We have conducted a spectroscopic analysis of the far ultraviolet archival spectra of four symbiotic variables, EG And, AE Ara, CQ Dra and RW Hya. RW Hya and EG And have never had a recorded outburst while CQ Dra and AE Ara have outburst histories. We analyze these systems while they are in quiescence in order to help reveal the physical properties of their hot components via comparisons of the observations with optically thick accretion disk models and NLTE model white dwarf photospheres. We have extended the wavelength coverage down to the Lyman Limit with FUSE spectra. We find that the hot component in RW Hya is a low mass white dwarf with a surface temperature of 160,000K. We re-examine whether or not the symbiotic system CQ Dra is a triple system with a red giant transferring matter to a hot component made up of a cataclysmic variable in which the white dwarf has a surface temperature as low as ∼20,000K. The very small size of the hot component contributing to the shortest wavelengths of the FUSE spectrum of CQ Dra agrees with an optically thick and geometrically thin (∼4% of the WD surface) hot (∼ 120, 000K) boundary layer. Our analysis of EG And reveals that its hot component is a hot, bare, low mass white dwarf with a surface temperature of 80-95,000K, with a surface gravity log(g) = 7.5. For AE Ara, we also find that a low gravity (log(g) ∼ 6) hot (T ∼ 130, 000K) WD accounts for the hot component.

中文翻译：

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FUSE 共生变量中吸积热成分的光谱学

我们对四个共生变量 EG And、AE Ara、CQ Dra 和 RW Hya 的远紫外档案光谱进行了光谱分析。RW Hya 和 EG 从未记录过爆发，而 CQ Dra 和 AE Ara 有爆发历史。我们在这些系统处于静止状态时对其进行分析，以便通过将观测结果与光学厚吸积盘模型和 NLTE 模型白矮星光球层进行比较，帮助揭示其热组件的物理特性。我们使用 FUSE 光谱将波长覆盖范围扩展到莱曼极限。我们发现 RW Hya 中的热成分是一颗表面温度为 160,000K 的低质量白矮星。我们重新检查了共生系统 CQ Dra 是否是一个三重系统，红巨星将物质转移到一个热成分中，该热成分由一个激变变量组成，其中白矮星的表面温度低至 20,000K。有助于 CQ Dra 的 FUSE 光谱的最短波长的热成分的非常小尺寸与光学厚且几何薄（WD 表面的 4%）热（〜 120, 000K）边界层一致。我们对 EG 的分析表明，它的热成分是一颗热的、裸露的、低质量的白矮星，表面温度为 80-95,000K，表面重力 log(g) = 7.5。对于 AE Ara，我们还发现低重力 (log(g) ∼ 6) 热 (T ∼ 130, 000K) WD 占热分量。有助于 CQ Dra 的 FUSE 光谱的最短波长的热成分的非常小尺寸与光学厚且几何薄（WD 表面的 4%）热（〜 120, 000K）边界层一致。我们对 EG 的分析表明，它的热成分是一颗热的、裸露的、低质量的白矮星，表面温度为 80-95,000K，表面重力 log(g) = 7.5。对于 AE Ara，我们还发现低重力 (log(g) ∼ 6) 热 (T ∼ 130, 000K) WD 占热分量。有助于 CQ Dra 的 FUSE 光谱的最短波长的热成分的非常小尺寸与光学厚且几何薄（WD 表面的 4%）热（〜 120, 000K）边界层一致。我们对 EG 的分析表明，它的热成分是一颗热的、裸露的、低质量的白矮星，表面温度为 80-95,000K，表面重力 log(g) = 7.5。对于 AE Ara，我们还发现低重力 (log(g) ∼ 6) 热 (T ∼ 130, 000K) WD 占热分量。