海王星系的最后一次巨大撞击。对跨土星区域寡头质量的限制
Last giant impact on the Neptunian system. Constraints on oligarchic masses in the trans-Saturnian region
摘要：
目前，大型天体的随机撞击是通常被接受的能够解释冰巨星的巨大性的机制。我们试图在现代理论的框架内，将巨大的撞击作为海王星目前的不稳定性的原因。我们还使用目前的海王星不规则卫星（海卫一除外）的轨道特性设置在海王星形成结束时的巨大影响的情况下的限制。我们模拟角动量转移到原海王星和脉冲转移到其不规则的卫星之间的最后一次随机碰撞（GC）的原行星和寡头质量在海王星的形成结束。我们得到，一个大于4个地球质量的撞击物质量是不可能的，因为它不能再现行星的当前旋转属性，除非碰撞的碰撞参量非常小。另一方面，如果撞击物质量大于1.4地球质量，那么现在的海王星不规则卫星必须在随机撞击结束后形成或捕获。寡头质量的上限（海王星的质量为4个地球质量，海王星不规则卫星的质量为1.4个地球质量）与未知参数无关，如星子的质量和分布，天王星和海王星形成的位置，太阳星云初始表面质量密度和生长状态。如果发生了随机撞击，这些结果应该被理解为在冰行星形成结束时跨土星区域的寡头质量的上限约束，并可用于设定行星形成情景的约束。
英文摘要：
Stochastic impacts by large bodies are, at present, the usually accepted mechanisms able to account for the obliquity of the ice giants. We attempt to set constraints on giant impacts as the cause of Neptune's current obliquity in the framework of modern theories. We also use the present orbital properties of the Neptunian irregular satellites (with the exception of Triton) to set constraints on the scenario of giant impacts at the end of Neptune formation. We model the angular momentum transfer to proto-Neptune and the impulse transfer to its irregular satellites by the last stochastic collision (GC) between the protoplanet and an oligarchic mass at the end of Neptune's formation. We obtain that an impactor mass greather than 4 Earth masses is not possible since it cannot reproduce the present rotational properties of the planet, unless the impact parameter of the collision were very small. On the other hand, if the impactor mass was greather than 1.4 Earth masses, the present Neptunian irregular satellites had to be formed or captured after the end of stochastic impacts. The upper bounds on the oligarchic masses (4 Earth masses from the obliquity of Neptune and 1.4 earth masses from the Neptunian irregular satellites) are independent of unknown parameters, such as the mass and distribution of the planetesimals, the location at which Uranus and Neptune were formed, the Solar Nebula initial surface mass density, and the growth regime. If stochastic impacts had occurred, these results should be understood as upper constraints on the oligarchic masses in the trans-Saturnian region at the end of ice planet formation and may be used to set constraints on planetary formation scenarios.
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