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arXiv 2403.07985astro-ph.SR
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白矮星双星路径巡天——X. 已知紫外超量双星的Gaia轨道

The white dwarf binary pathways survey -- X. Gaia orbits for known UV excess binaries

J. A. Garbutt, S. G. Parsons, O. Toloza, B. T. Gänsicke, M. S. Hernandez, D. Koester, F. Lagos, R. Raddi, A. Rebassa-Mansergas, J. J. Ren, M. R. Schreiber, M. Zorotovic

备注：
17 pages, 10 figures, Accepted for publication in MNRAS
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AI总结：

本研究结合Gaia第三次数据发布数据与紫外超量星表，通过光谱能量分布拟合得到206个含白矮星的双星样本的轨道及质量信息，验证了部分系统的白矮星质量吻合度，并揭示了这类双星的轨道周期范围与演化路径的多样性。

摘要：

拥有F、G或K型伴星的白矮星是银河系中大量奇异系统的最后共同前身星，尽管目前已识别出数千个此类系统，但迄今为止很少有系统在轨道周期和子星质量方面得到完整表征。Gaia第三次数据发布（Gaia data release 3）已对数十万个系统进行了观测，因此我们可以结合该数据与我们此前的紫外超量星表，开展光谱能量分布拟合，从而得到一个包含206个可能含有白矮星的双星样本，样本附带轨道周期信息，其中天体测量系统可直接测量子星质量，光谱系统则可得到子星质量下限。在这206个样本中，有4个此前已通过哈勃空间望远镜（Hubble Space Telescope）进行了紫外光谱观测，证实了白矮星的存在，且我们发现这些系统中白矮星的动力学质量与光谱质量高度吻合。我们发现白矮星加F、G或K型星的双星系统轨道周期范围很广，从不足1天到数百天不等。根据质量-周期关系，我们的样本中有大量系统可能是经历过稳定质量转移后的系统，而另一些系统则难以通过稳定质量转移或标准的公共包层演化来解释。

英文摘要：

White dwarfs with a F, G or K type companion represent the last common ancestor for a plethora of exotic systems throughout the galaxy, though to this point very few of them have been fully characterised in terms of orbital period and component masses, despite the fact several thousand have been identified. Gaia data release 3 has examined many hundreds of thousands of systems, and as such we can use this, in conjunction with our previous UV excess catalogues, to perform spectral energy distribution fitting in order to obtain a sample of 206 binaries likely to contain a white dwarf, complete with orbital periods, and either a direct measurement of the component masses for astrometric systems, or a lower limit on the component masses for spectroscopic systems. Of this sample of 206, four have previously been observed with Hubble Space Telescope spectroscopically in the ultraviolet, which has confirmed the presence of a white dwarf, and we find excellent agreement between the dynamical and spectroscopic masses of the white dwarfs in these systems. We find that white dwarf plus F, G or K binaries can have a wide range of orbital periods, from less than a day to many hundreds of days. A large number of our systems are likely post-stable mass transfer systems based on their mass/period relationships, while others are difficult to explain either via stable mass transfer or standard common envelope evolution.

机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。

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