Long term dynamical evolution and classification of classical TNOs

Long term dynamical evolution and classification of classical TNOs
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经典 TNO 的长期动态演化和分类

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发表时间：
2006
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通讯作者：
T. Mukai
T. Mukai
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作者：
P. S. Lykawka;T. Mukai

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经典跨海王星天体(TNO)被认为代表了跨海王星带(TNB)中最具活力的原始种群，为太阳系的形成提供了前所未有的线索。利用大量的模拟研究了经典TNOS的长期动态演化。我们在大范围的初始条件下跟踪了17000多个粒子的演化，并考虑了四颗巨行星对4个Gyr的扰动。经典区域中物体的演化既取决于它们的倾角，也取决于它们的半长轴，内部区域(a&lt；45AU)和外部区域(a&gt；45AU)的演化是不同的。原因是与天王星和海王星(天王星和海王星40-42)和5：3(a∼)重叠的世俗共振的影响 ∼42.3(AU)，7：4(A∼ ∼43.7(AU)，9：5(A∼ ∼44.5(AU)和11：6(A∼ ∼45.0(AU)平均运动共振强烈雕刻内部区域，而在外部区域仅有2：1平均运动共振(a∼ ∼47.7(AU)造成了重要的扰动。特别是，我们发现：(A)长期共振导致内部区域的低I体(I&lt；10°)的实质性侵蚀，除了那些在平均运动共振中幸存了数十亿年的物体；(B)位于45°AU40°AU和I&gT；5°的最佳稳定区，没有主要扰动；(C)经典区域的边界定义得更好：42-47.5 AU(Q&gT；38 AU)对于冷经典TNos和40-47.5 AU(Q&GT；(D)在40-42AU区域看到的高倾斜度的TNO反映了它们的初始条件。因此，它们应该被归类为热门的经典跨国公司。最后，我们报告了我们的结果与观测结果的很好的匹配，表明前者可以为经典区域的轨道结构提供解释和预测。
AbstractClassical trans-Neptunian objects (TNOs) are believed to represent the most dynamically pristine population in the trans-Neptunian belt (TNB) offering unprecedented clues about the formation of our Solar System. The long term dynamical evolution of classical TNOs was investigated using extensive simulations. We followed the evolution of more than 17000 particles with a wide range of initial conditions taking into account the perturbations from the four giant planets for 4 Gyr. The evolution of objects in the classical region is dependent on both their inclination and semimajor axes, with the inner (a<45 AU) and outer regions (a>45 AU) evolving differently. The reason is the influence of overlapping secular resonances with Uranus and Neptune (40–42 AU) and the 5:3 (a∼ ∼42.3 AU), 7:4 (a∼ ∼43.7 AU), 9:5 (a∼ ∼44.5 AU) and 11:6 (a∼ ∼ 45.0 AU) mean motion resonances strongly sculpting the inner region, while in the outer region only the 2:1 mean motion resonance (a∼ ∼47.7 AU) causes important perturbations. In particular, we found: (a) A substantial erosion of low-i bodies (i<10°) in the inner region caused by the secular resonances, except those objects that remained protected inside mean motion resonances which survived for billion of years; (b) An optimal stable region located at 45 AU40 AU and i>5° free of major perturbations; (c) Better defined boundaries for the classical region: 42–47.5 AU (q>38 AU) for cold classical TNOs and 40–47.5 AU (q>35 AU) for hot ones, with i=4.5° as the best threshold to distinguish between both populations; (d) The high inclination TNOs seen in the 40–42 AU region reflect their initial conditions. Therefore they should be classified as hot classical TNOs. Lastly, we report a good match between our results and observations, indicating that the former can provide explanations and predictions for the orbital structure in the classical region.