Nine New Cataclysmic Variable Stars with Negative Superhumps
Negative superhumps (NSHs) are signals a few percent shorter than the orbital period of a binary star and are considered to originate from the reverse precession of the tilted disk. Based on TESS photometry, we find nine new cataclysmic variable stars with NSHs. Three (ASAS J1420, TZ Per, and V392 H...
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| Format: | Article |
| Language: | English |
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IOP Publishing
2024-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/ad0f1c |
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| author | Qi-Bin Sun Sheng-Bang Qian Li-Ying Zhu Wen-Ping Liao Er-Gang Zhao Fu-Xing Li Xiang-Dong Shi Min-Yu Li |
| author_facet | Qi-Bin Sun Sheng-Bang Qian Li-Ying Zhu Wen-Ping Liao Er-Gang Zhao Fu-Xing Li Xiang-Dong Shi Min-Yu Li |
| author_sort | Qi-Bin Sun |
| collection | DOAJ |
| description | Negative superhumps (NSHs) are signals a few percent shorter than the orbital period of a binary star and are considered to originate from the reverse precession of the tilted disk. Based on TESS photometry, we find nine new cataclysmic variable stars with NSHs. Three (ASAS J1420, TZ Per, and V392 Hya) of these stars similar to AH Her still have NSHs during dwarf nova outbursts, and the NSH amplitude varies with the outburst. The variation in the radius of the accretion disk partially explains this phenomenon. However, it does not explain the rebound of the NSH amplitude after the peak of the outburst and the fact that the NSH amplitude of the quiescence is sometimes not the largest, and it is necessary to include the disk instability model (DIM) and add other ingredients. Therefore, we suggest that the variation of NSH amplitude with outburst can be an important basis for studying the origin of NSHs and improving the DIM. The six (ASASSN-V J1137, ASASSN-V J0611, 2MASS J0715, LAMOST J0925, ASASSN-17qj, and ZTF 18acakuxo) remaining stars have been poorly studied, and for the first time we determine their orbital periods, NSHs, and superorbital signal (SOR) periods. The NSH periods and amplitudes of ASASSN-V J1137 and ASASSN-17qj vary with the SOR, and based on the comparison of the observations with the theory, we suggest that a single change in tilted disk angle does not explain the observations of the SOR and that other ingredients need to be considered as well. |
| first_indexed | 2024-03-08T02:53:04Z |
| format | Article |
| id | doaj.art-666b12549b004977946a640519c922a0 |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-08T02:53:04Z |
| publishDate | 2024-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-666b12549b004977946a640519c922a02024-02-13T13:05:40ZengIOP PublishingThe Astrophysical Journal1538-43572024-01-01962212310.3847/1538-4357/ad0f1cNine New Cataclysmic Variable Stars with Negative SuperhumpsQi-Bin Sun0https://orcid.org/0000-0003-0516-404XSheng-Bang Qian1Li-Ying Zhu2https://orcid.org/0000-0002-0796-7009Wen-Ping Liao3https://orcid.org/0000-0001-9346-9876Er-Gang Zhao4Fu-Xing Li5https://orcid.org/0000-0002-0285-6051Xiang-Dong Shi6https://orcid.org/0000-0002-5038-5952Min-Yu Li7https://orcid.org/0000-0002-8564-8193Yunnan Observatories, Chinese Academy of Sciences , 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 sunqibin@ynao.ac.cn; Key Laboratory of the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences , Kunming 650216, People’s Republic of China; Center for Astronomical Mega-Science, Chinese Academy of Sciences , 20A Datun Road, Chaoyang District, Beijing, 100012, People’s Republic of China; University of Chinese Academy of Sciences , No.19(A) Yuquan Road, Shijingshan District, Beijing, People’s Republic of ChinaYunnan Observatories, Chinese Academy of Sciences , 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 sunqibin@ynao.ac.cn; Key Laboratory of the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences , Kunming 650216, People’s Republic of China; Center for Astronomical Mega-Science, Chinese Academy of Sciences , 20A Datun Road, Chaoyang District, Beijing, 100012, People’s Republic of China; University of Chinese Academy of Sciences , No.19(A) Yuquan Road, Shijingshan District, Beijing, People’s Republic of ChinaYunnan Observatories, Chinese Academy of Sciences , Kunming 650216, People’s Republic of China ; qsb@ynao.ac.cn; Key Laboratory of the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences , Kunming 650216, People’s Republic of China; Center for Astronomical Mega-Science, Chinese Academy of Sciences , 20A Datun Road, Chaoyang District, Beijing, 100012, People’s Republic of China; University of Chinese Academy of Sciences , No.19(A) Yuquan