AI 中文总结
本研究分析NGTS观测到的NOI 105872系统，其深不对称凌食表明存在环次级星盘候选体，盘半径约0.005天文单位，为年轻恒星环境中的盘动力学提供基准。
AI 中文摘要
年轻恒星系统为理解恒星/行星形成过程提供了关键见解，通常表现出复杂且不断演化的测光变率。在本文中，我们分析了围绕 NOI 105872 的天体，该天体由下一代凌星巡天（NGTS）观测到，凌食了一颗位于猎户座星云星团中的年轻（$4.1\pm0.4$ Myr）M 型恒星。该系统表现出深度、不对称的凌食，周期约为 0.69 天，同时凌食形态存在变化。我们结合了来自多个地面和空间设施、跨度约十年的测光观测，以研究该系统的性质。我们探索了一系列物理情景来重现凌食轮廓及其演化。经过分析，我们首选的解释是围绕 M 型主星轨道上的伴星的一个环次级星盘。我们采用六参数盘模型，并对每个数据集独立拟合凌食轮廓。最佳拟合解给出的盘半径约为 0.005 天文单位或 0.98 倍恒星半径，各历元间的取向大致一致，但存在可能归因于盘进动或恒星内在变率的差异。希尔半径的约束表明伴星质量与极低质量恒星伴星一致。这些结果确立了 NOI 105872 作为年轻恒星环境中环次级星盘系统的候选体。持续的测光监测和光谱后续观测对于确认这一解释至关重要。如果得到确认，像 NOI 105872 这样的系统将为理解盘动力学、伴星形成以及年轻恒星中复杂凌食现象的起源提供宝贵的基准。
英文摘要
Young stellar systems provide key insights into the processes governing star/planet formation, often exhibiting complex and evolving photometric variability. In this paper, we present an analysis of the object around NOI 105872, observed by the Next Generation Transit Survey (NGTS) to eclipse a young ($4.1\pm0.4$ Myr) M-type star in the Orion Nebula Cluster. The system displays deep, asymmetric eclipses with a period of $\sim0.69$ days, alongside variability in morphology. We combine photometric observations spanning approximately a decade from multiple ground- and space-based facilities to investigate the nature of this system. We explore a range of physical scenarios to reproduce the eclipse profiles and their evolution. After analysis, our preferred explanation is a circumsecondary disk surrounding a companion in orbit around the M-type primary. We adopt a six-parameter disk model and fit the eclipse profiles independently to each dataset. The best-fitting solution yields a disk radius of $\sim 0.005 \mathrm{au}$ or $0.98 R_{*}$, with broadly consistent orientations across epochs, but with variations that may be attributed to disk precession or intrinsic stellar variability. Constraints from the Hill radius imply a companion mass consistent with a very low-mass stellar companion. These results establish NOI 105872 as a candidate for a circumsecondary disk system in a young stellar environment. Continued photometric monitoring and spectroscopic follow-up will be essential to confirm this interpretation. If confirmed, systems such as NOI 105872 provide valuable benchmarks for understanding disk dynamics, companion formation, and the origin of complex eclipse phenomena in young stars.
Comments18 pages, 16 figures. Accepted for publication in MNRAS
