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YZ Phoenicis: a very short period K-type contact binary with variation of the O'Connell effect and orbital period change
Sarotsakulchai, Thawicharat1,2,3; Qian SB(钱声帮)1,2,4,5; Soonthornthum, Boonrucksar3; Zhou X(周肖)1,4,5; Zhang J(张嘉)1,4,5; Li LJ(李临甲)1,4,5; Reichart, Daniel E.6; Haislip, Joshua B.6; Kouprianov, Vladimir V.6; Poshyachinda, Saran3
发表期刊PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN
2019-08-01
卷号71期号:4页码:18
DOI10.1093/pasj/psz062
产权排序第1完成单位
收录类别SCI ; EI
关键词binaries: close binaries: eclipsing stars: evolution stars: starspots stars: individual (YZ Phoenicis)
摘要

YZPhe is a very short-period contact binary (Sp. = K2V) with an orbital period of 0.2347d near the short period limit (0.22d). We present the complete light curves which photometric data were obtained from the 60 cm telescope of PROMPT-8 at CTIO in Chile during 2016 June to October and 2017 August. The photometric solutions were determined by using the Wilson & Devinney code and the results reveal that YZPhe is a W-subtype shallow contact binary (, q = 2.635, or 1/q = 0.379 for W subtype) with rotational motion of a large hot spot on the more massive component, showing a strong O'Connell effect with variation of maxima in photometric time series at period of 4.20yr and stellar cycle at period of 1.28yr. By compiling all available eclipse times, the result shows a long-term period decrease at a rate of dP/dt = -2.64(+/- 0.02) x 10(-8)dyr(-1), superimposed on a cyclic variation (A(3) = 0.0081d and P-3 = 40.76yr). This variation cannot be explained by the Applegate mechanism. Thus, the cyclic change may be interpreted as the light-travel time effect via the presence of a cool third body. Based on photometric solutions, the third light was detected as of the total light in V and I bands. These results support the existence of a third body. The long-term period decrease can be explained by mass transfer from the more massive component () to the less massive one () or plus angular momentum loss (AML) via magnetic braking. With 1/q < 0.4 and long-term period decrease, all factors suggest that YZPhe is on the AML-controlled state and its fill-out factor will increase, as well as the system evolving into a deeper normal contact binary.

资助项目Chinese Natural Science Foundation[11703080] ; Chinese Natural Science Foundation[11703082] ; Yunnan Natural Science Foundation[2018FB006] ; [CZ. 1.05/3.2.00/08.0144]
项目资助者Chinese Natural Science Foundation[11703080, 11703082] ; Yunnan Natural Science Foundation[2018FB006] ; [CZ. 1.05/3.2.00/08.0144]
语种英语
学科领域天文学 ; 恒星与银河系 ; 恒星形成与演化
文章类型Article
出版者OXFORD UNIV PRESS
出版地GREAT CLARENDON ST, OXFORD OX2 6DP, ENGLAND
ISSN0004-6264
URL查看原文
WOS记录号WOS:000482425000015
WOS研究方向Astronomy & Astrophysics
WOS类目Astronomy & Astrophysics
关键词[WOS]SKY AUTOMATED SURVEY ; ECLIPSING BINARIES ; ADDITIONAL COMPONENTS ; EVOLUTIONARY STATUS ; VARIABLE-STARS ; CLOSE BINARIES ; LIGHT ; LIMIT ; MODULATION ; MECHANISM
EI入藏号20215211380454
EI主题词Photometry
EI分类号431 Air Transportation - 432 Highway Transportation - 433 Railroad Transportation - 434 Waterway Transportation - 641.3 Mass Transfer - 657.2 Extraterrestrial Physics and Stellar Phenomena - 941.4 Optical Variables Measurements
引用统计
被引频次:11[WOS]   [WOS记录]     [WOS相关记录]
文献类型期刊论文
条目标识符http://ir.ynao.ac.cn/handle/114a53/21162
专题双星与变星研究组
中国科学院天体结构与演化重点实验室
通讯作者Sarotsakulchai, Thawicharat
作者单位1.Yunnan Observatories, Chinese Academy of Sciences, 650216 Kunming, China
2.University of Chinese Academy of Sciences, 19 A Yuquan Rd., Shijingshan, 100049 Beijing, China
3.National Astronomical Research Institute of Thailand, Donkaew, Maerim, Chiang Mai 50180, Thailand
4.Key Laboratory of the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, 650216 Kunming, China
5.Center forAstronomical Mega-Science, ChineseAcademyof Sciences, 20A Datun Rd., ChaoyangDistrict, 100012 Beijing, China
6.Department of Physics and Astronomy, University of North Carolina, CB #3255, Chapel Hill, NC 27599, USA
第一作者单位中国科学院云南天文台
通讯作者单位中国科学院云南天文台
推荐引用方式
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Sarotsakulchai, Thawicharat,Qian SB,Soonthornthum, Boonrucksar,et al. YZ Phoenicis: a very short period K-type contact binary with variation of the O'Connell effect and orbital period change[J]. PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN,2019,71(4):18.
APA Sarotsakulchai, Thawicharat.,Qian SB.,Soonthornthum, Boonrucksar.,Zhou X.,Zhang J.,...&Poshyachinda, Saran.(2019).YZ Phoenicis: a very short period K-type contact binary with variation of the O'Connell effect and orbital period change.PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN,71(4),18.
MLA Sarotsakulchai, Thawicharat,et al."YZ Phoenicis: a very short period K-type contact binary with variation of the O'Connell effect and orbital period change".PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 71.4(2019):18.
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