Evidence of Stellar Oscillations in the Post-common-envelope Binary Candidate ASASSN-V J205543.90+240033.5
ASASSN-V J205543.90+240033.5 (ASJ2055) is a possible post-common-envelope binary system. Its optical photometric data show an orbital variation of about 0.52 days and a fast period modulation of P _0 ∼ 9.77 minutes, whose origin is unknown. In this Letter, we report evidence of the stellar oscillati...
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IOP Publishing
2023-01-01
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| Series: | The Astrophysical Journal Letters |
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| Online Access: | https://doi.org/10.3847/2041-8213/acec4c |
| _version_ | 1827825769897787392 |
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| author | J. Takata A. K. H. Kong X. F. Wang F. F. Song J. Mao X. Hou C.-P. Hu L. C.-C. Lin K. L. Li C. Y. Hui |
| author_facet | J. Takata A. K. H. Kong X. F. Wang F. F. Song J. Mao X. Hou C.-P. Hu L. C.-C. Lin K. L. Li C. Y. Hui |
| author_sort | J. Takata |
| collection | DOAJ |
| description | ASASSN-V J205543.90+240033.5 (ASJ2055) is a possible post-common-envelope binary system. Its optical photometric data show an orbital variation of about 0.52 days and a fast period modulation of P _0 ∼ 9.77 minutes, whose origin is unknown. In this Letter, we report evidence of the stellar oscillation of the companion star as the origin of the fast period modulation. We analyze the photometric data taken by the Transiting Exoplanet Survey Satellite, the Liverpool Telescope, and the Lulin One-meter Telescope. It is found that the period of the 9.77 minutes signal measured in 2022 August is significantly shorter than that in 2021 July/August, and the magnitude of the change is of the order of ∣△ P _0 ∣/ P _0 ∼ 0.0008(4). Such a large variation will be incompatible with the scenario of the white dwarf (WD) spin as the origin of the 9.77 minutes periodic modulation. We suggest that the fast periodic signal is related to the emission from the irradiated companion star rather than that of the WD. Using existing photometric data covering a wide wavelength range, we estimate that the hot WD in ASJ2055 has a temperature of T _eff ∼ 80,000 K and is heating the oscillating M-type main-sequence star with T _eff ∼ 3500 K on its unirradiated surface. The stellar oscillation of the M-type main-sequence star has been predicted in theoretical studies, but no observational confirmation has been done. ASJ2055, therefore, has the potential to be a unique laboratory for investigating the stellar oscillation of an M-type main-sequence star and the heating effect on stellar oscillation. |
| first_indexed | 2024-03-12T02:55:11Z |
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| institution | Directory Open Access Journal |
| issn | 2041-8205 |
| language | English |
| last_indexed | 2024-03-12T02:55:11Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
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| series | The Astrophysical Journal Letters |
| spelling | doaj.art-7a157d18bd5e446c908607e055f3fe382023-09-03T15:22:06ZengIOP PublishingThe Astrophysical Journal Letters2041-82052023-01-019532L1710.3847/2041-8213/acec4cEvidence of Stellar Oscillations in the Post-common-envelope Binary Candidate ASASSN-V J205543.90+240033.5J. Takata0https://orcid.org/0000-0002-8731-0129A. K. H. Kong1https://orcid.org/0000-0002-5105-344XX. F. Wang2F. F. Song3https://orcid.org/0009-0004-9835-353XJ. Mao4https://orcid.org/0000-0002-7077-7195X. Hou5C.-P. Hu6L. C.