发表机构
Universidade de Coimbra; Universidade Estadual Paulista (UNESP); Observatoire de Paris, Université PSL, Sorbonne Université, CNRS; The University of Hong Kong; Hong Kong Institute for Astronomy and Astrophysics, The University of Hong Kong; Zentrum für Astronomie der Universität Heidelberg; Sofia University St. Kliment Ohridski（科英布拉大学; 圣保罗州立大学; 巴黎天文台，巴黎文理研究大学，索邦大学，法国国家科学研究中心; 香港大学; 香港大学香港天体物理研究所; 海德堡大学天文学中心; 索菲亚大学）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本研究利用蒙特卡洛方法和角稳定图，结合频率分析，约束ν Octantis系统中逆行行星的轨道，发现其最可能处于28/−11平均运动共振区域，并通过拱线对齐增强长期稳定性。
AI 中文摘要
ν Octantis系统由一个致密的恒星双星和一个逆行S型行星组成，该行星在接近稳定边界处运行。在此，我们通过蒙特卡洛方法探索行星轨道要素，研究该系统的动力学可行构型。为处理大量自由参数，我们采用了一种新方法，即同时改变所有相关轨道参数，我们称之为角稳定图。此外，由于行星的密切轨道周期发生大幅振荡，我们将这些图与频率分析相结合，以识别与观测数据一致的稳定构型。我们发现，逆行行星轨道最可能位于高阶28/−11平均运动共振的影响区域内，其长期稳定性通过长期拱线对齐得到增强。
英文摘要
The $ν$ Octantis system is composed of a compact stellar binary and a retrograde S-type planet orbiting near the edge of stability. Here, we investigate the dynamically viable architectures of this system by exploring the planetary orbital elements with a Monte Carlo method. To handle the large number of free parameters, we employed a novel approach in which all relevant orbital parameters were varied simultaneously, which we refer to as corner stability maps. Furthermore, since the osculating orbital period of the planet undergoes large oscillations, we combined these maps with frequency analysis to identify the stable configurations that remain consistent with the observational data. We find that the retrograde planetary orbit most likely lies in the region of influence of the high-order 28/$-$11 mean-motion resonance, where its long-term stability is enhanced by secular apsidal alignment.
Comments18 pages, 11 figures, Published in A&A
DOI：10.1051/0004-6361/202555409
