Resonance Structure of Kuiper Belt Objects and Their Dynomical Evolution

自1992年首次发现以来，已经发现了大约130个位于海王星轨道外的柯伊伯带天体。它们被认为是星子的残余物，它们的动力学行为可能对太阳系早期行星的形成提供一些信息。本文研究了平均运动共振、长期共振、次级共振和Kozai共振的动力学结构，并与主带小行星的动力学结构进行了比较。下面我们对本次调查的主要结果进行总结。1)对于平均运动共振，我们主要研究与海王星的（p: p+1）共振。除了1:2意味着运动共振,意味着运动共振的临界参数平均约180゚,另一方面关键参数在主小行星带0゚周围摆动,在我们所寻求的意思是运动共振区域的双共振Kozai共振,世俗的共振和年代 ... 更econdary共振与使用半解析方法,然后我们确认的存在双共振并研究其稳定性。2)在平均运动共振区附近分布了约35000个具有不同初始条件的天体，并对它们在外巨行星扰动下500万年的轨道进行了积分，研究了它们的稳定性。它们之间的稳定轨道行为与半解析方法的结果吻合得很好。从我们的数值模拟中，我们发现了半解析方法无法预测的混沌但有趣的轨道。它们中的一些从外部进入共振区，一些从共振区出来。这种过渡性变化的时间尺度相当长。这种现象主要是由天王星的扰动引起的，这一点从三体近似的数值实验中得到了证实，其中扰动体只有海王星，没有发生过渡变化。少

About 130 Kuiper belt objects, which are located outside of Neptune orbit, have been found since the first discovery in 1992. They are believed to be the remnants of planetesimals and their dynamical behaviors may have some information on the planetary formation at the early stage of the solar system. In this study we investigate the dynamical structures of resonances such as mean motion resonances, secular resonances, secondary resonances, and Kozai resonance and compare these structures with those of asteroids in the main belt.In the following we summarize the main results of this investigation.1)As for the mean motion resonances we mainly study (p : p+1) resonances with Neptune. Other than 1 : 2 mean motion resonance, the critical arguments of the mean motion resonances librate around 180ﾟ, On the other hand the critical arguments in the main asteroid belt librate around 0ﾟ, In the mean motion resonance area we seek the double resonance with Kozai resonance, secular resonance, and s … More econdary resonance with use of semi-analytical methods and then we confirm the existence of the double resonance and study their stability.2)We distribute about 35000 bodies near the mean motion resonance regions with different initial conditions and integrate their orbits over five million years under the perturbations from outer giant planets and study their stability. The behaviors of the stable orbits among them are in good agreement with those from the semi-analytical methods. From our numerical simulations, we found the chaotic but interesting orbits which are not predicted from the semi-analytical method. Some of them enter the resonance region from the outside and some of them get out of the resonance region. The time scale of this transitional variation is quite long. This phenomena is caused from the perturbation from mainly Uranus, which is confirmed from the numerical experiment of the three-body approximation, where the disturbing body is only Neptune and the transitional variation does not occur. Less