-C. Lin7https://orcid.org/0000-0003-4083-9567K. L. Li8https://orcid.org/0000-0001-8229-2024C. Y. Hui9https://orcid.org/0000-0003-1753-1660Department of Astronomy, School of Physics, Huazhong University of Science and Technology , Wuhan 430074, People’s Republic of China ; takata@hust.edu.cnInstitute of Astronomy, National Tsing Hua University , Hsinchu 30013, Taiwan ; akong@gapp.nthu.edu.twDepartment of Astronomy, School of Physics, Huazhong University of Science and Technology , Wuhan 430074, People’s Republic of China ; takata@hust.edu.cnYunnan Observatories, Chinese Academy of Sciences, 650011 Kunming, Yunnan Province, People’s Republic of China; Key Laboratory for the Structure and Evolution of Celestial Objects , Chinese Academy of Sciences, 650011 Kunming, People’s Republic of China; University of Chinese Academy of Sciences , 100049 Beijing, People’s Republic of ChinaYunnan Observatories, Chinese Academy of Sciences, 650011 Kunming, Yunnan Province, People’s Republic of China; Key Laboratory for the Structure and Evolution of Celestial Objects , Chinese Academy of Sciences, 650011 Kunming, People’s Republic of China; Center for Astronomical Mega-Science , Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, 100012 Beijing, People’s Republic ChinaYunnan Observatories, Chinese Academy of Sciences, 650011 Kunming, Yunnan Province, People’s Republic of China; Key Laboratory for the Structure and Evolution of Celestial Objects , Chinese Academy of Sciences, 650011 Kunming, People’s Republic of ChinaDepartment of Physics, National Changhua University of Education , Changhua 50007, TaiwanDepartment of Physics, National Cheng Kung University , Tainan 701401, TaiwanDepartment of Physics, National Cheng Kung University , Tainan 701401, TaiwanDepartment of Astronomy and Space Science, Chungnam National University , Daejeon 305-764, Republic of KoreaASASSN-V J205543.90+240033.5 (ASJ2055) is a possible post-common-envelope binary system. Its optical photometric data show an orbital variation of about 0.52 days and a fast period modulation of P _0 ∼ 9.77 minutes, whose origin is unknown. In this Letter, we report evidence of the stellar oscillation of the companion star as the origin of the fast period modulation. We analyze the photometric data taken by the Transiting Exoplanet Survey Satellite, the Liverpool Telescope, and the Lulin One-meter Telescope. It is found that the period of the 9.77 minutes signal measured in 2022 August is significantly shorter than that in 2021 July/August, and the magnitude of the change is of the order of ∣△ P _0 ∣/ P _0 ∼ 0.0008(4). Such a large variation will be incompatible with the scenario of the white dwarf (WD) spin as the origin of the 9.77 minutes periodic modulation. We suggest that the fast periodic signal is related to the emission from the irradiated companion star rather than that of the WD. Using existing photometric data covering a wide wavelength range, we estimate that the hot WD in ASJ2055 has a temperature of T _eff ∼ 80,000 K and is heating the oscillating M-type main-sequence star with T _eff ∼ 3500 K on its unirradiated surface. The stellar oscillation of the M-type main-sequence star has been predicted in theoretical studies, but no observational confirmation has been done. ASJ2055, therefore, has the potential to be a unique laboratory for investigating the stellar oscillation of an M-type main-sequence star and the heating effect on stellar oscillation.https://doi.org/10.3847/2041-8213/acec4cBinary starsWhite dwarf stars |
| spellingShingle | J. Takata A. K. H. Kong X. F. Wang F. F. Song J. Mao X. Hou C.-P. Hu L. C.-C. Lin K. L. Li C. Y. Hui Evidence of Stellar Oscillations in the Post-common-envelope Binary Candidate ASASSN-V J205543.90+240033.5 The Astrophysical Journal Letters Binary stars White dwarf stars |
| title | Evidence of Stellar Oscillations in the Post-common-envelope Binary Candidate ASASSN-V J205543.90+240033.5 |
| title_full | Evidence of Stellar Oscillations in the Post-common-envelope Binary Candidate ASASSN-V J205543.90+240033.5 |
| title_fullStr | Evidence of Stellar Oscillations in the Post-common-envelope Binary Candidate ASASSN-V J205543.90+240033.5 |
| title_full_unstemmed | Evidence of Stellar Oscillations in the Post-common-envelope Binary Candidate ASASSN-V J205543.90+240033.5 |
| title_short | Evidence of Stellar Oscillations in the Post-common-envelope Binary Candidate ASASSN-V J205543.90+240033.5 |
| title_sort | evidence of stellar oscillations in the post common envelope binary candidate asassn v j205543 90 240033 5 |
| topic | Binary stars White dwarf stars |
| url | https://doi.org/10.3847/2041-8213/acec4c |
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