标题： 关于热木星和恒星聚类：主星人口统计学的作用 显示英文标题

标题： On Hot Jupiters and Stellar Clustering: The Role of Host Star Demographics

摘要： 热木星（HJ）在恒星环境中的变化提供了关于这些极端行星主要形成渠道的线索。 最近的研究表明，HJ的宿主恒星更倾向于位于相空间密度高的区域，这可能反映了原始环境条件。 这些区域的动力学温度较低（|v| < 40 km/s），促使了另一种假设，即这种相关性反映了年龄偏差：高密度区域的行星系统总体上更年轻，因此不太可能发生潮汐内旋和破坏。 我们测试了相空间高密度区域中HJ的明显过剩是否源于内在宿主特性（质量、金属量、年龄）的差异，这些特性可能与相空间密度相关，或者是否存在额外的环境效应。 我们使用2MASS和Gaia DR3的测光数据、视差以及自洽的光谱和光谱测光观测值，得出了行星宿主恒星的质量、金属量和年龄的统一估计。 在2265个确认的系外行星宿主样本中，我们发现高密度区域的恒星周围HJ有显著的相对过剩。 然而，我们也发现高密度区域更倾向于容纳年轻的、质量更大的和金属量更高的恒星，与低密度区域相比。 在对这些差异进行校正后，无论是通过将相空间密度与年龄进行去趋势处理，还是通过在子样本中匹配宿主特性，我们都没有发现高密度和低密度区域之间HJ种群的显著差异。 我们的结果表明，之前报道的HJ出现率与相空间密度之间的相关性是由宿主恒星人口统计学上的潜在差异驱动的，而不是由内在的环境效应引起的。 显示英文摘要

摘要： The variation in hot Jupiter (HJ) occurrence across stellar environments holds clues as to the dominant formation channels of these extreme planets. Recent studies suggest HJ hosts preferentially reside in regions of high phase space density, possibly reflecting natal environmental conditions. These regions are kinematically cold (|v| < 40 km/s), prompting the alternative hypothesis that the correlation reflects an age bias: planetary systems in overdensities are systematically younger and therefore less likely to have undergone tidal inspiral and destruction. We test whether the apparent excess of HJs in phase space overdensities arises from differences in intrinsic host properties -- mass, metallicity, age -- which may correlate with phase space density or whether there is evidence for an additional environmental effect. We derive homogeneous estimates for the mass, metallicity, and age of planet-hosting stars using 2MASS and Gaia DR3 photometry, parallaxes, and self-consistent spectroscopic and spectrophotometric observables. In a sample of 2265 confirmed exoplanet hosts, we find a significant relative excess of HJs orbiting stars in overdense regions. However, we also find that overdensities preferentially host younger, more massive, and more metal-rich stars compared to underdensities. After correcting for these differences, either by detrending the phase space density against age or by matching host properties across subsamples, we find no significant differences in the HJ populations between over- and underdense regions. Our results suggest that the previously reported correlation between HJ occurrence and phase space density is driven by underlying differences in host star demographics rather than an intrinsic environmental effect.