Variability of Magnetic Hot Stars from the TESS Observations
Magnetic hot stars refer to stars that have effective temperatures approximately in the range from 7000–50,000 K, and with large-scale globally organized magnetic fields. These magnetic fields exhibit strengths ranging from tens of Gauss to tens of kilo-Gauss. They are key in understanding the effec...
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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/acf197 |
| _version_ | 1827806184819654656 |
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| author | Dong-Xiang Shen Gang Li Iskandar Abdusamatjan Jian-Ning Fu Chun-Hua Zhu Jin-Long Yu Yu Zhang Guo-Liang Lü Nan-Nan Zhai Jin-Zhong Liu |
| author_facet | Dong-Xiang Shen Gang Li Iskandar Abdusamatjan Jian-Ning Fu Chun-Hua Zhu Jin-Long Yu Yu Zhang Guo-Liang Lü Nan-Nan Zhai Jin-Zhong Liu |
| author_sort | Dong-Xiang Shen |
| collection | DOAJ |
| description | Magnetic hot stars refer to stars that have effective temperatures approximately in the range from 7000–50,000 K, and with large-scale globally organized magnetic fields. These magnetic fields exhibit strengths ranging from tens of Gauss to tens of kilo-Gauss. They are key in understanding the effects caused by magnetic fields in the stellar evolution. However, there are only three magnetic hot stars studied via a combination of spectropolarimetric and asteroseismic modeling. Combined with Transiting Exoplanet Survey Satellite sectors 1–56 data sets, we provided a photometric variability and stochastic low-frequency (SLF) variability study of 118 magnetic hot stars. Nine new rotating variable stars are identified. Using the Bayesian Markov Chain Monte Carlo framework, we fitted the morphologies of SLF variability for magnetic hot stars. Our analysis reveals that the magnetic hot stars in our sample have γ < 5.5 with the vast majority having 1 ≤ γ ≤ 3. The ν _char is primarily in the ranges of 0 day ^−1 < ν _char < 6.3 day ^−1 . The amplitude of SLF variability, log α _0 , shows a dominant distribution ranging from 0.8–3. No significant correlations are observed between the luminosity and fitting parameters, suggesting no clear dependence of SLF variability on stellar mass for our sample of magnetic hot stars with masses between approximately 1.5 M _⊙ < M < 20 M _⊙ . We found a significant negative correlation between the B _p and ν _char . This suppression effect of magnetic fields on ν _char may be a result of their inhibition of macroturbulence. |
| first_indexed | 2024-03-11T21:37:33Z |
| format | Article |
| id | doaj.art-32584fd9f22440e9b133610ddeaa7d56 |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-11T21:37:33Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-32584fd9f22440e9b133610ddeaa7d562023-09-26T17:14:14ZengIOP PublishingThe Astrophysical Journal1538-43572023-01-01955212310.3847/1538-4357/acf197Variability of Magnetic Hot Stars from the TESS ObservationsDong-Xiang Shen0https://orcid.org/0000-0002-1926-8248Gang Li1https://orcid.org/0000-0001-9313-251XIskandar Abdusamatjan2Jian-Ning Fu3https://orcid.org/0000-0001-8241-1740Chun-Hua Zhu4Jin-Long Yu5Yu Zhang6https://orcid.org/0000-0001-7134-2874Guo-Liang Lü7Nan-Nan Zhai8https://orcid.org/0009-0008-3490-7934Jin-Zhong Liu9https://orcid.org/0000-0002-7420-6744School of Physical Science and Technology, Xinjiang University , Urumqi 830046, People’s Republic of China ; shendongxiang@stu.xju.edu.cn chunhuazhu@sina.cnInstitute of Astronomy, KU Leuven , Celestijnenlaan 200D, B-3001 Leuven, BelgiumXinjiang Astronomical Observatory, National Astronomical Observatories, Chinese Academy of Sciences , Urumqi 830000, People's Republic of China liujinzh@xao.ac.cn; School of Astronomy and Space Science, University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of ChinaDepartment of Astronomy, Beijing Normal University , Beijing, 100871, People’s Republic of ChinaSchool of Physical Science and Technology, Xinjiang University , Urumqi 830046, People’s Republic of China ; shendongxiang@stu.xju.edu.cn chunhuazhu@sina.cnCollege of Mechanical and Electronic Engineering, Tarim University , 843300, Alar, People’s Republic of ChinaXinjiang Astronomical Observatory, National Astronomical Observatories, Chinese Academy of Sciences , Urumqi 830000, People's Republic of China liujinzh@xao.ac.cnXinjiang Astronomical Observatory, National Astronomical Observatories, Chinese Academy of Sciences , Urumqi 830000, People's Republic of China liujinzh@xao.ac.cnXinjiang Astronomical Observatory, National Astronomical Observatories, Chinese Academy of Sciences , Urumqi 830000, People's Republic of China liujinzh@xao.ac.cnXinjiang Astronomical Observatory, National Astronomical Observatories, Chinese Academy of Sciences , Urumqi 830000, People's Republic of China liujinzh@xao.ac.cnMagnetic hot stars refer to stars that have effective temperatures approximately in the range from 7000–50,000 K, and with large-scale globally organized magnetic fields. These magnetic fields exhibit strengths ranging from tens of Gauss to tens of kilo-Gauss. They are key in understanding the effects caused by magnetic fields in the stellar evolution. However, there are only three magnetic hot stars studied via a combination of spectropolarimetric and asteroseismic modeling. Combined with Transiting Exoplanet Survey Satellite sectors 1–56 data sets, we provided a photometric variability and stochastic low-frequency (SLF) variability study of 118 magnetic hot stars. Nine new rotating variable stars are identified. Using the Bayesian Markov Chain Monte Carlo framework, we fitted the morphologies of SLF variability for magnetic hot stars. Our analysis reveals that the magnetic hot stars in our sample have γ < 5.5 with the vast majority having 1 ≤ γ ≤ 3. The ν _char is primarily in the ranges of 0 day ^−1 < ν _char < 6.3 day ^−1 . The amplitude of SLF variability, log α _0 , shows a dominant distribution ranging from 0.8–3. No significant correlations are observed between the luminosity and fitting parameters, suggesting no clear dependence of SLF variability on stellar mass for our sample of magnetic hot stars with masses between approximately 1.5 M _⊙ < M < 20 M _⊙ . We found a significant negative correlation between the B _p and ν _char . This suppression effect of magnetic fields on ν _char may be a result of their inhibition of macroturbulence.https://doi.org/10.3847/1538-4357/acf197Magnetic fieldsEarly-type variable starsEarly-type starsAsteroseismology |
| spellingShingle | Dong-Xiang Shen Gang Li Iskandar Abdusamatjan Jian-Ning Fu Chun-Hua Zhu Jin-Long Yu Yu Zhang Guo-Liang Lü Nan-Nan Zhai Jin-Zhong Liu Variability of Magnetic Hot Stars from the TESS Observations The Astrophysical Journal Magnetic fields Early-type variable stars Early-type stars Asteroseismology |
| title | Variability of Magnetic Hot Stars from the TESS Observations |
| title_full | Variability of Magnetic Hot Stars from the TESS Observations |
| title_fullStr | Variability of Magnetic Hot Stars from the TESS Observations |
| title_full_unstemmed | Variability of Magnetic Hot Stars from the TESS Observations |
| title_short | Variability of Magnetic Hot Stars from the TESS Observations |
| title_sort | variability of magnetic hot stars from the tess observations |
| topic | Magnetic fields Early-type variable stars Early-type stars Asteroseismology |
| url | https://doi.org/10.3847/1538-4357/acf197 |
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