Asteroseismology of 687 TESS Red Giants: Individual Frequencies and Asymptotic Parameters
The individual modes and asymptotic parameters are important characteristics of stellar oscillation. Using TESS 2 minute cadence data from Sectors 1 to 75, we perform asteroseismic analysis of 687 red giants, and provide their oscillation mode parameters. The mode parameters, including frequencies ν...
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2025-01-01
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| Online Access: | https://doi.org/10.3847/1538-4365/adde57 |
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| author | Jianzhao Zhou Shaolan Bi Yaguang Li Jie Yu Tanda Li Xianfei Zhang Lifei Ye Mengjie Li Liu Long Tiancheng Sun Yuqin Chen |
| author_facet | Jianzhao Zhou Shaolan Bi Yaguang Li Jie Yu Tanda Li Xianfei Zhang Lifei Ye Mengjie Li Liu Long Tiancheng Sun Yuqin Chen |
| author_sort | Jianzhao Zhou |
| collection | DOAJ |
| description | The individual modes and asymptotic parameters are important characteristics of stellar oscillation. Using TESS 2 minute cadence data from Sectors 1 to 75, we perform asteroseismic analysis of 687 red giants, and provide their oscillation mode parameters. The mode parameters, including frequencies ν _n _, _l , amplitudes A _n _, _l , and line widths Γ _n _, _l , are obtained through Markov Chain Monte Carlo fitting. The median uncertainty for frequency is 0.047 μ Hz. Using the radial mode frequencies, we calculate the values of Δ ν , and derive asymptotic parameters ( ϵ _p , ϵ _c , δν _0 _l , q , and ΔΠ _1 ) based on l = 0, 1, 2 modes. For red giants with Δ ν > 15.6 μ Hz, there is a weaker correlation between δν _02 and Δ ν , and a stronger mass dependence, compared to stars with lower Δ ν . Additionally, the ratio δν _02 /Δ ν presents a pronounced increase with Δ ν decrease, as these stars undergo rapid core contraction and their convective envelopes extend deep into the interior. At this stage, the ratio δν _02 /Δ ν may serve as a robust indicator for diagnosing the location of the convective boundary. Furthermore, the ϵ _c values can be a potential index to distinguish red clump (RC) and secondary RC stars from red giant branch stars in the TESS field. |
| format | Article |
| id | doaj-art-76f543cd9d3746a6b4754cbf78471b01 |
| institution | DOAJ |
| issn | 0067-0049 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
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| series | The Astrophysical Journal Supplement Series |
| spelling | doaj-art-76f543cd9d3746a6b4754cbf78471b012025-08-20T03:12:50ZengIOP PublishingThe Astrophysical Journal Supplement Series0067-00492025-01-0127923710.3847/1538-4365/adde57Asteroseismology of 687 TESS Red Giants: Individual Frequencies and Asymptotic ParametersJianzhao Zhou0https://orcid.org/0009-0004-9024-9666Shaolan Bi1https://orcid.org/0000-0002-7642-7583Yaguang Li2https://orcid.org/0000-0003-3020-4437Jie Yu3https://orcid.org/0000-0002-0007-6211Tanda Li4https://orcid.org/0000-0001-6396-2563Xianfei Zhang5https://orcid.org/0000-0002-3672-2166Lifei Ye6https://orcid.org/0009-0009-1338-1045Mengjie Li7Liu Long8https://orcid.org/0000-0003-2908-1492Tiancheng Sun9https://orcid.org/0000-0003-0795-4854Yuqin Chen10https://orcid.org/0000-0002-8442-901XInstitute for Frontiers in Astronomy and Astrophysics, Beijing Normal University , Beijing 102206, People’s Republic of China ; bisl@bnu.edu.cn; School of Physics and Astronomy, Beijing Normal University , Beijing 100875, People’s Republic of ChinaInstitute for Frontiers in Astronomy and Astrophysics, Beijing Normal University , Beijing 102206, People’s Republic of China ; bisl@bnu.edu.cn; School of Physics and Astronomy, Beijing Normal University , Beijing 100875, People’s Republic of ChinaInstitute for Astronomy, University of Hawai‘i , 2680 Woodlawn Drive, Honolulu, HI 96822, USASchool of Astronomy and Space Science, Nanjing University , Nanjing 210023, People's Republic of China; Key Laboratory of Modern Astronomy and Astrophysics, Ministry of Education, Nanjing 210023, People's Republic of China; Research School of