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| Main Authors: | , , , , , , , , |
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| Format: | Preprint |
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2024
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| Subjects: | |
| Online Access: | https://arxiv.org/abs/2403.02621 |
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| _version_ | 1866929264678404096 |
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| author | Wu, Jin-Feng Zhu, Li-Ying Matekov, Azizbek Li, Lin-jia Ehgamberdiev, Shuhrat Asfandiyarov, Ildar Wang, Jiang-Jiao Zhang, Jia Meng, Fang-Bin |
| author_facet | Wu, Jin-Feng Zhu, Li-Ying Matekov, Azizbek Li, Lin-jia Ehgamberdiev, Shuhrat Asfandiyarov, Ildar Wang, Jiang-Jiao Zhang, Jia Meng, Fang-Bin |
| contents | We presented the multi-filter light curves of CSS_J154915.7+375506 inaugurally, which were observed by the 1.5 m AZT-22 telescope at Maidanak Astronomical Observatory. A low-resolution spectrum obtained by LAMOST reveals it is an A-type close binary. By analyzing the BVRI total-eclipse light curves, we are able to derive a reliable photometric solution for this system, which indicates that CSS_J154915.7+375506 is an extremely low-mass-ratio (q=0.138) marginal contact binary system. The location in the HR diagram shows that its secondary component with a much smaller mass is the more evolved one, indicating the mass ratio reversal occurred. The present secondary component had transferred a significant amount of mass to the present primary one. By the combination of a total of 20 times of minimum, we investigated its O-C curve. A periodic oscillation and a possible period decrease have been detected. As the period decreases, the system will evolve towards the contact phase. This makes CSS\_J154915.7+375506 a valuable case to study the formation scenario of contact binaries through mass reversal. The periodic oscillation suggested a third body with a minimal mass of $0.91\,M_{\odot}$, which is larger than that of the less massive component in the central binary. This implies that the secondary body was not replaced by the third body during early stellar interactions, indicating that it is a fossil system and retains its original dynamical information. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2403_02621 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | CSS_J154915.7+375506: A low-mass-ratio marginal contact binary system with a hierarchical third body Wu, Jin-Feng Zhu, Li-Ying Matekov, Azizbek Li, Lin-jia Ehgamberdiev, Shuhrat Asfandiyarov, Ildar Wang, Jiang-Jiao Zhang, Jia Meng, Fang-Bin Solar and Stellar Astrophysics We presented the multi-filter light curves of CSS_J154915.7+375506 inaugurally, which were observed by the 1.5 m AZT-22 telescope at Maidanak Astronomical Observatory. A low-resolution spectrum obtained by LAMOST reveals it is an A-type close binary. By analyzing the BVRI total-eclipse light curves, we are able to derive a reliable photometric solution for this system, which indicates that CSS_J154915.7+375506 is an extremely low-mass-ratio (q=0.138) marginal contact binary system. The location in the HR diagram shows that its secondary component with a much smaller mass is the more evolved one, indicating the mass ratio reversal occurred. The present secondary component had transferred a significant amount of mass to the present primary one. By the combination of a total of 20 times of minimum, we investigated its O-C curve. A periodic oscillation and a possible period decrease have been detected. As the period decreases, the system will evolve towards the contact phase. This makes CSS\_J154915.7+375506 a valuable case to study the formation scenario of contact binaries through mass reversal. The periodic oscillation suggested a third body with a minimal mass of $0.91\,M_{\odot}$, which is larger than that of the less massive component in the central binary. This implies that the secondary body was not replaced by the third body during early stellar interactions, indicating that it is a fossil system and retains its original dynamical information. |
| title | CSS_J154915.7+375506: A low-mass-ratio marginal contact binary system with a hierarchical third body |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2403.02621 |