A photometric study of the short-period eclipsing binary 1SWASP J204932.94-654025.8, showing strong third light

被引:2
|
作者
Zhang, Bin [1 ,2 ]
Qian, Sheng-Bang [1 ,2 ,3 ,4 ,5 ,6 ]
Zejda, Miloslav [7 ]
Wang, Jing-Jing [8 ]
Zhi, Qi-Jun [1 ,2 ]
Dong, Ai-Jun [1 ,2 ]
Xie, Wei [1 ,2 ]
Zhu, Li-Ying [3 ,4 ,5 ]
Jiang, Lin-Qiao [9 ]
机构
[1] Guizhou Normal Univ, Sch Phys & Elect Sci, Guiyang 550001, Guizhou, Peoples R China
[2] Guizhou Normal Univ, Guizhou Prov Key Lab Radio Astron & Data Proc, Guiyang 550001, Guizhou, Peoples R China
[3] Chinese Acad Sci, Yunnan Observ, POB 110, Kunming 650216, Yunnan, Peoples R China
[4] Chinese Acad Sci, Key Lab Struct & Evolut Celestial Objects, POB 110, Kunming 650216, Yunnan, Peoples R China
[5] Univ Chinese Acad Sci, Yuquan Rd 19,Sijingshang Block, Beijing 100049, Peoples R China
[6] Chinese Acad Sci, Ctr Astron Mega Sci, 20A Datun Rd, Beijing 100012, Peoples R China
[7] Masaryk Univ, Dept Theoret Phys & Astrophys, Kotlarska 2, Brno 61137, Czech Republic
[8] China Univ Petr Beijing Karamay, Anding Rd 355, Karamay 834000, Peoples R China
[9] Sichuan Univ Sci & Engn, Sch Phys & Elect Engn, Zigong 643000, Peoples R China
基金
中国国家自然科学基金;
关键词
Binary; Eclipsing binary; Orbital period; Light curves; CONTACT BINARIES; CLOSE BINARIES; STARS; LIMIT; MASS; CURVES;
D O I
10.1016/j.newast.2019.101324
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
1SWASP J204932.94-654025.8 (hereafter J2049) is a newly discovered eclipsing binary system with an orbital period of 0.2299103 days. BVRc light curves (LCs) are presented and analyzed by using the 2013 version of the Wilson-Devinney (W-D) program. Because the observed LCs are asymmetric, a hot star-spot was employed on the secondary component during our analysis. We found that 32049 is a W-subtype shallow contact eclipsing binary system with an orbit inclination of 62.69 +/- 0.95 and a mass ratio of q =1.326 +/- 0.056. More importantly, we found the presence of a strong third light, with an average luminosity contribution of 31.3% of the total light. Based on times of the light minima, the orbital period changes of J2049 are studied for the first time, and there is no evidence for any significant dp/dt now. Considering the presence of the third light and the short time span of the eclipse times, more observations are needed in the future.
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页数:5
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