Stability Analysis of Earth Co-orbital Objects
Stability Analysis of Earth Co-orbital Objects
复制标题
地球共轨物体的稳定性分析
DOI：
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发表时间：
2022
期刊：
影响因子：
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通讯作者：
D. Qiao
中科院分区：
文献类型：
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作者：
Yi Qi;D. Qiao
本文研究了基于环面结构的地球共轨天体的稳定性问题。哈密顿量是评价共轨稳定性的一个指标。根据环面空间中蝌蚪面、马蹄面、准卫星面和临界复合面的拓扑特征，将共轨区域划分为若干区域。我们选择了221个潜在的ECO作为代表性样本。对日地系统的数值积分表明，在QS-HS和QS-TP运动中，碰撞线以上的大部分天体是短期或长期稳定的ECO，而在不稳定区的大部分天体是不稳定的ECO，这与我们的半解析结论一致。具有较大哈密顿量值的ECO的稳定性可能更强。提出了一种无需长期数值积分的确定潜在ECO长期共轨稳定性的有效方法。在多行星模型中的数值积分表明，我们的稳定性分析仍然适用于真实的太阳系。作为我们的稳定性分析的应用，两个确定的QS-HS ECO碰撞线以上的第一次确定和分析。例如，2019年VL 5的QS-HS状态可以持续超过3000年，而其当前的HS状态将持续至少800年。
In this paper, we investigate the stability of Earth co-orbital objects (ECOs) based on the torus structure. The Hamiltonian value is an index to evaluate co-orbital stability. According to topological characters of tadpole (TP), horseshoe (HS), quasi-satellite (QS), and critical compound surfaces in the torus space, the co-orbital area is divided into several regions in detail. We select 221 potential ECOs as representative samples. Numerical integration in the Sun–Earth system illustrates that most of objects above the collision line are short- or long-term stable ECOs in the QS–HS and QS–TP motions, and most of objects in the unstable region are unstable ones, which is in agreement with our semi-analytical conclusions. The stability of an ECO with a larger Hamiltonian value could be stronger. An efficient method to determine the long-term co-orbital stability of a potential ECO is proposed without long-term numerical integration. Numerical integration in the multiplanet model demonstrates that our stability analysis is still applicable for the real solar system. As an application of our stability analysis, two well-determined QS–HS ECOs above the collision line are identified and analyzed for the first time. For instance, the QS–HS state of 2019 VL5 can be sustained for more than 3000 yr, and its current HS state will be sustained for at least 800 yr.
影响因子：
3.2
作者：
A. Christou;G. Borisov;A. Dell’Oro;Seth Andrew Jacobson;A. Cellino;E. Unda-Sanzana
通讯作者：
A. Christou;G. Borisov;A. Dell’Oro;Seth Andrew Jacobson;A. Cellino;E. Unda-Sanzana
火星 L5 特洛伊小行星的组成和起源：光谱学的见解
影响因子：
3.2
作者：
Christou A
通讯作者：
Christou A