论文标题
天王星与冷冻内部的热演化
Thermal Evolution of Uranus with a Frozen Interior
论文作者
论文摘要
天王星的固有光度比海王星小10倍，这是一个观察到的，标准的巨型行星进化模型（假定可忽略的粘度）无法捕获。在这里，我们表明，天王星内部的一半以上很可能处于固态，并且通过在内部深处存放积聚热量来解释天王星的衰弱，该模型解释了该高粘度区域。冷冻的内部还解释了其卫星轨道演变所需的天王星的质量因素。
The intrinsic luminosity of Uranus is a factor of 10 less than that of Neptune, an observation that standard giant planetary evolution models, which assume negligible viscosity, fail to capture. Here we show that more than half of the interior of Uranus is likely to be in a solid state, and that thermal evolution models that account for this high viscosity region satisfy the observed faintness of Uranus by storing accretional heat deep in the interior. A frozen interior also explains the quality factor of Uranus required by the evolution of the orbits of its satellites.
