Observational Properties of 155 β Cephei Pulsating Variable Stars
β Cephei pulsating variable (BCEP) stars are the most massive pulsating variable stars in the main sequence, exhibiting both p - and g -mode pulsations. In this study, we identified 155 BCEP stars or candidates using data from TESS and Gaia, of which 83 were first confirmed as BCEP stars. They have...
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IOP Publishing
2024-01-01
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| Series: | The Astrophysical Journal Supplement Series |
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| Online Access: | https://doi.org/10.3847/1538-4365/ad1f66 |
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| author | Xiang-dong Shi Sheng-bang Qian Li-ying Zhu Lin-jia Li Er-gang Zhao Wen-xu Lin |
| author_facet | Xiang-dong Shi Sheng-bang Qian Li-ying Zhu Lin-jia Li Er-gang Zhao Wen-xu Lin |
| author_sort | Xiang-dong Shi |
| collection | DOAJ |
| description | β Cephei pulsating variable (BCEP) stars are the most massive pulsating variable stars in the main sequence, exhibiting both p - and g -mode pulsations. In this study, we identified 155 BCEP stars or candidates using data from TESS and Gaia, of which 83 were first confirmed as BCEP stars. They have visual magnitudes ranging from 8 to 12 mag and effective temperatures between approximately 20,000 and 30,000 K, while the parallaxes of most targets are between 0.2 and 0.6 mas. The study indicates that these BCEP stars have pulsation periods ranging from 0.06 to 0.31 days, with amplitudes ranging from 0.1 to 55.8 mmag in the TESS band. Additionally, the number of BCEP stars increases as the pulsation amplitude decreases. These targets align with the distribution region of BCEP stars in the luminosity–period ( L – P ) and temperature–period diagrams. We have updated the L – P relation of BCEP stars. The Hertzsprung–Russell diagram indicates that these targets are in the main-sequence evolutionary phase, with masses ranging from 7 to 20 M _⊙ and luminosities between 2800 and 71,000 L _⊙ . They are almost in the theoretical instability region of BCEP stars but as previously reported, this region at the low-mass end (red) is not filled. The distribution of the pulsation constant indicates that the dominant pulsation periods of BCEP stars consist mainly of low-order p -mode pulsations with a high proportion of radial fundamental modes. These BCEP stars are excellent objects for enhancing our understanding of the structure and evolution of massive stars through asteroseismology. |
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| publishDate | 2024-01-01 |
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| series | The Astrophysical Journal Supplement Series |
| spelling | doaj.art-30c336cdebdd4e2f94e6cf47e73bbe2e2024-03-01T09:47:49ZengIOP PublishingThe Astrophysical Journal Supplement Series0067-00492024-01-0127112810.3847/1538-4365/ad1f66Observational Properties of 155 β Cephei Pulsating Variable StarsXiang-dong Shi0https://orcid.org/0000-0002-5038-5952Sheng-bang Qian1Li-ying Zhu2Lin-jia Li3Er-gang Zhao4Wen-xu Lin5Yunnan Observatories, Chinese Academy of Sciences (CAS) , P.O. Box 110, Kunming 650216, People's Republic of China ; sxd@ynao.ac.cn; Department of Astronomy, Key Laboratory of Astroparticle Physics of Yunnan Province, Yunnan University , Kunming 650091, People's Republic of China; University of Chinese Academy of Sciences , No. 1 Yanqihu East Rd., Huairou District, Beijing 101408, People's Republic of China; Key Laboratory of the Structure and Evolution of Celestial Objects , CAS, Kunming 650216, People's Republic of ChinaDepartment of Astronomy, Key Laboratory of Astroparticle Physics of Yunnan Province, Yunnan University , Kunming 650091, People's Republic of China; University of Chinese Academy of Sciences , No. 1 Yanqihu East Rd., Huairou District, Beijing 101408, People's Republic of China; Key Laboratory of the Structure and Evolution of Celestial Objects , CAS, Kunming 650216, People's Republic of ChinaYunnan Observatories, Chinese