绘架座β星c的希尔球凌日与另一类1981年类似事件的搜寻
The Hill sphere transits of Beta Pictoris c and the search for another 1981-like event
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中文总结 AI 辅助
本研究针对绘架座β星c的希尔球凌日，搜寻1981年类似的光度波动事件，未发现有力证据，排除其与绘架座β星b、c希尔球相关的假设，为2028年观测提供方向。
中文摘要 AI 辅助
绘架座β星是一个年轻且邻近的行星系统，拥有一个边缘朝向的碎屑盘和至少三颗气态巨行星，其行星周围的环境可能存在系外卫星和星环，探测这些天体将对卫星和行星形成理论极具参考价值。1981年观测到绘架座β星存在约4%的光度波动，表明该系统发生了尘埃凌日，这可能与两颗内侧行星的希尔球有关。我们通过搜寻2017年至2023年多期测光数据中的类似事件，来探究1981年事件的起源，并在绘架座β星c的希尔球凌日中寻找行星周围物质的迹象。我们将BRITE卫星、bRing以及ASTEP天文台的观测数据拟合到1981年事件的模型中，以搜寻类似事件，同时采用简单的平盘模型搜寻与行星周围盘凌日相符的信号。尽管未在希尔球主凌期间找到1981年事件的有力证据，但我们确实发现了2019年7月26日前后的一个候选事件。由于绘架座β星c最近投影分离时间存在不确定性，无法可靠确定2018年主凌期间是否存在盘结构，不过bRing对第二次主凌的测光为希尔球尘埃含量设定了上限，约为10²²克物质。由于在测光时间序列中绘架座β星c的凌日期间未发现与1981年事件类似的有力证据，我们排除了该事件与绘架座β星c和绘架座β星b的希尔球相关的假设。未来2028年下一次希尔球凌日可通过地面天文台和PLATO望远镜实现观测，PLATO的首次长期科学指向将包含绘架座β星。
英文摘要
Beta Pictoris is a young and nearby planetary system hosting an edge-on debris disk and at least three gas-giant planets. Their circumplanetary environments could host exomoons and rings, a detection of which would be highly informative for moon and planet formation theories. A photometric fluctuation of about 4% was seen towards Beta Pictoris in 1981, indicating the transit of dust in the system, which could be associated with the Hill spheres of the two inner planets. We search for the origin of the 1981 event by searching for an analogous event in multi-epoch photometry from 2017 to 2023, and look for signs of circumplanetary material in transits of the Hill sphere of Beta Pictoris c. Observations from the BRITE satellite, and the bRing and ASTEP observatories are fitted to a model of the 1981 event to search for a similar event, and also search for a signal consistent with a circumplanetary disk transit using a simple flat disk model. No compelling evidence for a 1981 event during a Hill sphere primary transit is found, although we do find a candidate event around 2019 July 26. Due to the uncertainty in the time of closest projected separation of Beta Pictoris c, a search for a disk during the primary transit of 2018 could not be robustly determined, but bRing photometry for the second primary transit places an upper limit on the dust content of the Hill sphere of ~ $10^{22}$ grams of material. With no compelling detection of an event similar to that seen in 1981 during the transits of Beta Pictoris c in the photometric time series, we rule out the hypothesis that this event was related to the Hill spheres of Beta Pictoris c and Beta Pictoris b. Future observations of the next Hill sphere transit in 2028 can be realised with both ground-based observatories and with PLATO, whose first long duration science pointing will include Beta Pictoris.
发表机构
- Leiden University（莱顿大学）
- Universität Innsbruck（因斯布鲁克大学）
- Université Côte d’Azur（蔚蓝海岸大学）
- European Southern Observatory（欧洲南方天文台）
- University of Southern Queensland（昆士兰南部大学）
- Northwestern University（西北大学）
- Johns Hopkins University（约翰斯·霍普金斯大学）
- Space Telescope Science Institute（太空望远镜科学研究所）
- Observatoire de Paris（巴黎天文台）
- PSL（巴黎文理研究大学）
- Sorbonne Université（索邦大学）
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