发表机构
Aristotle University of Thessaloniki; University of Warwick; Democritus University of Thrace（萨洛尼卡亚里士多德大学; 华威大学; 色雷斯德谟克利特大学）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究将椭圆型限制性三体问题应用于白矮星周围的尘埃粒子，发现高偏心率下的新不对称周期轨道族，并通过N体模拟表明水星质量行星可产生显著轨道周期偏差，有助于探测隐藏的共轨系外行星。
AI 中文摘要
（摘要已删节。）我们的目标是将论文 I 推广到次星体为偏心轨道的情形，并在此分析椭圆型限制性三体问题（ERTBP）。我们的次星体质量包括谷神星、水星、地球和海王星，以便通过我们的分析帮助推断大型小行星和行星的存在。我们研究了平面（2D-ERTBP）和非共面（3D-ERTBP）轨道上的尘埃粒子。我们在2D-ERTBP和3D-ERTBP中计算了1/1共振对称和不对称周期轨道的族。这样做产生了本身具有新颖性的结果，并为我们的后续步骤提供了精确指导的诊断工具。基于这些结果，我们生成了详细的相图。最后，我们运行了适当播种的N体模拟，以与周期轨道进行比较，并为白矮星附近的碎片提供观测联系。在高偏心率2D-ERTBP区域中，发现了新的不对称周期轨道族，称为$E^A_{41}$、$E^A_{42}$和$E^A_{43}$。它们由新的分岔点$B_T^4$沿论文 I 中展示的新$A_2$族产生。此外，还发现了新的孤立不对称周期轨道族，即$E^A_{44}$、$E^A_{45}$和$E^A_{46}$。从$L_4$出发的短周期和长周期不对称轨道族，称为$E^A_S$和$E^A_L$，也被计算出来。在2D-和3D-ERTBP区域中，大多数对称或不对称周期轨道族的尘埃粒子都表现出高偏心运动。N体模拟揭示，在十年时间内，尘埃的轨道周期偏差高于圆形限制性三体问题（论文 I）中的偏差；在某些架构中，水星质量的行星可以定期产生超过约100秒的偏差，这可能有助于对隐藏的小行星或绕白矮星运行的行星进行观测推断。
英文摘要
Abridged. We aim to extend Paper I to the eccentric secondary orbit case and now analyse the elliptic restricted three-body problem (ERTBP). Our secondary masses include Ceres, Mercury, Earth, and Neptune so that we can help infer the presence of both large asteroids and planets through our analysis. We study dust particles on both planar (2D-ERTBP) and non-coplanar (3D-ERTBP) orbits. We computed families of 1/1 resonant symmetric and asymmetric periodic orbits in the 2D-ERTBP and 3D-ERTBP. Doing so produces novel results in their own right and diagnostic tools for precise guidance for our next steps. Based on them, we generated detailed phase portraits. Finally, we run suitably seeded $N$-body simulations to compare with the periodic orbits, and to provide observational links with debris close to WDs. New families of asymmetric periodic orbits, called $E^A_{41}$, $E^A_{42}$, and $E^A_{43}$ in the high-eccentricity 2D-ERTBP regime were discovered. They are generated by the new bifurcation point, $B_T^4$, along the new $A_2$ family, showcased in Paper I. Moreover, new isolated families of asymmetric periodic orbits, namely $E^A_{44}$, $E^A_{45}$, and $E^A_{46}$ were discovered. Families of short- and long- period asymmetric orbits starting from $L_4$, called $E^A_S$ and $E^A_L$, were also computed. In both the 2D- and 3D-ERTBP regimes, highly eccentric motion is exhibited for the dust particles in the majority of the families of either symmetric or asymmetric periodic orbits. The $N$-body simulations reveal that over ten years, the orbital period deviations of the dust are higher than in the circular restricted three-body problem (Paper I); in some architectures, Mercury-mass planets can regularly generate deviations exceeding $\sim$100 s, which potentially aids observational inferences of hidden asteroids or planets orbiting WDs.
CommentsAccepted for publication in A&A
DOI：10.1051/0004-6361/202661509
