The First Photometric Analysis of Two Low-mass-ratio Contact Binary Systems in TESS Survey
Low-mass-ratio ( q ) contact binary systems are progenitors of stellar mergers such as blue stragglers or fast-rotating FK Com stars. In this study, we present the first light curve analysis of two newly identified low mass-ratio contact binary systems, TIC 55007847 and TIC 63597006, that are identi...
| Main Authors: | , , , , , , , , , , |
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| Format: | Article |
| Language: | English |
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IOP Publishing
2024-01-01
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| Series: | The Astronomical Journal |
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| Online Access: | https://doi.org/10.3847/1538-3881/ad2760 |
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| author | Qiyuan Cheng Jianping Xiong Xu Ding Kaifan Ji Jiao Li Chao Liu Jiangdan Li Jingxiao Luo Xin Lyu Zhanwen Han Xuefei Chen |
| author_facet | Qiyuan Cheng Jianping Xiong Xu Ding Kaifan Ji Jiao Li Chao Liu Jiangdan Li Jingxiao Luo Xin Lyu Zhanwen Han Xuefei Chen |
| author_sort | Qiyuan Cheng |
| collection | DOAJ |
| description | Low-mass-ratio ( q ) contact binary systems are progenitors of stellar mergers such as blue stragglers or fast-rotating FK Com stars. In this study, we present the first light curve analysis of two newly identified low mass-ratio contact binary systems, TIC 55007847 and TIC 63597006, that are identified from TESS. Both stars are classified as A-subtype contact binaries. We obtained the precise orbit periods for the two objects by using the O − C method, i.e., P = 0.6117108 day for TIC 55007847 and P = 0.7008995 day for TIC 63597006, and found an obvious periodic signal in the O − C curve of TIC 63597006. We suggest that the periodic signal comes from a third body. We further use the Markov chain Monte Carlo method with PHOEBE to derive the photometric solutions for the two binaries. The photometric solution for this object shows that the contribution of the third body is about 6%. Our analysis revealed that TIC 55007847 has an extremely low mass ratio of q = 0.08. By calculating the ratio of spin angular momentum to the orbital angular momentum J _s / J _o , we found that TIC 55007847 is very close to the instability threshold with J _s / J _o = 0.31, indicating that it may merge into a single, fast-rotating star in the future. For TIC 63597006, q = 0.14 and J _s / J _o = 0.15. This object is in a relatively stable evolutionary status at present. |
| first_indexed | 2024-04-25T02:02:42Z |
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| issn | 1538-3881 |
| language | English |
| last_indexed | 2024-04-25T02:02:42Z |
| publishDate | 2024-01-01 |
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| record_format | Article |
| series | The Astronomical Journal |
| spelling | doaj.art-381ef076657c4a78ab2ab96fa74917cf2024-03-07T14:45:26ZengIOP PublishingThe Astronomical Journal1538-38812024-01-01167414810.3847/1538-3881/ad2760The First Photometric Analysis of Two Low-mass-ratio Contact Binary Systems in TESS SurveyQiyuan Cheng0Jianping Xiong1https://orcid.org/0000-0003-4829-6245Xu Ding2https://orcid.org/0000-0002-2427-161XKaifan Ji3https://orcid.org/0000-0001-8950-3875Jiao Li4Chao Liu5https://orcid.org/0000-0002-1802-6917Jiangdan Li6https://orcid.org/0000-0003-3832-8864Jingxiao Luo7Xin Lyu8https://orcid.org/0000-0001-8550-0095Zhanwen Han9https://orcid.org/0000-0001-9204-7778Xuefei Chen10https://orcid.org/0000-0001-5284-8001Yunnan Observatories, Chinese Academy of Sciences , 396 YangFangWang, Guandu District, Kunming, 650216, People's Republic of China ; cxf@ynao.ac.cn; School of Astronomy and Space Science, University of Chinese Academy of Sciences , Beijing, 100049, People's Republic of ChinaYunnan Observatories, Chinese Academy of Sciences , 396 YangFangWang, Guandu District, Kunming, 650216, People's Republic of China ; cxf@ynao.ac.cn; Key Laboratory for Structure and Evolution of Celestial Objects , Chinese Academy of Sciences, P.O. Box 110, Kunming 650216, People's Republic of China; International Centre of Supernovae , Yunnan Key Laboratory, Kunming 650216, People's Republic of ChinaYunnan Observatories, Chinese Academy of Sciences , 396 YangFangWang, Guandu District, Kunming, 650216, People's Republic of China ; cxf@ynao.ac.cnYunnan Observatories, Chinese Academy of Sciences , 396 YangFangWang, Guandu District, Kunming, 650216, People's Republic of China ; cxf@ynao.ac.cnKey Laboratory of Space Astronomy and Technology , National Astronomical Observatories, CAS, Beijing 100101, People's Republic of ChinaSchool of Astronomy and