Five Massive Contact Binaries with Twin Components in LMC
Massive contact binaries refer to the close binary systems in which the components have filled their respective Roche lobes and share a common envelope with early-type spectra. Twin binaries are a special type of binary system characterized by two components with nearly equal masses. The Magellanic...
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| Format: | Article |
| Language: | English |
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IOP Publishing
2023-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/acf196 |
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| author | Fu-Xing Li Sheng-Bang Qian Chu-Qi Wu Min-Yu Li Er-Gang Zhao Wen-Ping Liao Li-Ying Zhu Qi-Bin Sun Jia Zhang |
| author_facet | Fu-Xing Li Sheng-Bang Qian Chu-Qi Wu Min-Yu Li Er-Gang Zhao Wen-Ping Liao Li-Ying Zhu Qi-Bin Sun Jia Zhang |
| author_sort | Fu-Xing Li |
| collection | DOAJ |
| description | Massive contact binaries refer to the close binary systems in which the components have filled their respective Roche lobes and share a common envelope with early-type spectra. Twin binaries are a special type of binary system characterized by two components with nearly equal masses. The Magellanic Cloud, comprising the Large Magellanic Cloud (LMC) and the Small Magellanic Cloud, is a fascinating galaxy that is distinct from the Milky Way. With its low metallicity, it serves as an ideal test bed for studying the formation and evolution of massive binaries and testing theoretical models. In this work, based on long-term observations with Optical Gravitational Lensing Experiment and MAssive Compact Halo Object in the LMC, we identified and performed comprehensive analyses of five massive twin contact binaries via the method of the light travel time effect and Wilson–Devinney code. The results show that all of these twin binaries are accompanied by low-mass third bodies. The third bodies have minimum masses ranging from 0.33 to 1.46 M _⊙ . Their orbital periods range from 4.34 to 12.03 yr. The maximum distances between the third bodies and the central binary systems range from 6.7 to 11.4 au. Remarkably, four out of the five massive twins have evolved into deep-contact binaries, which indicates that all of them may have originated from Case A mass transfer. These results strongly suggest the significant influence of the third body in the formation and evolution of massive contact binaries and may hold the key to unraveling the origins of massive binaries. |
| first_indexed | 2024-03-11T19:24:09Z |
| format | Article |
| id | doaj.art-8c0124a256d24623b343475dcbf6b1c5 |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-11T19:24:09Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-8c0124a256d24623b343475dcbf6b1c52023-10-06T17:17:56ZengIOP PublishingThe Astrophysical Journal1538-43572023-01-0195614910.3847/1538-4357/acf196Five Massive Contact Binaries with Twin Components in LMCFu-Xing Li0https://orcid.org/0000-0002-0285-6051Sheng-Bang Qian1Chu-Qi Wu2Min-Yu Li3https://orcid.org/0000-0002-8564-8193Er-Gang Zhao4Wen-Ping Liao5https://orcid.org/0000-0001-9346-9876Li-Ying Zhu6https://orcid.org/0000-0002-0796-7009Qi-Bin Sun7https://orcid.org/0000-0003-0516-404XJia Zhang8https://orcid.org/0000-0003-2017-9151Yunnan Observatories, Chinese Academy of Sciences (CAS) , P.O. Box 110, 650216 Kunming, People's Republic of China ; lfx@ynao.ac.cn; Department of Astronomy, Key Laboratory of Astroparticle Physics of Yunnan Province, Yunnan University , Kunming 650091, People's Republic of China; Key Laboratory of the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences , P.O. Box 110, 650216 Kunming, People's Republic of ChinaYunnan Observatories, Chinese Academy of Sciences (CAS) , P.O. Box 110, 650216 Kunming, People's Republic of China ; lfx@ynao.ac.cn; Department of Astronomy, Key Laboratory of Astroparticle Physics of Yunnan Province, Yunnan University , Kunming 650091, People's Republic of China; Key Laboratory of the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences , P.O. Box 110, 650216 Kunming, People's Republic of China; University of Chinese Academy of Sciences , No.1 Yanqihu East Road, Huairou District, Beijing, 101408, People's Republic of ChinaYunnan Observatories, Chinese Academy of Sciences (CAS) , P.O. Box 110, 650216 Kunming, People's Republic of China ; lfx@ynao.ac.cn; Key Laboratory of the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences , P.O. Box 110, 650216 Kunming, People's Republic of China; University of Chinese Academy of Sciences , No.1 Yanqihu East Road, Huairou District, Beijing, 101408, People's Republic of ChinaYunnan Observatories, Chinese Academy of Sciences (CAS) , P.O. Box 110, 650216 Kunming, People's Republic of China ; lfx@ynao.ac.cn; Key Laboratory of the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences , P.O. Box 110, 650216 Kunming, People's Republic of China; University of Chinese Academy of Sciences , No.1 Yanqihu East Road, Huairou District, Beijing, 101408, People's Republic of ChinaYunnan Observatories, Chinese Academy of Sciences (CAS) , P.O. Box 110, 650216 Kunming, People's Republic of China ; lfx@ynao.ac.cn; Key Laboratory of the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences , P.O. Box 110, 650216 Kunming, People's Republic of ChinaYunnan Observatories, Chinese Academy of Sciences (CAS) , P.O. Box 110, 650216 Kunming, People's Republic of China ; lfx@ynao.ac.cn; Key Laboratory of the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences , P.O. Box 110, 650216 Kunming, People's Republic of China; University of Chinese Academy of Sciences , No.1 Yanqihu East Road, Huairou District, Beijing, 101408, People's Republic of ChinaYunnan Observatories, Chinese Academy of Sciences (CAS) , P.O. Box 110, 650216 Kunming, People's Republic of China ; lfx@ynao.ac.cn; Key Laboratory of the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences , P.O. Box 110, 650216 Kunming, People's Republic of China; University of Chinese Academy of Sciences , No.1 Yanqihu East Road, Huairou District, Beijing, 101408, People's Republic of ChinaYunnan Observatories, Chinese Academy of Sciences (CAS) , P.O. Box 110, 650216 Kunming, People's Republic of China ; lfx@ynao.ac.cn; Key Laboratory of the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences , P.O. Box 110, 650216 Kunming, People's Republic of China; University of Chinese Academy of Sciences , No.1 Yanqihu East Road, Huairou District, Beijing, 101408, People's Republic of ChinaYunnan Observatories, Chinese Academy of Sciences (CAS) , P.O. Box 110, 650216 Kunming, People's Republic of China ; lfx@ynao.ac.cn; Key Laboratory of the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences , P.O. Box 110, 650216 Kunming, People's Republic of ChinaMassive contact binaries refer to the close binary systems in which the components have filled their respective Roche lobes and share a common envelope with early-type spectra. Twin binaries are a special type of binary system characterized by two components with nearly equal masses. The Magellanic Cloud, comprising the Large Magellanic Cloud (LMC) and the Small Magellanic Cloud, is a fascinating galaxy that is distinct from the Milky Way. With its low metallicity, it serves as an ideal test bed for studying the formation and evolution of massive binaries and testing theoretical models. In this work, based on long-term observations with Optical Gravitational Lensing Experiment and MAssive Compact Halo Object in the LMC, we identified and performed comprehensive analyses of five massive twin contact binaries via the method of the light travel time effect and Wilson–Devinney code. The results show that all of these twin binaries are accompanied by low-mass third bodies. The third bodies have minimum masses ranging from 0.33 to 1.46 M _⊙ . Their orbital periods range from 4.34 to 12.03 yr. The maximum distances between the third bodies and the central binary systems range from 6.7 to 11.4 au. Remarkably, four out of the five massive twins have evolved into deep-contact binaries, which indicates that all of them may have originated from Case A mass transfer. These results strongly suggest the significant influence of the third body in the formation and evolution of massive contact binaries and may hold the key to unraveling the origins of massive binaries.https://doi.org/10.3847/1538-4357/acf196Multiple starsEclipsing binary starsEarly stellar evolutionEarly-type stars |
| spellingShingle | Fu-Xing Li Sheng-Bang Qian Chu-Qi Wu Min-Yu Li Er-Gang Zhao Wen-Ping Liao Li-Ying Zhu Qi-Bin Sun Jia Zhang Five Massive Contact Binaries with Twin Components in LMC The Astrophysical Journal Multiple stars Eclipsing binary stars Early stellar evolution Early-type stars |
| title | Five Massive Contact Binaries with Twin Components in LMC |
| title_full | Five Massive Contact Binaries with Twin Components in LMC |
| title_fullStr | Five Massive Contact Binaries with Twin Components in LMC |
| title_full_unstemmed | Five Massive Contact Binaries with Twin Components in LMC |
| title_short | Five Massive Contact Binaries with Twin Components in LMC |
| title_sort | five massive contact binaries with twin components in lmc |
| topic | Multiple stars Eclipsing binary stars Early stellar evolution Early-type stars |
| url | https://doi.org/10.3847/1538-4357/acf196 |
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