Minute-cadence Observations of the LAMOST Fields with the TMTS. VI. Physical Parameters of Contact Binaries
With the development of wide-field surveys, a large amount of data on short-period W UMa contact binaries have been obtained. Continuous and uninterrupted light curves as well as high-resolution spectroscopic data are crucial in determining the absolute physical parameters. Targets with both TMTS li...
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IOP Publishing
2025-01-01
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| Series: | The Astronomical Journal |
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| Online Access: | https://doi.org/10.3847/1538-3881/ada7eb |
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| author | Qiqi Xia Xiaofeng Wang Kai Li Xiang Gao Fangzhou Guo Jie Lin Cheng Liu Jun Mo Haowei Peng Qichun Liu Gaobo Xi Shengyu Yan Xiaojun Jiang Jicheng Zhang Cui-Ying Song Jianrong Shi Xiaoran Ma Danfeng Xiang Wenxiong Li |
| author_facet | Qiqi Xia Xiaofeng Wang Kai Li Xiang Gao Fangzhou Guo Jie Lin Cheng Liu Jun Mo Haowei Peng Qichun Liu Gaobo Xi Shengyu Yan Xiaojun Jiang Jicheng Zhang Cui-Ying Song Jianrong Shi Xiaoran Ma Danfeng Xiang Wenxiong Li |
| author_sort | Qiqi Xia |
| collection | DOAJ |
| description | With the development of wide-field surveys, a large amount of data on short-period W UMa contact binaries have been obtained. Continuous and uninterrupted light curves as well as high-resolution spectroscopic data are crucial in determining the absolute physical parameters. Targets with both TMTS light curves and LAMOST medium-resolution spectra were selected. The absolute physical parameters were inferred with the W-D code for 10 systems, all of them are W-type shallow or medium contact binaries. The O'Connell effect observed in the light curves can be explained by adding a spot on the primary or secondary component in the models. According to O − C analysis, the orbital periods exhibit a long-term increasing or decreasing trend, among which J0132, J1300, and J1402 show periodic variations that may be attributed to the presence of a third body or magnetic activity cycles. Spectral subtraction analysis revealed that the equivalent width of H α indicates strong magnetic activity in J0047, J0305, J0638, and J1402. Among the 10 selected binary systems, except for J0132 and J0913, the more massive components are found to be main-sequence stars while the less massive components have evolved off the main sequence. In J0132, both components are in the main sequence, whereas both components of J0913 lie above the terminal-age main sequence. Based on the relationship between orbital angular momentum and total mass for these two systems, as well as their low fill-out factors, it is possible that these two systems are newly formed contact binaries, having recently evolved from the detached configuration. |
| format | Article |
| id | doaj-art-5fd9802fb4ec43acbaffbddc5dd4ff4a |
| institution | Kabale University |
| issn | 1538-3881 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
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| series | The Astronomical Journal |
| spelling | doaj-art-5fd9802fb4ec43acbaffbddc5dd4ff4a2025-02-12T07:05:32ZengIOP PublishingThe Astronomical Journal1538-38812025-01-01169313910.3847/1538-3881/ada7ebMinute-cadence Observations of the LAMOST Fields with the TMTS. VI. Physical Parameters of Contact BinariesQiqi Xia0https://orcid.org/0009-0000-5672-5789Xiaofeng Wang1https://orcid.org/0000-0002-7334-2357Kai Li2https://orcid.org/0000-0003-3590-335XXiang Gao3https://orcid.org/0009-0009-6364-0391Fangzhou Guo4Jie Lin5Cheng Liu6Jun Mo7Haowei Peng8Qichun Liu9Gaobo Xi10Shengyu Yan11https://orcid.org/0009-0004-4256-1209Xiaojun Jiang12Jicheng Zhang13Cui-Ying Song14Jianrong Shi15https://orcid.org/0000-0002-0349-7839Xiaoran Ma16Danfeng Xiang17Wenxiong Li18https://orcid.org/0000-0002-0096-3523Physics Department and Tsinghua Center for Astrophysics, Tsinghua University , Beijing 100084, People’s Republic of China ; wang_xf@mail.tsinghua.edu.cnPhysics Department and Tsinghua Center for Astrophysics, Tsinghua University , Beijing 100084, People’s Republic of China ; wang_xf@mail.tsinghua.edu.cnShandong Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, School of Space Science and Physics, Institute of Space Sciences, Shandong University , Weihai, Shandong 264209, People’s Republic of ChinaShandong Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, School of Space Science and Physics, Institute of Space Sciences, Shandong University , Weihai, Shandong 264209, People’s Republic of ChinaPhysics Department and Tsinghua Center for Astrophysics, Tsinghua University , Beijing 100084, People’s Republic of China ; wang_xf@mail.tsinghua.edu.cnDepartment of Astronomy, University of Science and Technology of China , Hefei 230026, People’s Republic of China; School of Astronomy and Space Science, University of Science and Technology of China , Hefei 230026, People’s