Space Science, University of Chinese Academy of Sciences , Beijing, 100049, People's Republic of China; Key Laboratory of Space Astronomy and Technology , National Astronomical Observatories, CAS, Beijing 100101, People's Republic of China; Institute for Frontiers in Astronomy and Astrophysics, Beijing Normal University , Beijing, 102206, People's Republic of ChinaYunnan Observatories, Chinese Academy of Sciences , 396 YangFangWang, Guandu District, Kunming, 650216, People's Republic of China ; cxf@ynao.ac.cnYunnan Observatories, Chinese Academy of Sciences , 396 YangFangWang, Guandu District, Kunming, 650216, People's Republic of China ; cxf@ynao.ac.cn; School of Astronomy and Space Science, University of Chinese Academy of Sciences , Beijing, 100049, People's Republic of ChinaSchool of Astronomy and Space Science, University of Chinese Academy of Sciences , Beijing, 100049, People's Republic of China; National Astronomical Observatories , Chinese Academy of Sciences, Beijing 100101, People's Republic of China; Key Laboratory of Radio Astronomy and Technolgoy , Chinese Academy of Sciences, A20 Datun Road, Chaoyang District, Beijing, 100101, People's Republic of ChinaYunnan Observatories, Chinese Academy of Sciences , 396 YangFangWang, Guandu District, Kunming, 650216, People's Republic of China ; cxf@ynao.ac.cn; Key Laboratory for Structure and Evolution of Celestial Objects , Chinese Academy of Sciences, P.O. Box 110, Kunming 650216, People's Republic of China; International Centre of Supernovae , Yunnan Key Laboratory, Kunming 650216, People's Republic of ChinaYunnan Observatories, Chinese Academy of Sciences , 396 YangFangWang, Guandu District, Kunming, 650216, People's Republic of China ; cxf@ynao.ac.cn; Key Laboratory for Structure and Evolution of Celestial Objects , Chinese Academy of Sciences, P.O. Box 110, Kunming 650216, People's Republic of China; International Centre of Supernovae , Yunnan Key Laboratory, Kunming 650216, People's Republic of ChinaLow-mass-ratio ( q ) contact binary systems are progenitors of stellar mergers such as blue stragglers or fast-rotating FK Com stars. In this study, we present the first light curve analysis of two newly identified low mass-ratio contact binary systems, TIC 55007847 and TIC 63597006, that are identified from TESS. Both stars are classified as A-subtype contact binaries. We obtained the precise orbit periods for the two objects by using the O − C method, i.e., P = 0.6117108 day for TIC 55007847 and P = 0.7008995 day for TIC 63597006, and found an obvious periodic signal in the O − C curve of TIC 63597006. We suggest that the periodic signal comes from a third body. We further use the Markov chain Monte Carlo method with PHOEBE to derive the photometric solutions for the two binaries. The photometric solution for this object shows that the contribution of the third body is about 6%. Our analysis revealed that TIC 55007847 has an extremely low mass ratio of q = 0.08. By calculating the ratio of spin angular momentum to the orbital angular momentum J _s / J _o , we found that TIC 55007847 is very close to the instability threshold with J _s / J _o = 0.31, indicating that it may merge into a single, fast-rotating star in the future. For TIC 63597006, q = 0.14 and J _s / J _o = 0.15. This object is in a relatively stable evolutionary status at present.https://doi.org/10.3847/1538-3881/ad2760Interacting binary starsContact binary starsStellar evolutionFundamental parameters of stars |
| spellingShingle | Qiyuan Cheng Jianping Xiong Xu Ding Kaifan Ji Jiao Li Chao Liu Jiangdan Li Jingxiao Luo Xin Lyu Zhanwen Han Xuefei Chen The First Photometric Analysis of Two Low-mass-ratio Contact Binary Systems in TESS Survey The Astronomical Journal Interacting binary stars Contact binary stars Stellar evolution Fundamental parameters of stars |
| title | The First Photometric Analysis of Two Low-mass-ratio Contact Binary Systems in TESS Survey |
| title_full | The First Photometric Analysis of Two Low-mass-ratio Contact Binary Systems in TESS Survey |
| title_fullStr | The First Photometric Analysis of Two Low-mass-ratio Contact Binary Systems in TESS Survey |
| title_full_unstemmed | The First Photometric Analysis of Two Low-mass-ratio Contact Binary Systems in TESS Survey |
| title_short | The First Photometric Analysis of Two Low-mass-ratio Contact Binary Systems in TESS Survey |
| title_sort | first photometric analysis of two low mass ratio contact binary systems in tess survey |
| topic | Interacting binary stars Contact binary stars Stellar evolution Fundamental parameters of stars |
| url | https://doi.org/10.3847/1538-3881/ad2760 |
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