Road, Shijingshan District, Beijing, People’s Republic of ChinaYunnan Observatories, Chinese Academy of Sciences , Kunming 650216, People’s Republic of China ; qsb@ynao.ac.cn; Key Laboratory of the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences , Kunming 650216, People’s Republic of China; Center for Astronomical Mega-Science, Chinese Academy of Sciences , 20A Datun Road, Chaoyang District, Beijing, 100012, People’s Republic of China; University of Chinese Academy of Sciences , No.19(A) Yuquan Road, Shijingshan District, Beijing, People’s Republic of ChinaYunnan Observatories, Chinese Academy of Sciences , Kunming 650216, People’s Republic of China ; qsb@ynao.ac.cn; Key Laboratory of the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences , Kunming 650216, People’s Republic of China; Center for Astronomical Mega-Science, Chinese Academy of Sciences , 20A Datun Road, Chaoyang District, Beijing, 100012, People’s Republic of ChinaYunnan Observatories, Chinese Academy of Sciences , Kunming 650216, People’s Republic of China ; qsb@ynao.ac.cn; Key Laboratory of the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences , Kunming 650216, People’s Republic of China; Center for Astronomical Mega-Science, Chinese Academy of Sciences , 20A Datun Road, Chaoyang District, Beijing, 100012, People’s Republic of ChinaYunnan Observatories, Chinese Academy of Sciences , Kunming 650216, People’s Republic of China ; qsb@ynao.ac.cn; Key Laboratory of the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences , Kunming 650216, People’s Republic of China; Center for Astronomical Mega-Science, Chinese Academy of Sciences , 20A Datun Road, Chaoyang District, Beijing, 100012, People’s Republic of ChinaYunnan Observatories, Chinese Academy of Sciences , Kunming 650216, People’s Republic of China ; qsb@ynao.ac.cn; Key Laboratory of the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences , Kunming 650216, People’s Republic of China; Center for Astronomical Mega-Science, Chinese Academy of Sciences , 20A Datun Road, Chaoyang District, Beijing, 100012, People’s Republic of China; University of Chinese Academy of Sciences , No.19(A) Yuquan Road, Shijingshan District, Beijing, People’s Republic of ChinaNegative superhumps (NSHs) are signals a few percent shorter than the orbital period of a binary star and are considered to originate from the reverse precession of the tilted disk. Based on TESS photometry, we find nine new cataclysmic variable stars with NSHs. Three (ASAS J1420, TZ Per, and V392 Hya) of these stars similar to AH Her still have NSHs during dwarf nova outbursts, and the NSH amplitude varies with the outburst. The variation in the radius of the accretion disk partially explains this phenomenon. However, it does not explain the rebound of the NSH amplitude after the peak of the outburst and the fact that the NSH amplitude of the quiescence is sometimes not the largest, and it is necessary to include the disk instability model (DIM) and add other ingredients. Therefore, we suggest that the variation of NSH amplitude with outburst can be an important basis for studying the origin of NSHs and improving the DIM. The six (ASASSN-V J1137, ASASSN-V J0611, 2MASS J0715, LAMOST J0925, ASASSN-17qj, and ZTF 18acakuxo) remaining stars have been poorly studied, and for the first time we determine their orbital periods, NSHs, and superorbital signal (SOR) periods. The NSH periods and amplitudes of ASASSN-V J1137 and ASASSN-17qj vary with the SOR, and based on the comparison of the observations with the theory, we suggest that a single change in tilted disk angle does not explain the observations of the SOR and that other ingredients need to be considered as well.https://doi.org/10.3847/1538-4357/ad0f1cBinary starsCataclysmic variable starsDwarf novae |
| spellingShingle | Qi-Bin Sun Sheng-Bang Qian Li-Ying Zhu Wen-Ping Liao Er-Gang Zhao Fu-Xing Li Xiang-Dong Shi Min-Yu Li Nine New Cataclysmic Variable Stars with Negative Superhumps The Astrophysical Journal Binary stars Cataclysmic variable stars Dwarf novae |
| title | Nine New Cataclysmic Variable Stars with Negative Superhumps |
| title_full | Nine New Cataclysmic Variable Stars with Negative Superhumps |
| title_fullStr | Nine New Cataclysmic Variable Stars with Negative Superhumps |
| title_full_unstemmed | Nine New Cataclysmic Variable Stars with Negative Superhumps |
| title_short | Nine New Cataclysmic Variable Stars with Negative Superhumps |
| title_sort | nine new cataclysmic variable stars with negative superhumps |
| topic | Binary stars Cataclysmic variable stars Dwarf novae |
| url | https://doi.org/10.3847/1538-4357/ad0f1c |
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