冥族小天体及其他共振柯伊伯带天体的受迫轨道平面
The forced orbital planes of the Plutinos and other resonant KBOs
浏览论文内容
中文总结 AI 辅助
该研究重新测量冥族小天体等共振柯伊伯带天体的平均轨道平面，发现双共振冥族小天体子群平均平面不同，其他四类共振群平均平面与局部拉普拉斯平面等无统计差异，为相关理论分析提供经验依据。
中文摘要 AI 辅助
对于非共振小行星的受迫平面，已有研究表明可通过线性拉普拉斯-拉格朗日长期摄动理论给出的局部拉普拉斯平面很好地估计，但目前尚无针对共振小行星受迫平面的现存理论。我们采用改进的方法，重新测量了观测到的冥族小天体（Plutinos，一类被锁定在海王星3:2平均运动共振中的柯伊伯带天体）的平均轨道平面。在J2000黄道分点参考系中，测得的平均平面倾角为1.9度，升交点经度为46.8度，平面位置的95%置信度为2度；该平面与局部拉普拉斯平面明显分离，但与太阳系不变平面无差异。我们还以高统计置信度表明，两个动力学子群（近日点幅角在+90度和-90度附近 librate 的双共振冥族小天体）的平均平面彼此不同。此外，我们测量了柯伊伯带中其他四个观测到的共振群的平均平面：5:3、7:4、2:1和5:2。尽管这些群的样本量较大（范围为56-105），但它们的平均平面目前在统计上与其局部拉普拉斯平面、海王星平面和不变平面无差异。对于所有五个共振群，我们还报告了其倾角的最佳拟合冯·米塞斯（von Mises）函数。这些经验测量凸显了理论分析的必要性，以理解共振小行星群的空间动力学。此类分析有望助力利用这些天体揭示未建模的摄动和/或未发现的摄动天体。
英文摘要
The forced plane of non-resonant minor planets has been understood to be well-estimated by the local Laplace plane given by linear Laplace-Lagrange secular perturbation theory, but there is no extant theory for the forced plane of resonant minor planets. With improved methodology, we revisit our previous measurement of the mean orbital plane of the observed Plutinos, a group of Kuiper belt objects locked in Neptune's 3:2 mean motion resonance. In the J2000 ecliptic-equinox reference frame, the measured mean plane has an inclination of 1.9 degrees and an ascending node at 46.8 degrees longitude, with a 95% confidence of 2 degrees in the plane position; it is well separated from the local Laplace plane but is indistinguishable from the solar system's invariable plane. We also show that, at high statistical confidence, the two dynamical subgroups, the doubly resonant Plutinos whose arguments of perihelion librate about +90 and -90 degrees, have different mean planes from each other. Additionally, we measure the mean planes of four other observed resonant groups in the Kuiper belt: the 5:3, 7:4, 2:1, and 5:2. Although these groups have substantial sample sizes (in the range 56-105), their mean planes are presently not statistically distinguishable from their local Laplace plane, Neptune's plane, and the invariable plane. For all five resonant groups, we also report the best-fit von Mises function for their inclinations. These empirical measurements underscore the need for theoretical analysis to understand the spatial dynamics of resonant populations of minor planets. Such analysis could potentially enable their use for uncovering unmodeled perturbations and/or undiscovered perturbers.
