Photometric Analysis of the Cataclysmic Variable Star LT Eri
LT Eri is a long-period eclipsing cataclysmic variable star (CV). This study investigates its outbursts, negative superhumps (NSHs), tilted-disk precession, eclipse-depth variations, and observed minus calculated ( O – C ) behavior, using photometric data from the Transiting Exoplanet Survey Satelli...
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IOP Publishing
2025-01-01
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| Series: | The Astronomical Journal |
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| Online Access: | https://doi.org/10.3847/1538-3881/ad9dd2 |
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| author | Qi-Bin Sun Sheng-Bang Qian Li-Ying Zhu Qin-Mei Li Fu-Xing Li Min-Yu Li Ping Li |
| author_facet | Qi-Bin Sun Sheng-Bang Qian Li-Ying Zhu Qin-Mei Li Fu-Xing Li Min-Yu Li Ping Li |
| author_sort | Qi-Bin Sun |
| collection | DOAJ |
| description | LT Eri is a long-period eclipsing cataclysmic variable star (CV). This study investigates its outbursts, negative superhumps (NSHs), tilted-disk precession, eclipse-depth variations, and observed minus calculated ( O – C ) behavior, using photometric data from the Transiting Exoplanet Survey Satellite (TESS), the Zwicky Transient Facility, the All-Sky Automated Survey for Supernovae, and the American Association of Variable Star Observers. Our analysis reveals an outburst period of 14.7(31) days, with variable periods ranging from 11.62(4) to 22.15(13) days. Both long and short outbursts were detected, lasting approximately 18 and 10 days, respectively. Analysis of the TESS photometry shows that the NSH period is updated to 0.16265161(7) days, persists during the outburst, and its amplitude is correlated with the outburst phase. A suspected signal of tilted-disk precession with a period of 3.5781(6) days is also detected. Additionally, the eclipse depth shows a periodic variation of 3.6270(9) days, closely matching the tilted-disk precession period; however, no biperiodic variation is found, as seen in the dwarf nova HS 2325+8205, suggesting that this phenomenon is not universal. An O – C analysis reveals a weak oscillation with a period of 3.5772(6) days. Our superposition of sine curves consistent with the NSH period and amplitude, along with mean eclipse curves, produces periodic O – C variations with a period of 3.6666(2) days. This indicates that the observed periodic variations in O – C , often around the disk precession period in CVs, may result from the beat between the NSHs and the eclipse rather than actual variations in the accretion disk. |
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| institution | Kabale University |
| issn | 1538-3881 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
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| series | The Astronomical Journal |
| spelling | doaj-art-ebc360fa697548b6897a5a74649ea3ee2025-01-13T17:16:40ZengIOP PublishingThe Astronomical Journal1538-38812025-01-0116926210.3847/1538-3881/ad9dd2Photometric Analysis of the Cataclysmic Variable Star LT EriQi-Bin Sun0Sheng-Bang Qian1Li-Ying Zhu2https://orcid.org/0000-0002-0796-7009Qin-Mei Li3Fu-Xing Li4https://orcid.org/0000-0002-0285-6051Min-Yu Li5https://orcid.org/0000-0002-8564-8193Ping Li6Department of Astronomy, School of Physics and Astronomy, Yunnan University , Kunming 650091, People’s Republic of China ; qiansb@ynu.edu.cn; Key Laboratory of Astroparticle Physics of Yunnan Province, Yunnan University , Kunming 650091, People’s Republic of ChinaDepartment of Astronomy, School of Physics and Astronomy, Yunnan University , Kunming 650091, People’s Republic of China ; qiansb@ynu.edu.cn; Key Laboratory of Astroparticle Physics of Yunnan Province, Yunnan University , Kunming 650091, People’s Republic of ChinaYunnan Observatories, Chinese Academy of Sciences , Kunming 650216, People’s Republic of China; University of Chinese Academy of Sciences , No. 19(A) Yuquan Road, Shijingshan District, Beijing, People's Republic of ChinaDepartment of Astronomy, School of Physics and Astronomy, Yunnan University , Kunming 650091, People’s Republic of China ; qiansb@ynu.edu.cn; Key Laboratory of Astroparticle Physics of Yunnan Province, Yunnan University , Kunming 650091, People’s Republic of China; Department of Physics, College of Physics, Guizhou University , Guiyang 550025, People’s Republic of ChinaYunnan Observatories, Chinese Academy of Sciences , Kunming 650216, People’s Republic of ChinaYunnan Observatories, Chinese Academy of Sciences , Kunming 650216, 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; University of Chinese Academy of Sciences , No. 19(A) Yuquan Road, Shijingshan District, Beijing, People's Republic of ChinaLT Eri is a long-period eclipsing cataclysmic variable star (CV). This study investigates its outbursts, negative superhumps (NSHs), tilted-disk precession, eclipse-depth variations, and observed minus calculated ( O – C ) behavior, using photometric data from the Transiting Exoplanet Survey Satellite (TESS), the Zwicky Transient Facility, the All-Sky Automated Survey for Supernovae, and the American Association of Variable Star Observers. Our analysis reveals an outburst period of 14.7(31) days, with variable periods ranging from 11.62(4) to 22.15(13) days. Both long and short outbursts were detected, lasting approximately 18 and 10 days, respectively. Analysis of the TESS photometry shows that the NSH period is updated to 0.16265161(7) days, persists during the outburst, and its amplitude is correlated with the outburst phase. A suspected signal of tilted-disk precession with a period of 3.5781(6) days is also detected. Additionally, the eclipse depth shows a periodic variation of 3.6270(9) days, closely matching the tilted-disk precession period; however, no biperiodic variation is found, as seen in the dwarf nova HS 2325+8205, suggesting that this phenomenon is not universal. An O – C analysis reveals a weak oscillation with a period of 3.5772(6) days. Our superposition of sine curves consistent with the NSH period and amplitude, along with mean eclipse curves, produces periodic O – C variations with a period of 3.6666(2) days. This indicates that the observed periodic variations in O – C , often around the disk precession period in CVs, may result from the beat between the NSHs and the eclipse rather than actual variations in the accretion disk.https://doi.org/10.3847/1538-3881/ad9dd2Eclipsing binary starsCataclysmic variable stars |
| spellingShingle | Qi-Bin Sun Sheng-Bang Qian Li-Ying Zhu Qin-Mei Li Fu-Xing Li Min-Yu Li Ping Li Photometric Analysis of the Cataclysmic Variable Star LT Eri The Astronomical Journal Eclipsing binary stars Cataclysmic variable stars |
| title | Photometric Analysis of the Cataclysmic Variable Star LT Eri |
| title_full | Photometric Analysis of the Cataclysmic Variable Star LT Eri |
| title_fullStr | Photometric Analysis of the Cataclysmic Variable Star LT Eri |
| title_full_unstemmed | Photometric Analysis of the Cataclysmic Variable Star LT Eri |
| title_short | Photometric Analysis of the Cataclysmic Variable Star LT Eri |
| title_sort | photometric analysis of the cataclysmic variable star lt eri |
| topic | Eclipsing binary stars Cataclysmic variable stars |
| url | https://doi.org/10.3847/1538-3881/ad9dd2 |
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