Academy of Sciences (CAS) , P.O. Box 110, Kunming 650216, People's Republic of China ; sxd@ynao.ac.cn; University of Chinese Academy of Sciences , No. 1 Yanqihu East Rd., Huairou District, Beijing 101408, People's Republic of China; Key Laboratory of the Structure and Evolution of Celestial Objects , CAS, Kunming 650216, People's Republic of ChinaYunnan Observatories, Chinese Academy of Sciences (CAS) , P.O. Box 110, Kunming 650216, People's Republic of China ; sxd@ynao.ac.cn; University of Chinese Academy of Sciences , No. 1 Yanqihu East Rd., Huairou District, Beijing 101408, People's Republic of China; Key Laboratory of the Structure and Evolution of Celestial Objects , CAS, Kunming 650216, People's Republic of ChinaYunnan Observatories, Chinese Academy of Sciences (CAS) , P.O. Box 110, Kunming 650216, People's Republic of China ; sxd@ynao.ac.cn; University of Chinese Academy of Sciences , No. 1 Yanqihu East Rd., Huairou District, Beijing 101408, People's Republic of China; Key Laboratory of the Structure and Evolution of Celestial Objects , CAS, Kunming 650216, People's Republic of ChinaYunnan Observatories, Chinese Academy of Sciences (CAS) , P.O. Box 110, Kunming 650216, People's Republic of China ; sxd@ynao.ac.cn; University of Chinese Academy of Sciences , No. 1 Yanqihu East Rd., Huairou District, Beijing 101408, People's Republic of China; Key Laboratory of the Structure and Evolution of Celestial Objects , CAS, Kunming 650216, People's Republic of Chinaβ Cephei pulsating variable (BCEP) stars are the most massive pulsating variable stars in the main sequence, exhibiting both p - and g -mode pulsations. In this study, we identified 155 BCEP stars or candidates using data from TESS and Gaia, of which 83 were first confirmed as BCEP stars. They have visual magnitudes ranging from 8 to 12 mag and effective temperatures between approximately 20,000 and 30,000 K, while the parallaxes of most targets are between 0.2 and 0.6 mas. The study indicates that these BCEP stars have pulsation periods ranging from 0.06 to 0.31 days, with amplitudes ranging from 0.1 to 55.8 mmag in the TESS band. Additionally, the number of BCEP stars increases as the pulsation amplitude decreases. These targets align with the distribution region of BCEP stars in the luminosity–period ( L – P ) and temperature–period diagrams. We have updated the L – P relation of BCEP stars. The Hertzsprung–Russell diagram indicates that these targets are in the main-sequence evolutionary phase, with masses ranging from 7 to 20 M _⊙ and luminosities between 2800 and 71,000 L _⊙ . They are almost in the theoretical instability region of BCEP stars but as previously reported, this region at the low-mass end (red) is not filled. The distribution of the pulsation constant indicates that the dominant pulsation periods of BCEP stars consist mainly of low-order p -mode pulsations with a high proportion of radial fundamental modes. These BCEP stars are excellent objects for enhancing our understanding of the structure and evolution of massive stars through asteroseismology.https://doi.org/10.3847/1538-4365/ad1f66Massive starsPulsating variable stars |
| spellingShingle | Xiang-dong Shi Sheng-bang Qian Li-ying Zhu Lin-jia Li Er-gang Zhao Wen-xu Lin Observational Properties of 155 β Cephei Pulsating Variable Stars The Astrophysical Journal Supplement Series Massive stars Pulsating variable stars |
| title | Observational Properties of 155 β Cephei Pulsating Variable Stars |
| title_full | Observational Properties of 155 β Cephei Pulsating Variable Stars |
| title_fullStr | Observational Properties of 155 β Cephei Pulsating Variable Stars |
| title_full_unstemmed | Observational Properties of 155 β Cephei Pulsating Variable Stars |
| title_short | Observational Properties of 155 β Cephei Pulsating Variable Stars |
| title_sort | observational properties of 155 β cephei pulsating variable stars |
| topic | Massive stars Pulsating variable stars |
| url | https://doi.org/10.3847/1538-4365/ad1f66 |
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