Physical parameters and orbital period variation of a newly discovered cataclysmic variable GSC 4560-02157

作     者：Zhong-Tao Han Sheng-Bang Qian Irina Voloshina Vladimir G. Metlov Li-Ying Zhu Lin-Jia Li 

作者机构：Yunnan Observatories Chinese Academy of Sciences Kunming 650216 China Key Laboratory of the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming 650216China University of Chinese Academy of Sciences Beijing 100049 China Sternberg Astronomical Institute Moscow State University Universitetskij prospect 13 Moscow 119992 Russia 

出 版 物：《Research in Astronomy and Astrophysics》 (天文和天体物理学研究（英文版）)

年 卷 期：2016年第16卷第10期

页      面：55-62页

核心收录：

学科分类：07[理学] 070401[理学-天体物理] 0704[理学-天文学] 

基　　金：partly supported by the National Natural Science Foundation of China(Nos.11133007 and 11325315) the Key Research Program of the Chinese Academy of Sciences(Grant No.KGZD-EW-603) the Science Foundation of Yunnan Province(Nos.2012HC011 and 2013FB084) by the Strategic Priority Research Program The Emergence of Cosmological Structures of the Chinese Academy of Sciences(No.XDB09010202) 

主　　题：techniques: photometric    stars: binaries: cataclysmic variables    stars: individual:GSC 4560 02157 

摘      要：GSC 4560-02157 is a new eclipsing cataclysmic variable with an orbital period of 0.265359 days. By using the published V- and R-band data together with our observations, we discovered that the O - C curve of GSC 4560-02157 may show a cyclic variation with a period of 3.51 years and an amplitude of 1.40 min. If this variation is caused by a light travel-time effect via the existence of a third body, then its mass can be derived as M3 sin i1≈ 91.08 Mjup, and it should be a low-mass star. In addition, several physical parameters were measured. The color of the secondary star was determined to be V - R = 0.77（±0.03） which corresponds to a spectral type of K2-3. The secondary star＇s mass was estimated as M2 = 0.73（±0.02） Mo by combing the derived V - R value around phase 0 with the assumption that it obeys the mass-luminosity relation for main sequence stars. This mass is consistent with the mass-period relation for CV donor stars. For the white dwarf, the eclipse durations and contacts of the white dwarf yield an upper limit on the white dwarf＇s radius corresponding to a lower limit on mass of M1 ≈ 0.501 M⊙. The overestimated radius and previously published spectral data indicate that the boundary layer may have a very high temperature.