近共振系外行星系统中低水平动力学激发的证据
Evidence for Low-Level Dynamical Excitation in Near-Resonant Exoplanet Systems
AI总结：
本研究通过对近共振热木星TOI-2202 b的Rossiter-McLaughlin测量，结合现有近共振系统自旋-轨道数据，首次开展种群层面分析，证实这类系统符合静态形成路径，存在低水平动力学激发空间。
摘要：
近共振行星系统的几何结构为探究系外行星系统的初始条件提供了一个相对原始的窗口。由于近共振系统可能经历的动力学扰动极少，这类系统的自旋-轨道取向能够揭示静态行星形成的典型结果，以及原始恒星倾角分布。然而，目前用于约束近共振系统自旋-轨道取向的测量数据还很少。我们利用6.5米麦哲伦·克莱望远镜上的卡内基行星搜寻光谱仪（PFS），对近共振热木星TOI-2202 b进行了Rossiter-McLaughlin测量。这是长周期系外行星系统恒星倾角（SOLES）巡天的第八项成果。我们推导出天空投影二维自旋-轨道角$λ=26^{+12}_{-15}$$^{\text{o}}$，三维自旋-轨道角$ψ=31^{+13}_{-11}$$^{\text{o}}$，发现TOI-2202 b——迄今为止具有三维自旋-轨道约束的质量最大的近共振系外行星——很可能与宿主恒星的赤道并非完全对齐。结合近共振系统自旋-轨道测量的全部统计数据，我们证明当前周期比$P_2/P_1\boldsymbol{\text{lesssim}}4$的近共振系统集合总体上符合静态形成路径，同时存在低水平（$\boldsymbol{\text{lesssim}}20^{\text{o}}$）原行星盘错位或盘消散后自旋-轨道激发的空间。我们的研究结果首次对近共振行星系统的自旋-轨道几何结构开展了种群层面的分析。
英文摘要：
The geometries of near-resonant planetary systems offer a relatively pristine window into the initial conditions of exoplanet systems. Given that near-resonant systems have likely experienced minimal dynamical disruptions, the spin-orbit orientations of these systems inform the typical outcomes of quiescent planet formation, as well as the primordial stellar obliquity distribution. However, few measurements have been made to constrain the spin-orbit orientations of near-resonant systems. We present a Rossiter-McLaughlin measurement of the near-resonant warm Jupiter TOI-2202 b, obtained using the Carnegie Planet Finder Spectrograph (PFS) on the 6.5m Magellan Clay Telescope. This is the eighth result from the Stellar Obliquities in Long-period Exoplanet Systems (SOLES) survey. We derive a sky-projected 2D spin-orbit angle $λ=26^{+12}_{-15}$ $^{\circ}$ and a 3D spin-orbit angle $ψ=31^{+13}_{-11}$ $^{\circ}$, finding that TOI-2202 b - the most massive near-resonant exoplanet with a 3D spin-orbit constraint to date - likely deviates from exact alignment with the host star's equator. Incorporating the full census of spin-orbit measurements for near-resonant systems, we demonstrate that the current set of near-resonant systems with period ratios $P_2/P_1\lesssim4$ is generally consistent with a quiescent formation pathway, with some room for low-level ($\lesssim20^{\circ}$) protoplanetary disk misalignments or post-disk-dispersal spin-orbit excitation. Our result constitutes the first population-wide analysis of spin-orbit geometries for near-resonant planetary systems.
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