arXiv 2411.008292024-11astro-ph.EP

共振柯伊伯带天体——冥族小天体的新型多弧段模型

A new multiple-arc model of the resonant Kuiper belt objects -- Plutinos

Yue Chen, Jian Li

备注：: arXiv admin note: substantial text overlap with arXiv:2305.18157
DOI：: 10.1093/mnras/stae2462

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AI总结：

本文提出一种针对海王星2:3共振冥族小天体的三弧段模型，以更精确地计算其对行星的引力摄动，并验证了该模型在不同共振振幅和偏心率下的适用性及可扩展性。

摘要：

在行星历表中纳入柯伊伯带天体（KBOs）的引力影响时，通常采用均匀环模型。本文针对海王星2:3平均运动共振（MMR）中的KBO族群（即冥族小天体，Plutinos），考虑其共振特性，提出了一种三弧段模型。每个“弧段”指均匀环的一部分，由适当数量的质点组成。随后，通过太阳-海王星距离的变化量（Δd_SN）数值测量冥族小天体的总摄动。我们进行了全面研究，分别考虑了与冥族小天体共振振幅（A）和偏心率（e）相关的各种方位角分布和径向分布。结果表明，在100年时间跨度内：（1）在最小偏心率e=0.05时，由冥族小天体引起的太阳-海王星距离变化Δd_SN随A减小而显著下降，与环模型得到的Δd_SN值偏差可达约100公里；（2）当e在0.1-0.2中等范围内增大时，弧段模型与环模型之间Δd_SN的差异变得越来越显著；（3）在最大偏心率e≳0.25时，无论A如何，Δd_SN可趋近于零，且弧段模型与环模型在Δd_SN上表现出显著差异，最大可达170公里。随后，通过将我们的三弧段模型与观测到的冥族小天体对海王星和土星位置引起的摄动进行比较，进一步验证了该模型的适用性。此外，为冥族小天体设计的多弧段模型概念可轻松扩展到其他由小天体密集填充的平均运动共振中。

英文摘要：

To incorporate the gravitational influence of Kuiper belt objects (KBOs) in planetary ephemerides, uniform-ring models are commonly employed. In this paper, for representing the KBO population residing in Neptune's 2:3 mean motion resonance (MMR), known as the Plutinos, we introduce a three-arc model by considering their resonant characteristics. Each `arc' refers to a segment of the uniform ring and comprises an appropriate number of point masses. Then the total perturbation of Plutinos is numerically measured by the change in the Sun-Neptune distance ($Δd_{SN}$). We conduct a comprehensive investigation to take into account various azimuthal and radial distributions associated with the resonant amplitudes ($A$) and eccentricities ($e$) of Plutinos, respectively. The results show that over a 100-year period: (1) at the smallest $e=0.05$, the Sun-Neptune distance change $Δd_{SN}$ caused by Plutinos decreases significantly as $A$ reduces. It can deviate from the value of $Δd_{SN}$ obtained in the ring model by approximately 100 km; (2) as $e$ increases in the medium range of 0.1-0.2, the difference in $Δd_{SN}$ between the arc and ring models becomes increasingly significant; (3) at the largest $e\gtrsim0.25$, $Δd_{SN}$ can approach zero regardless of $A$, and the arc and ring models exhibit a substantial difference in $Δd_{SN}$, reaching up to 170 km. Then the applicability of our three-arc model is further verified by comparing it to the perturbations induced by observed Plutinos on the positions of both Neptune and Saturn. Moreover, the concept of the multiple-arc model, designed for Plutinos, can be easily extended to other MMRs densely populated by small bodies.

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