Investigation of Superhumps in SU UMa-type Dwarf Novae Based on the Observations of TESS
We report a superhumps analysis of seven SU UMa-type dwarf novae based on observations made by the Transiting Exoplanet Survey Satellite (TESS). Superhumps are seen during the superoutbursts of SU UMa-type dwarf novae. The monthlong data sets of TESS are well suited for studying the variations of su...
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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/acebdf |
| _version_ | 1827292250353172480 |
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| author | Wei Liu Shengbang Qian |
| author_facet | Wei Liu Shengbang Qian |
| author_sort | Wei Liu |
| collection | DOAJ |
| description | We report a superhumps analysis of seven SU UMa-type dwarf novae based on observations made by the Transiting Exoplanet Survey Satellite (TESS). Superhumps are seen during the superoutbursts of SU UMa-type dwarf novae. The monthlong data sets of TESS are well suited for studying the variations of superhumps. We selected seven non-eclipsing SU UMa-type dwarf novae with superhumps in which TESS light curves are available and have not yet been studied. The A, B, and C stages of superhumps in superoutbursts were determined by the O − C method. The results indicate that not all complete superoutbursts show three obvious stages, such as DT Oct and the second superoutburst of J1730+6247. We calculated the superhump period for each stage and the mean period for all superoutbursts. Taking the stage A superhump method, the mass ratio (M2/M1) was estimated. According to the results, the seven stars are pre-bounce systems with mass ratios ranging from 0.1 to 0.2. By combining the orbital periods and the mean superhump periods, the precession periods were calculated. The results show that the precession periods of the seven SU UMa stars are about 2 days. |
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| language | English |
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| series | The Astrophysical Journal |
| spelling | doaj.art-9be944766be4432388128c626cbdb0bd2024-04-05T16:09:06ZengIOP PublishingThe Astrophysical Journal1538-43572023-01-01954213510.3847/1538-4357/acebdfInvestigation of Superhumps in SU UMa-type Dwarf Novae Based on the Observations of TESSWei Liu0https://orcid.org/0000-0002-0690-3273Shengbang Qian1Yunnan Observatories, Chinese Academy of Sciences , PO Box 110, Kunming 650216, People’s Republic of China ; qsb@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 Road, Huairou District, Beijing 101408, People’s Republic of China; Key Laboratory of the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences , PO Box 110, Kunming 650216, People’s Republic of ChinaYunnan Observatories, Chinese Academy of Sciences , PO Box 110, Kunming 650216, People’s Republic of China ; qsb@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 Road, Huairou District, Beijing 101408, People’s Republic of China; Key Laboratory of the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences , PO Box 110, Kunming 650216, People’s Republic of ChinaWe report a superhumps analysis of seven SU UMa-type dwarf novae based on observations made by the Transiting Exoplanet Survey Satellite (TESS). Superhumps are seen during the superoutbursts of SU UMa-type dwarf novae. The monthlong data sets of TESS are well suited for studying the variations of superhumps. We selected seven non-eclipsing SU UMa-type dwarf novae with superhumps in which TESS light curves are available and have not yet been studied. The A, B, and C stages of superhumps in superoutbursts were determined by the O − C method. The results indicate that not all complete superoutbursts show three obvious stages, such as DT Oct and the second superoutburst of J1730+6247. We calculated the superhump period for each stage and the mean period for all superoutbursts. Taking the stage A superhump method, the mass ratio (M2/M1) was estimated. According to the results, the seven stars are pre-bounce systems with mass ratios ranging from 0.1 to 0.2. By combining the orbital periods and the mean superhump periods, the precession periods were calculated. The results show that the precession periods of the seven SU UMa stars are about 2 days.https://doi.org/10.3847/1538-4357/acebdfDwarf novaeSU Ursae Majoris starsBinary stars |
| spellingShingle | Wei Liu Shengbang Qian Investigation of Superhumps in SU UMa-type Dwarf Novae Based on the Observations of TESS The Astrophysical Journal Dwarf novae SU Ursae Majoris stars Binary stars |
| title | Investigation of Superhumps in SU UMa-type Dwarf Novae Based on the Observations of TESS |
| title_full | Investigation of Superhumps in SU UMa-type Dwarf Novae Based on the Observations of TESS |
| title_fullStr | Investigation of Superhumps in SU UMa-type Dwarf Novae Based on the Observations of TESS |
| title_full_unstemmed | Investigation of Superhumps in SU UMa-type Dwarf Novae Based on the Observations of TESS |
| title_short | Investigation of Superhumps in SU UMa-type Dwarf Novae Based on the Observations of TESS |
| title_sort | investigation of superhumps in su uma type dwarf novae based on the observations of tess |
| topic | Dwarf novae SU Ursae Majoris stars Binary stars |
| url | https://doi.org/10.3847/1538-4357/acebdf |
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