发表机构
University of Padua; Aristotle University of Thessaloniki; University of Warwick; Democritus University of Thrace（帕多瓦大学; 塞萨洛尼基亚里士多德大学; 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
本研究通过扩展白矮星-次级天体-尘埃共轨圆形限制性三体问题至更高次级质量，发现新分岔点与周期轨道族，并利用N体模拟揭示水星、地球和海王星质量类似物可在10年内使尘埃轨道周期产生显著偏差，为探测未直接观测的共轨系外行星提供新方法。
AI 中文摘要
（删节版）越来越多的对凌星尘埃碎片绕白矮星运行的观测显示，这些碎片呈现出复杂的特征，通常伴有轨道周期漂移。这些碎片的母体小行星或行星可能仍部分完好地运行在近圆轨道上，该轨道可能倾斜或共面，其周期与尘埃的周期相似。或者，这些碎片可能与其他完整的小行星或行星同时存在，这些天体后来在白矮星周围通过潮汐作用变为圆轨道，但仍然无法直接观测到。我们首先试图通过将我们先前对白矮星-次级天体-尘埃共轨圆形限制性三体问题（CRTBP）的研究扩展到更高的次级天体质量（对应谷神星、水星、地球和海王星）来改进对这一可探测性阈值的识别。接下来，我们继续探索CRTBP的解析表征与数值表征之间的联系。首先，我们在平面和空间CRTBP情形下计算了1/1平均运动共振（MMR）中的周期轨道族，其中尘埃处于任意偏心的轨道上。其次，我们生成了全局相空间图。第三，我们通过N体模拟确定了与白矮星非常接近的碎片的观测联系。对于我们应用的每种方法，我们都报告了一组新颖的结果。这些结果包括3个新发现的分岔点，$B_T^4, B_{cs}^4$和$B_{cs}^5$，在二维CRTBP中高尘埃偏心率区域有2个非对称周期轨道分支，称为$A_2$和$A_3$，以及在三维CRTBP中有2个对称轨道族。这些图揭示了稳定性区域，它们是尘埃偏心率、近心点幅角以及相对于1/1 MMR的半长轴微小偏差的函数。N体模拟显示，在10年内，水星、地球和海王星的质量类似物分别使尘埃的轨道周期产生1-10秒、10-100秒和超过100秒的偏差。
英文摘要
Abridged. Mounting observations of transiting dusty debris orbiting WDs display complex signatures that often feature orbital period drifts. The asteroid or planet progenitor of this debris might still be partly intact on a near-circular orbit that is inclined or coplanar, with a period that is similar to that of the dust. Alternatively, the debris could persist concurrently with other intact asteroids or planets that had tidally circularised around the WD at a later time, but still remain directly unobservable. We sought to first improve the identification of this detectability threshold by expanding our previous investigation of the WD-secondary-dust co-orbital circular restricted three-body problem (CRTBP) to higher secondary masses corresponding to Ceres, Mercury, Earth, and Neptune. Next, we continued to explore the link between the analytic and numerical characterisations of the CRTBP. First, we computed families of periodic orbits in the 1/1 mean-motion-resonance (MMR) in both the planar and spatial CRTBP cases, where the dust is on an arbitrarily eccentric orbit. Second, we generated global phase space portraits. Third, we determined observational links with debris located in very close proximity to WDs via N-body simulations. For each method we applied, we report a novel set of results. These include 3 newly discovered bifurcation points, $B_T^4, B_{cs}^4$, and $B_{cs}^5$, 2 branches of asymmetric periodic orbits, called $A_2$ and $A_3$, at high dust eccentricity regime in the 2D-CRTBP, and 2 families of symmetric orbits in the 3D-CRTBP. The maps reveal stability domains as a function of the dust's eccentricity, argument of pericentre, and slight semi-major axis deviations from the 1/1 MMR. The N-body simulations reveal that over 10 yr, mass analogues of Mercury, Earth, and Neptune generate orbital period deviations in the dust of, respectively, 1-10 s, 10-100 s, and over 100 s.
CommentsAccepted for publication in A&A
DOI：10.1051/0004-6361/202661508
