摘要
First multi-wavelength photometric light curves(LCs)of the short-period eclipsing binary(EB)1 SWASP J034439.97+030425.5(hereafter J0344)are presented and analyzed by using the 2013 version of the Wilson-Devinney(W-D)code.To explain the asymmetric LCs of J0344,a cool star-spot on the less massive component was employed.The photometric solutions suggest that J0344 is a W-subtype shallow contact EB with a contact degree of f=4.9%±3.0%and a mass ratio of q=2.456±0.013.Moreover,an obvious third light was detected in our analysis.We calculated the average luminosity contribution of the third light to the total light,and that value reaches up to 49.78%.Based on the O-C method,the variations of the orbital period were studied for the first time.Our O-C diagram reveals a secular decrease superimposed on a cyclic oscillation.The orbital period decreases at a rate of d P/dt=-6.07×10-7 d yr-1,which can be explained by the mass transfer from the more massive component to the less massive one.Besides,its O-C diagram also shows a cyclic oscillation with an amplitude of 0.0030 d and a period about 7.08 yr,which can be explained by the presence of a third body with a minimum mass of M3 min=0.15±0.02 M⊙.The third component may play an important role in the formation and evolution of J0344 by drawing angular momentum from the central system.
作者
Bin Zhang
Sheng-Bang Qian
Jing-Jing Wang
Qi-Jun Zhi
Ai-Jun Dong
Wei Xie
Li-Ying Zhu
Lin-Qiao Jiang
张斌;钱声帮;王晶晶;支启军;董爱军;谢伟;朱俐颖;江林巧(School of Physics and Electronic Science,Guizhou Normal University,Guiyang 550001,China;Guizhou Provincial Key Laboratory of Radio Astronomy and Data Processing,Guizhou Normal University,Guiyang 550001,China;Yunnan Observatories,Chinese Academy of Sciences,Kunming 650216,China;Key Laboratory of the Structure and Evolution of Celestial Objects,Chinese Academy of Sciences,Kunming 650216,China;University of Chinese Academy of Sciences,Beijing 100049,China;Center for Astronomical Mega-Science,Chinese Academy of Sciences,Beijing 100101,China;China University of Petroleum-Beijing at Karamay,Karamay 834000,China;School of Physics and Electronic Engineering,Sichuan University of Science and Engineering,Zigong 643000,China)
基金
supported by the Natural Natural Science Foundation of China(NSFC)(Grant Nos.U1931101,11933008,11573063,U1731238,U1831120 and 11565010)
the Key Science Foundation of Yunnan Province(No.2017FA001)
the Special Funds for Theoretical Physics of the NSFC(No.11847102)
the Joint Research Fund in Astronomy(Grant Nos.U1631108 and U1831109)under cooperative agreement between the NSFC and the Chinese Academy of Sciences(CAS)
the research fund of Sichuan University of Science and Engineering(Grant No.2015RC42)
the Science Foundation of China University of Petroleum-Beijing At Karamay(No.RCYJ2016B-03-006)
the Key Laboratory for the Structure and Evolution of Celestial Objects,CAS(No.OP201708)
the Doctoral Starting up Foundation of Guizhou Normal University 2018(GZNUD[2018]12)
the Guizhou province’s innovation and entrepreneurial project for high-level overseas talents(Grant No.[2019]02)
supported by the Open Project Program of the Key Laboratory of Optical Astronomy,National Astronomical Observatories,Chinese Academy of Sciences。
