TY Pup: A Low-mass-ratio and Deep Contact Binary as a Progenitor Candidate of Luminous Red Novae
文献类型:期刊论文
作者 | Sarotsakulchai, T.1,2,3; Qian SB(钱声帮)1,2,4,5; Soonthornthum, B.3; Zhou X(周肖)1,4,5; Zhang J(张嘉)1,4,5; Reichart, D. E.6; Haislip, J. B.6; Kouprianov, V. V.6; Poshyachinda, S.3 |
刊名 | ASTRONOMICAL JOURNAL |
出版日期 | 2018-11-01 |
卷号 | 156期号:5页码:11 |
ISSN号 | 0004-6256 |
关键词 | binaries: close binaries: eclipsing stars: evolution stars: individual (TY Pup) |
DOI | 10.3847/1538-3881/aadcfa |
文献子类 | Article |
英文摘要 | TY Pup is a well-known bright eclipsing binary with an orbital period of 0.8192 days. New light curves in B, V, (RI)(C) bands were obtained with the 0.61 m reflector robotic telescope (PROMPT-8) at CTIO in Chile during 2015 and 2017. By analyzing those photometric data with the W-D method, it is found that TY Pup is a low-mass-ratio (q similar to 0.184) and deep-contact binary with a high fill-out factor (84.3%). An investigation of all available times of minimum light including three new ones obtained with the 60 cm and the 1.0 m telescopes at Yunnan Observatories in China indicates that the period change of TY Pup is complex. An upward parabolic variation in the O - C diagram is detected to be superimposed on a cyclic oscillation. The upward parabolic change reveals a long-term continuous increase in the orbital period at a rate of dP/dt = 5.57(+/- 0.08) x 10(-8) days yr(-1). The period increase can be explained by mass transfer from the less massive component (M-2 similar to 0.3 M-circle dot) to the more massive one (M-1 similar to 1.65 M-circle dot). The binary will be merging when it meets the criterion that the orbital angular momentum is less than three times the total spin angular momentum, i.e., J(orb) < 3J(rot). This suggests that the system will finally merge into a rapid-rotating single star and may produce a luminous red nova. The cyclic oscillation in the O - C diagram can be interpreted by the light-travel time effect via the presence of a third body. |
学科主题 | 天文学 |
URL标识 | 查看原文 |
出版地 | TEMPLE CIRCUS, TEMPLE WAY, BRISTOL BS1 6BE, ENGLAND |
WOS关键词 | THERMAL RELAXATION OSCILLATION ; SKY AUTOMATED SURVEY ; ADDITIONAL COMPONENTS ; LIGHT CURVES ; EFFECTIVE TEMPERATURES ; BOLOMETRIC CORRECTIONS ; ECLIPSING BINARIES ; STARS ; SYSTEMS ; PARAMETERS |
资助项目 | National Natural Science Foundation of China[11703082] |
WOS研究方向 | Astronomy & Astrophysics |
语种 | 英语 |
出版者 | IOP PUBLISHING LTD |
WOS记录号 | WOS:000447164500009 |
资助机构 | National Natural Science Foundation of China[11703082] |
源URL | [http://ir.ynao.ac.cn/handle/114a53/18022] |
专题 | 云南天文台_双星与变星研究组 云南天文台_中国科学院天体结构与演化重点实验室 |
通讯作者 | Sarotsakulchai, T. |
作者单位 | 1.Yunnan Observatories, Chinese Academy of Sciences, 650216 Kunming, People's Republic of China 2.University of Chinese Academy of Sciences, 19 A Yuquan Rd., Shijingshan, 100049 Beijing, People's Republic of China 3.National Astronomical Research Institute of Thailand, Ministry of Science and Technology, Bangkok, Thailand 4.Key Laboratory of the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, 650216 Kunming, People's Republic of China 5.Center for Astronomical Mega-Science, Chinese Academy of Sciences, 20A Datun Rd., Chaoyang District, Beijing, 100012, People's Republic of China 6.Department of Physics and Astronomy, University of North Carolina, CB #3255, Chapel Hill, NC 27599, USA |
推荐引用方式 GB/T 7714 | Sarotsakulchai, T.,Qian SB,Soonthornthum, B.,et al. TY Pup: A Low-mass-ratio and Deep Contact Binary as a Progenitor Candidate of Luminous Red Novae[J]. ASTRONOMICAL JOURNAL,2018,156(5):11. |
APA | Sarotsakulchai, T..,Qian SB.,Soonthornthum, B..,Zhou X.,Zhang J.,...&Poshyachinda, S..(2018).TY Pup: A Low-mass-ratio and Deep Contact Binary as a Progenitor Candidate of Luminous Red Novae.ASTRONOMICAL JOURNAL,156(5),11. |
MLA | Sarotsakulchai, T.,et al."TY Pup: A Low-mass-ratio and Deep Contact Binary as a Progenitor Candidate of Luminous Red Novae".ASTRONOMICAL JOURNAL 156.5(2018):11. |
入库方式: OAI收割
来源:云南天文台
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