标题： 邻近太阳系的恒星中具有行星的多重性 显示英文标题

标题： Multiplicity of stars with planets in the solar neighbourhood

摘要： - 目的：我们旨在量化恒星多重性对系外行星的存在和特性的影响力。 - 方法：我们使用Gaia DR3的最新天体测量数据以及先进的统计方法，研究了所有距离小于100 pc的系外行星宿主恒星。我们通过华盛顿双星目录和文献中的数据补充了对共同自行和视差伴星的搜索。在排除了一些基于径向速度数据、聚类和开放星协成员或具有解析的超冷伴星的系统后，我们保留了212个多重恒星系统中的215个系外行星宿主恒星。 - 结果：我们在15个已知系外行星宿主恒星的系统中发现了17个新的伴星，为236对恒星测定了精确的角距离和投影物理距离以及位置角，整理了多重系统中276颗行星的关键参数，并建立了一个包含687个具有系外行星的单恒星的比较样本。通过所有这些数据，我们对多重恒星系统中的行星进行了一系列假设的统计分析。尽管它们仅在2{\sigma }水平上具有统计显著性，但我们的分析指出了几个有趣的结果，包括在多重与单恒星系统中行星平均数量的比较以及高质星球在多重系统中倾向于位于更靠近轨道上的趋势。我们确认多重系统中的行星轨道偏心率大于单恒星系统中的行星。特别是，我们发现行星在恒星间投影物理距离与恒星-行星半长轴比值较小的情况下，表现出高轨道偏心率的趋势（> 4{\sigma }）。 显示英文摘要

摘要： - Aims: We intended to quantify the impact of stellar multiplicity on the presence and properties of exoplanets. - Methods: We investigated all exoplanet host stars at less than 100 pc using the latest astrometric data from Gaia DR3 and advanced statistical methodologies. We complemented our search for common proper motion and parallax companions with data from the Washington Double Star catalogue and the literature. After excluding a number of systems based on radial velocity data, and membership in clusters and open associations, or with resolved ultracool companions, we kept 215 exoplanet host stars in 212 multiple-star systems. - Results: We found 17 new companions in the systems of 15 known exoplanet host stars, measured precise angular and projected physical separations and position angles for 236 pairs of stars, compiled key parameters for 276 planets in multiple systems, and established a comparison sample comprising 687 single stars with exoplanets. With all of this, we statistically analysed a series of hypothesis regarding planets in multiple stellar systems. Although they are only statistically significant at a 2{\sigma} level, our analysis pointed to several interesting results on the comparison in the mean number of planets in multiple versus single stellar systems and the tendency of high mass planets to be located in closer orbits in multiple systems. We confirm that planets in multiple systems tend to have orbits with larger eccentricities than those in single systems. In particular, we found a significant (> 4{\sigma}) preference for planets to exhibit high orbital eccentricities at small ratios between star-star projected physical separations and star-planet semi-major axes.