Republic of ChinaBeijing Planetarium, Beijing Academy of Sciences and Technology , Beijing 100044, People’s Republic of ChinaPhysics Department and Tsinghua Center for Astrophysics, Tsinghua University , Beijing 100084, People’s Republic of China ; wang_xf@mail.tsinghua.edu.cnPhysics Department and Tsinghua Center for Astrophysics, Tsinghua University , Beijing 100084, People’s Republic of China ; wang_xf@mail.tsinghua.edu.cnPhysics Department and Tsinghua Center for Astrophysics, Tsinghua University , Beijing 100084, People’s Republic of China ; wang_xf@mail.tsinghua.edu.cnPhysics Department and Tsinghua Center for Astrophysics, Tsinghua University , Beijing 100084, People’s Republic of China ; wang_xf@mail.tsinghua.edu.cnPhysics Department and Tsinghua Center for Astrophysics, Tsinghua University , Beijing 100084, People’s Republic of China ; wang_xf@mail.tsinghua.edu.cnNational Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, People’s Republic of ChinaSchool of Physics and Astronomy, Beijing Normal University , Beijing 100875, People’s Republic of ChinaPhysics Department and Tsinghua Center for Astrophysics, Tsinghua University , Beijing 100084, People’s Republic of China ; wang_xf@mail.tsinghua.edu.cnNational Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, People’s Republic of ChinaPhysics Department and Tsinghua Center for Astrophysics, Tsinghua University , Beijing 100084, People’s Republic of China ; wang_xf@mail.tsinghua.edu.cnPhysics Department and Tsinghua Center for Astrophysics, Tsinghua University , Beijing 100084, People’s Republic of China ; wang_xf@mail.tsinghua.edu.cn; Beijing Planetarium, Beijing Academy of Sciences and Technology , Beijing 100044, People’s Republic of ChinaNational Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, People’s Republic of ChinaWith the development of wide-field surveys, a large amount of data on short-period W UMa contact binaries have been obtained. Continuous and uninterrupted light curves as well as high-resolution spectroscopic data are crucial in determining the absolute physical parameters. Targets with both TMTS light curves and LAMOST medium-resolution spectra were selected. The absolute physical parameters were inferred with the W-D code for 10 systems, all of them are W-type shallow or medium contact binaries. The O'Connell effect observed in the light curves can be explained by adding a spot on the primary or secondary component in the models. According to O − C analysis, the orbital periods exhibit a long-term increasing or decreasing trend, among which J0132, J1300, and J1402 show periodic variations that may be attributed to the presence of a third body or magnetic activity cycles. Spectral subtraction analysis revealed that the equivalent width of H α indicates strong magnetic activity in J0047, J0305, J0638, and J1402. Among the 10 selected binary systems, except for J0132 and J0913, the more massive components are found to be main-sequence stars while the less massive components have evolved off the main sequence. In J0132, both components are in the main sequence, whereas both components of J0913 lie above the terminal-age main sequence. Based on the relationship between orbital angular momentum and total mass for these two systems, as well as their low fill-out factors, it is possible that these two systems are newly formed contact binaries, having recently evolved from the detached configuration.https://doi.org/10.3847/1538-3881/ada7ebContact binary starsClose binary starsStellar evolutionStar formationLate-type starsStarspots |
| spellingShingle | Qiqi Xia Xiaofeng Wang Kai Li Xiang Gao Fangzhou Guo Jie Lin Cheng Liu Jun Mo Haowei Peng Qichun Liu Gaobo Xi Shengyu Yan Xiaojun Jiang Jicheng Zhang Cui-Ying Song Jianrong Shi Xiaoran Ma Danfeng Xiang Wenxiong Li Minute-cadence Observations of the LAMOST Fields with the TMTS. VI. Physical Parameters of Contact Binaries The Astronomical Journal Contact binary stars Close binary stars Stellar evolution Star formation Late-type stars Starspots |
| title | Minute-cadence Observations of the LAMOST Fields with the TMTS. VI. Physical Parameters of Contact Binaries |
| title_full | Minute-cadence Observations of the LAMOST Fields with the TMTS. VI. Physical Parameters of Contact Binaries |
| title_fullStr | Minute-cadence Observations of the LAMOST Fields with the TMTS. VI. Physical Parameters of Contact Binaries |
| title_full_unstemmed | Minute-cadence Observations of the LAMOST Fields with the TMTS. VI. Physical Parameters of Contact Binaries |
| title_short | Minute-cadence Observations of the LAMOST Fields with the TMTS. VI. Physical Parameters of Contact Binaries |
| title_sort | minute cadence observations of the lamost fields with the tmts vi physical parameters of contact binaries |
| topic | Contact binary stars Close binary stars Stellar evolution Star formation Late-type stars Starspots |
| url | https://doi.org/10.3847/1538-3881/ada7eb |
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