Miranda的轨道-热耦合演化
Coupled orbital-thermal evolution of Miranda
摘要：
米兰达有一个异常高的倾角（$I=4.338^\circ$），它的表面揭示了过去内生活动的迹象。对其轨道演化动力学方面的研究表明可能的共振过程，特别是与Umbriel的共振过程，可以解释米兰达目前的高倾角。引力相互作用引起的潮汐加热可导致偏心率上升，从而增加卫星内部的能量耗散，提高内部温度。我们在这里研究可能增加的轨道共振和由此产生的内生加热米兰达考虑到其温度依赖的流变性所造成的偏心率。耦合的轨道-热演化模型与不同的流变学模型和热参数开始从一个冷的热状态，与环境的辐射平衡运行。对于标称参数的演变方案研究，共振不足以提高既不偏心率，也不显着的内部温度。在与Umbriel的3：1共振期间，获得了约100的最低耗散函数$Q$和$e\approx0.02$的最终偏心率。
英文摘要：
Miranda has a unusually high inclination ($I=4.338^\circ$), and its surface reveals signs of past endogenic activity. Investigations of the dynamical aspects of its orbital evolution suggest probable resonant processes, in particular with Umbriel, as an explanation for the present high inclination of Miranda. The tidal heating induced by gravitational interactions can lead to the rise of eccentricities and, consequently, to the increased dissipation of energy inside the satellite and higher internal temperatures. We study here the possible increase in eccentricities caused by orbital resonances and the resulting endogenic heating on Miranda taking into account its temperature dependent rheology. The coupled orbital-thermal evolution model was run with different rheological models and the thermal parameters starting form a cold thermal state, in radiative equilibrium with the environment. For the nominal parameters of the evolution scenarios studied, the resonances were not sufficient to rise neither the eccentricities nor the internal temperatures significantly. Lowest dissipation function $Q$ of around 100 and final eccentricity of $e\approx0.02$ were obtained during the resonance 3:1 with Umbriel.
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