The Hill stability of binary asteroid and binary Kuiper Belt systems
The Hill stability of binary asteroid and binary Kuiper Belt systems
复制标题
DOI：
10.1111/j.1365-2966.2011.18720.x
复制
发表时间：
2011-07
影响因子：
4.8
通讯作者：
J. R. Donnison
中科院分区：
文献类型：
--
作者：
J. R. Donnison
从完整三体问题的Hill稳定性出发，讨论了由小行星二元系统或柯伊伯带二元系统组成的束缚三重系统在倾斜于中心第三体太阳的轨道上运动的动力学稳定性。这些三重系统的希尔稳定性区域，其中的二进制质量是非常小的相比，第三体，可以确定对中断，组件交换和捕获的可能性。这些类型的系统的二进制质量范围内的临界希尔稳定性曲线确定为不同的第二次到主要的质量比作为其轨道偏心率的函数。稳定的区域被发现增加与增加二进制质量。然而，区域的大小随着轨道偏心率的增加而大幅减小，并且随着双星的次级/初级质量比的减小而略有减小。本文对目前观测到的双星和多星系统作了一般性的讨论。在大多数系统中，主成分比副成分大得多，形成小行星-卫星系统。结果发现，那些系统的质量是很好地确定将位于稳定的区域，如果他们在圆形轨道上移动，但当他们的偏心率被考虑在内，它是不太清楚，系统是稳定的。对于那些群众没有很好地建立起来的系统来说，情况可能也是如此。可以对这些系统设置质量上限，以确保它们是希尔稳定的。对目前观测到的柯伊伯带双星也作了一般性的讨论。这些二元系统中的大多数都有次级成分，它们的直径通常与形成真正二元系统的主要成分的直径相当。与小行星双星类似，发现质量确定的双星系统如果在相对于太阳的圆形轨道上运动，则是稳定的。当考虑偏心率时，系统是否稳定就不那么清楚了。对于质量未知的系统，同样的结论也可能成立。可以再次对这些系统设置质量上限，以确保它们是希尔稳定的。
The dynamical stability of a bound triple system composed of a binary asteroid system or Kuiper Belt binary system moving on an orbit inclined to a central third body, the Sun, is discussed in terms of Hill stability for the full three-body problem. The regions of Hill stability of these triple systems, where the binary mass is very small compared with that of the third body, can be determined against the possibility of disruption, component exchange and capture. The critical Hill stability curves for the binary mass range of these types of systems are determined for different secondary-to-primary mass ratios as a function of their orbital eccentricity. The regions of stability are found to increase with increasing binary mass. The regions, however, decrease in size substantially with increasing orbital eccentricity and also decrease slightly as the secondary/primary mass ratio of the binary is decreased. The currently observed binary and multiple asteroid systems are discussed generally. In the majority of systems, the primary component is very much larger than the secondary component, forming an asteroid–satellite system. It was found that those systems where the binary mass is well determined would lie in stable regions if they moved on circular orbits, but when their eccentricity is taken into account, it is less clear that the systems are stable. The same is likely to be true for the systems where the masses are not well established. Upper mass limits could be placed on these systems that would ensure they are Hill stable. The currently observed Kuiper Belt binaries were also discussed generally. The majority of these binary systems have secondary components which are often comparable to the diameter of the primary component forming a true binary system. Similar to the asteroid binaries, it was found that binary systems where the mass was well determined were stable if they moved on circular orbits relative to the Sun. When the eccentricity is taken into account, it is less clear that the systems are stable. The same conclusions are also likely to be true for the systems with unknown masses. Upper mass limits again can be placed on these systems that would ensure they are Hill stable.