发表机构
Southwest Research Institute; SETI Institute（西南研究所; SETI研究所）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本文通过N体模拟研究米兰达异常轨道倾角的成因，发现天卫四-天卫二5:3共振可激发其倾角，并计算潮汐加热，为天王星潮汐耗散提供新约束。
AI 中文摘要
天王星的五颗主要卫星记录了复杂的地质历史，其特征既包括构造再表面化，也包括严重的撞击坑化，将它们的演化与太阳系中的动力学过程联系起来。米兰达是天王星最小且距离最近的主要卫星，具有异常大的轨道倾角（$4.3^\circ$）以及以冕状构造和构造结构为主的显著表面地质。在本文中，我们探讨米兰达的轨道倾角和地质历史是否可以通过天王星卫星系统内部的过去轨道共振来解释。利用代码SIMPL进行直接N体积分，我们在假设天王星快速潮汐耗散并改变卫星内部响应的条件下，探索了五颗主要卫星的潮汐和动力学演化。我们的模拟证实，即使米兰达的平均运动不参与该共振，米兰达的轨道倾角也可以通过涉及天卫四（Ariel）和天卫二（Umbriel）的共振相互作用而被激发。天卫四-天卫二5:3平均运动共振似乎是能够将米兰达的轨道倾角驱动至其当前值的最近期主要动力学事件。我们计算了与这些共振遭遇相关的潮汐加热，并表明，对于强耗散的天王星（$Q_U\sim600$），该共振可能导致米兰达的热通量接近形成其冕状构造所需的热通量。这些结果可能为天王星的潮汐耗散提供新的约束。
英文摘要
The five major moons of Uranus record a complicated geological history characterized by both tectonic resurfacing and heavy impact cratering, connecting their evolution to dynamical processes in the Solar System. Miranda, the smallest and closest major moon to Uranus, has an unusually large orbital inclination ($4.3^\circ$) and an remarkable surface geology dominated by coronae and tectonic structures. In this paper we explore whether Miranda's inclination and geological history can be explained through past orbital resonances within the Uranian satellite system. Using direct $N$-body integrations with the code SIMPL, we explore the tidal and dynamical evolution of the five major moons while assuming a fast tidal dissipation of Uranus and varying the internal responses of the satellites. Our simulations confirm that Miranda's inclination can be excited through resonant interactions involving Ariel and Umbriel, even when Miranda mean motion is not involved in that resonance. The Ariel-Umbriel 5:3 mean-motion resonance appears to be the most recent major dynamical event capable of driving Miranda's inclination to its current value. We compute the tidal heating associated with these resonance encounters and show that, for a strongly dissipative Uranus ($Q_U\sim600$), the resonance could cause heat fluxes in Miranda approaching those required to form its coronae. These results could provide new constraints on Uranus's tidal dissipation.
