BSN-VII：三颗冷、大振幅、低质量W亚型相接双星的测光光变曲线研究
BSN-VII: Photometric Light Curve Study of Three Cool, Large-Amplitude, Low Mass, W-Subtype Contact Binaries
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中文总结 AI 辅助
本研究结合地基与TESS空间测光，用BSN应用和MCMC方法分析三颗W亚型低质量相接双星的光变曲线，研究其构型、O'Connell效应及轨道周期变化，揭示了不同系统的周期模型适配性差异。
中文摘要 AI 辅助
我们结合地基观测与空间TESS测光，对三颗W UMa型相接双星系统V1104 Her、V1284 Her和V2822 Ori开展了全面的测光研究。利用BSN应用在相接构型下对光变曲线进行建模，通过马尔可夫链蒙特卡洛（MCMC）方法估计参数及其不确定度。推导的解表明目标系统处于浅相接构型，被归类为W亚型相接双星，其中质量更大的子星比其伴星更冷。V1284 Her的光变曲线呈现明显的O'Connell效应，通过在主星上引入一个冷星斑可重现该效应。利用轨道周期与半长轴的经验参数关系估计绝对参数，得到子星质量范围为0.48-0.86 M☉，证实了这些系统的低质量特性。通过检查线性和周期模型，利用文献、地基观测及TESS数据的食时研究轨道周期变化。统计模型比较表明，周期模型能更好地描述V1104 Her和V1284 Her的食时，而线性模型更适合V2822 Ori，尽管两种模型间的差异相对较小。
英文摘要
We present a comprehensive photometric study of three W UMa-type contact binary systems, V1104 Her, V1284 Her, and V2822 Ori, based on a combination of ground-based observations and space-based TESS photometry. The light curves were modeled using the BSN application under a contact configuration, with parameters and their uncertainties estimated through the Markov Chain Monte Carlo (MCMC) approach. The derived solutions indicate that the target systems are in a shallow-contact configuration. The target systems are classified as W-subtype contact binaries, with the more massive component cooler than its companion. The light curve of V1284 Her shows a pronounced O'Connell effect, which is reproduced by introducing a cool starspot on the primary component. Absolute parameters were estimated using the empirical parameter relationship between orbital period and semi-major axis, yielding component masses in the range $0.48$-$0.86\,M_\odot$ and confirming the low-mass nature of the systems. Orbital period variations were investigated using eclipse timings from the literature, ground-based observations, and TESS data by examining both linear and cyclic models. Statistical model comparison indicates that the cyclic model provides a better description of the eclipse timings for V1104 Her and V1284 Her, whereas the linear model is preferred for V2822 Ori, although the difference between the two models is relatively small.
发表机构
- LUX, Observatoire de Paris, CNRS, PSL（巴黎天文台）
- Astronomy Department, Raderon AI Lab.（拉德伦人工智能实验室天文学系）
- Instituto de Astronomía, UNAM（墨西哥国立自治大学天文学研究所）
- Farzanegan Institute（法尔扎内甘学院）
- Farhangian Institute（法尔洪吉安学院）
- Damghan Branch of the National Organization for Development of Exceptional Talents (SAMPAD)（国家特殊才能发展组织达姆甘分部）
- IPSA Institut Polytechnique des Sciences Avancées（高级科学理工学院）
- Çanakkale Onsekiz Mart University, Faculty of Science, Department of Physics（恰纳卡莱18三月大学理学院物理学系）
- Çanakkale Onsekiz Mart University, Astrophysics Research Center and Ulupnar Observatory（恰纳卡莱18三月大学天体物理研究中心和乌鲁普纳观测站）
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