wide') components. Similar emission profiles are observed in another nova-like system, 1RXS~J064434.5+33445, for which we also reanalysed the spectral data and redetermined the system parameters. The source of the `narrow', low-velocity component is the irradiated face of the secondary star. We disentangled and removed the `narrow' component from the H_alpha profile to study the origin and structure of the region emitting the wide component. We found that the `wide' component is not related to the white dwarf or the wind from the central part of the accretion disc, but is emanated from the outer side of the disc. Inspection of literature on similar systems indicates that this feature is common for some other long-period nova-like variables. We propose that the source of the `wide' component is an extended, low-velocity region in the outskirts of the opposite side of the accretion disc, with respect to the collision point of the accretion stream and the disc.
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