相接双星LP UMa轨道周期变化研究的新进展  

Progress of the Research on the Orbital Period Variation of the Contact Binary LP UMa

作　　者：李迎港 郑捷 陈天禄[1,2] 江林巧 鲍华 索南达吉 许超 LI Yinggang;ZHENG Jie;CHEN Tianlu;JIANG Linqiao;BAO Hua;Suonan-Daji;XU Chao(The Key Laboratory of Cosmic Rays(Tibet University),Ministry of Education,Lhasa 850000,China;Department of Physics,College of Science,Tibet University,Lhasa 850000,China;Key Laboratory of Optical Astronomy,National Astronomical Observatories,Chinese Academy of Sciences,Beijing 100101,China;College of Mathematics and Physics,Leshan Normal University,Leshan 614000,China)

机构地区：[1]西藏大学宇宙线教育部重点实验室,拉萨850000 [2]西藏大学理学院物理系,拉萨850000 [3]中国科学院国家天文台光学天文重点实验室,北京100101 [4]乐山师范学院数理学院物理系,乐山614000

出　　处：《天文学进展》2025年第1期129-141,共13页Progress In Astronomy

基　　金：西藏大学研究生“高水平人才培养计划”(2021-GSP-S039);西藏大学中央财政支持地方高校改革发展资金(00060858,00060867-01,00061082)。

摘　　要：LP UMa是一颗g波段亮度为13.34 mag的W UMa型相接双星,1997年首次被观测到,至今已有超过25 a的观测时间跨度,近400条极小时刻记录。多年来有数位研究者使用不同的数据和方法对其进行了研究,得出了不同的结论。自2022年12月―2023年12月,对相接双星LP UMa进行了8次观测,得到了11个极小时刻;同时从TESS数据库和AAVSO数据库中分别收集130和35个极小时刻,以及来自文献的214个极小时刻。基于这390个极小时刻重新研究了LP UMa的轨道周期变化,修正了之前作者关于该系统的轨道周期正在迅速增加和两子星之间存在快速的物质转移的结论。研究表明,LP UMa轨道周期的快速增加其实是周期性变化的一部分,很可能是第三天体的光时轨道效应引起了该系统O-C曲线的周期性变化,并算出第三天体的周期约为41.7 a,轨道偏心率约为0.0701,证实了LP UMa很可能也是一个存在第三天体的晚型相接双星系统。LP UMa is a W UMa type binary star with a brightness of 13.34 mag in the g-band.It has been observed for over 25 years since its first observation in 1997,with nearly 400 records of minimum moments.Over the years,multiple researchers have used different data and methods to study it,and have come to different research conclusions.Eight new observations have been done for the contact binary LP UMa by ground-based optical telescopes from December 2022 to December 2023,resulting in 11 determined times of light minimum in this paper.130 and 35 times of light minimum were derived from the TESS database and the American Association of Variable Stars Observers(AAVSO)database respectively,with an additional 214 minimum moments from literatures.Based on the total of 390 minimum moments mentioned above,the orbital period change of LP UMa was restudied,revising the previous conclusion that the rapid increase in the orbital period of the system is due to rapid material transfer between the binary stars.This research indicates that the rapid increase in the orbital period of LP UMa is actually part of the periodic variation,most likely caused by the optical time orbit effect of a third celestial body.We calculated that the period of the third celestial body is about 41.7 years,and the orbital eccentricity is about 0.0701,confirming that LP UMa is highly likely a late-type connected binary system with a third celestial body.

关 键 词：双星 LP UMa O-C 第三天体 光时轨道效应 

分 类 号：P153[天文地球—天文学]