论文标题
二进制行星的频率
Frequency of Planets in Binaries
论文作者
论文摘要
二进制行星的频率是在极性行星研究领域的重要问题，因为它与我们银河系的全球行星人群的估计以及我们对行星形成和进化的理解相关。由于此类目标带来的技术挑战，通常将多颗恒星排除在系系外行星搜索之外，尤其是使用径向速度技术进行的恒星搜索。结果，尽管最近做出了努力，但我们对多个恒星系统中行星频率的了解仍然不完整。另一方面，在汇编目标样品时缺乏有关二进制的知识，这意味着我们对单星周围的行星频率的估计可能会因未知二进制的存在而受到污染，尤其是如果这些物体在行星出现方面具有不同的行为。在先前的工作中，我们调查了Fisher和Valenti（2005）定义的均匀可检测性样品中包含的对象的二进制，表明其目标超过20％的目标实际上不是单星。在这里，我们提出了此普查的更新，这主要是由于第二个Gaia数据发布而成为现在可用的信息。新的二进制样本包括总共313个系统，其中通过这项工作添加了114个系统。我们还能够显着改善原始列表中大多数对的质量和轨道参数的估计值，尤其是在紧密分离的列表中。还确定了一些与白矮同伴的新系统。新分析的结果与我们以前的工作的发现非常吻合，这证实了二进制和单星之间的总行星频率缺乏差异，但表明对非常紧密的对的行星频率下降。}
The frequency of planets in binaries is an important issue in the field of extrasolar planet studies because of its relevance in the estimation of the global planet population of our galaxy and the clues it can give to our understanding of planet formation and evolution. Multiple stars have often been excluded from exoplanet searches, especially those performed using the radial velocity technique, due to the technical challenges posed by such targets. As a consequence and despite recent efforts, our knowledge of the frequency of planets in multiple stellar systems is still rather incomplete. On the other hand, the lack of knowledge about the binarity at the time of the compilation of the target samples means that our estimate of the planet frequency around single stars could be tainted by the presence of unknown binaries, especially if these objects have a different behavior in terms of planet occurrence. In a previous work we investigated the binarity of the objects included in the Uniform Detectability sample defined by Fisher and Valenti (2005), showing how more than 20% of their targets were, in fact, not single stars. Here, we present an update of this census, made possible mainly by the information now available thanks to the second Gaia Data Release. The new binary sample includes a total of 313 systems, of which 114 were added through this work. We were also able to significantly improve the estimates of masses and orbital parameters for most of the pairs in the original list, especially those at close separations. A few new systems with white dwarf companions were also identified. The results of the new analysis are in good agreement with the findings of our previous work, confirming the lack of difference in the overall planet frequency between binaries and single stars but suggesting a decrease in the planet frequency for very close pairs.}
