Abstract

We present the results of model analysis of the optical spectra of SU UMa and WZ Sge-type dwarf novae TY Psc, FL Psc, and V455 And. Spectroscopic observations were carried out at the SAO RAS 6-m BTA telescope in 2013. The selection criterion for the systems under study is their existence in a quiescent state with an optically thin accretion disk and dominance of white dwarf radiation. The fulfillment of the criterion was verified by observing the H I Balmer series broad absorption lines simultaneously with two-peak H I, He I, and Fe II emissions. A technique for automated fitting of model spectra of white dwarfs and observed spectra of dwarf novae based on quantitative criteria for their matching is proposed and implemented. The atmospheric parameters (effective temperature \(T_{\textrm{eff}}\) and surface gravity \(\log g\)) of accretors in TY Psc, FL Psc, and V455 And were determined applying it and used further to obtain their masses and radii. Due to the technique proposed here we obtained the estimates of the fundamental parameters of the secondaries using the theoretical ‘‘mass–radius’’ relationships for brown and red main-sequence dwarfs. As a result, we demonstrate the possibility in principle of determining all the main parameters of the SU UMa and WZ Sge dwarf novae based on modeling and the analysis of a small number of their spectra in the quiescent state.

中文翻译：

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SU UMa 和 WZ Sge 型矮新星静止状态的参数。I. FL Psc、TY Psc 和 V455 以及

摘要

我们展示了 SU UMa 和 WZ Sge 型矮新星 TY Psc、FL Psc 和 V455 And 的光谱模型分析结果。2013 年在 SAO RAS 6 米 BTA 望远镜上进行了光谱观测。研究系统的选择标准是它们处于静止状态，具有光学薄吸积盘和白矮星辐射的主导地位。通过观察同时具有双峰 HI、He I 和 Fe II 发射的 HI Balmer 系列宽吸收线，验证了标准的实现。提出并实施了一种基于定量标准自动拟合白矮星模型光谱和矮新星观测光谱的技术。大气参数（有效温度\(T_{\textrm{eff}}\)TY Psc、FL Psc 和 V455 中吸积体的表面重力\(\log g\) ) 并应用它确定并进一步用于获得它们的质量和半径。由于这里提出的技术，我们使用棕矮星和红矮星主序矮星的理论“质量-半径”关系获得了副星基本参数的估计值。因此，我们证明了基于建模和分析它们处于静止状态的少量光谱来确定 SU UMa 和 WZ Sge 矮新星所有主要参数的原则上的可能性。