Astronomy & Astrophysics, Australian National University , Cotter Road, Weston, ACT 2611, AustraliaInstitute for Frontiers in Astronomy and Astrophysics, Beijing Normal University , Beijing 102206, People’s Republic of China ; bisl@bnu.edu.cn; School of Physics and Astronomy, Beijing Normal University , Beijing 100875, People’s Republic of ChinaInstitute for Frontiers in Astronomy and Astrophysics, Beijing Normal University , Beijing 102206, People’s Republic of China ; bisl@bnu.edu.cn; School of Physics and Astronomy, Beijing Normal University , Beijing 100875, People’s Republic of ChinaInstitute for Frontiers in Astronomy and Astrophysics, Beijing Normal University , Beijing 102206, People’s Republic of China ; bisl@bnu.edu.cn; School of Physics and Astronomy, Beijing Normal University , Beijing 100875, People’s Republic of ChinaInstitute for Frontiers in Astronomy and Astrophysics, Beijing Normal University , Beijing 102206, People’s Republic of China ; bisl@bnu.edu.cn; School of Physics and Astronomy, Beijing Normal University , Beijing 100875, People’s Republic of ChinaDepartment of Physics, Xiangtan University , Xiangtan 411105, Hunan Province, People’s Republic of ChinaCAS Key Laboratory of Optical Astronomy, National Astronomical Observatories , Chinese Academy of Sciences, Beijing 100101, People’s Republic of ChinaInstitute for Frontiers in Astronomy and Astrophysics, Beijing Normal University , Beijing 102206, People’s Republic of China ; bisl@bnu.edu.cn; CAS Key Laboratory of Optical Astronomy, National Astronomical Observatories , Chinese Academy of Sciences, Beijing 100101, People’s Republic of ChinaThe individual modes and asymptotic parameters are important characteristics of stellar oscillation. Using TESS 2 minute cadence data from Sectors 1 to 75, we perform asteroseismic analysis of 687 red giants, and provide their oscillation mode parameters. The mode parameters, including frequencies ν _n _, _l , amplitudes A _n _, _l , and line widths Γ _n _, _l , are obtained through Markov Chain Monte Carlo fitting. The median uncertainty for frequency is 0.047 μ Hz. Using the radial mode frequencies, we calculate the values of Δ ν , and derive asymptotic parameters ( ϵ _p , ϵ _c , δν _0 _l , q , and ΔΠ _1 ) based on l = 0, 1, 2 modes. For red giants with Δ ν > 15.6 μ Hz, there is a weaker correlation between δν _02 and Δ ν , and a stronger mass dependence, compared to stars with lower Δ ν . Additionally, the ratio δν _02 /Δ ν presents a pronounced increase with Δ ν decrease, as these stars undergo rapid core contraction and their convective envelopes extend deep into the interior. At this stage, the ratio δν _02 /Δ ν may serve as a robust indicator for diagnosing the location of the convective boundary. Furthermore, the ϵ _c values can be a potential index to distinguish red clump (RC) and secondary RC stars from red giant branch stars in the TESS field.https://doi.org/10.3847/1538-4365/adde57AsteroseismologyGiant starsLow mass stars |
| spellingShingle | Jianzhao Zhou Shaolan Bi Yaguang Li Jie Yu Tanda Li Xianfei Zhang Lifei Ye Mengjie Li Liu Long Tiancheng Sun Yuqin Chen Asteroseismology of 687 TESS Red Giants: Individual Frequencies and Asymptotic Parameters The Astrophysical Journal Supplement Series Asteroseismology Giant stars Low mass stars |
| title | Asteroseismology of 687 TESS Red Giants: Individual Frequencies and Asymptotic Parameters |
| title_full | Asteroseismology of 687 TESS Red Giants: Individual Frequencies and Asymptotic Parameters |
| title_fullStr | Asteroseismology of 687 TESS Red Giants: Individual Frequencies and Asymptotic Parameters |
| title_full_unstemmed | Asteroseismology of 687 TESS Red Giants: Individual Frequencies and Asymptotic Parameters |
| title_short | Asteroseismology of 687 TESS Red Giants: Individual Frequencies and Asymptotic Parameters |
| title_sort | asteroseismology of 687 tess red giants individual frequencies and asymptotic parameters |
| topic | Asteroseismology Giant stars Low mass stars |
| url | https://doi.org/10.3847/1538-4365/adde57 |
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