We obtained photometric observations of the nova-like cataclysmic variable RW Tri and gathered all available AAVSO and other data from the literature. We determined the system parameters and found their uncertainties using the code developed by us to model the light curves of binary systems. New time-resolved optical spectroscopic observations of RW Tri were also obtained to study the properties of emission features produced by the system. The usual interpretation of the single-peaked emission lines in nova-like systems is related to the bi-conical wind from the accretion disc's inner part. However, we found that the Halpha emission profile is comprised of two components with different widths. We argue that the narrow component originates from the irradiated surface of the secondary, while the broader component's source is an extended, low-velocity region in the outskirts of the accretion disc, located opposite to the collision point of the accretion stream and the disc. It appears to be a common feature for long-period nova-like systems -- a point we discuss.

中文翻译：

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类新星激变变量 RW Tri 中的吸积流结构

我们获得了类新星灾难性变量 RW Tri 的光度观测，并从文献中收集了所有可用的 AAVSO 和其他数据。我们使用我们开发的代码来确定系统参数并发现它们的不确定性，以模拟二元系统的光变曲线。还获得了 RW Tri 的新时间分辨光谱观测，以研究该系统产生的发射特征的特性。类新星系统中单峰发射线的通常解释与来自吸积盘内部的双锥形风有关。然而，我们发现 Halpha 发射剖面由两个不同宽度的分量组成。我们认为狭窄的成分源自次级的受辐射表面，而较宽的成分的来源是扩展的，吸积盘外围的低速区域，位于吸积流与吸积盘碰撞点的对面。这似乎是长周期类新星系统的一个共同特征——我们将讨论这一点。