火卫一和火卫二中翻滚的激发
Excitation of Tumbling in Phobos and Deimos
摘要：
质量弹簧模型模拟被用来调查过去的粘弹性火卫一和火卫二自旋状态。从一个最初的潮汐锁定状态，我们发现交叉的自旋轨道共振与火星或平均运动共振与对方不激发火卫一或火卫二翻滚。然而，一旦翻滚，我们的模拟表明，这些卫星可以保持很长一段时间，在此期间，它们的轨道偏心率可以大大降低。我们归因于一个初始翻滚的粘弹性体的模拟下降到自旋同步状态在非常低的偏心率的翻滚混沌区体积偏心率的不敏感性的趋势。在翻滚体进入自旋同步共振之后，它可以表现出长寿命的非主轴旋转，并且这也可以延长具有增强的潮汐产生的能量耗散的时间段。火卫一和火卫二的低轨道偏心率可能部分是由于几乎灾难性的撞击而产生的自旋激发，而不是轨道共振激发后的潮汐演化。
英文摘要：
Mass-spring model simulations are used to investigate past spin states of a viscoelastic Phobos and Deimos. From an initially tidally locked state, we find crossing of a spin-orbit resonance with Mars or a mean motion resonance with each other does not excite tumbling in Phobos or Deimos. However, once tumbling our simulations show that these moons can remain so for an extended period and during this time their orbital eccentricity can be substantially reduced. We attribute the tendency for simulations of an initially tumbling viscoelastic body to drop into spin-synchronous state at very low eccentricity to the insensitivity of the tumbling chaotic zone volume to eccentricity. After a tumbling body enters the spin synchronous resonance, it can exhibit long lived non-principal axis rotation and this too can prolong the period of time with enhanced tidally generated energy dissipation. The low orbital eccentricities of Phobos and Deimos could in part be due to spin excitation by nearly catastrophic impacts rather than tidal evolution following orbital resonance excitation.
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