2017/05/09 by Z.-T. Han, Han, Zhong-tao, S.‐B. Qian +9
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysical Phenomena and Observations #Astrophysics of Galaxies (astro-ph.GA) #FOS: Physical sciences #Stellar, planetary, and galactic studies
paper · pdf · doi:10.48550/arxiv.1705.03160
openalex publication_date 2017/05/09 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
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 shows a cyclic variation with the 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, its mass can be derived as M3sini'≈91.08MJup, it should be a low-mass star. In addition, several physical parameters were measured. The colour of the secondary star was determined as 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)M\odot by combing the derived V-R value around phase 0 with the assumption that it obeys the mass-luminosity relation of the main sequence stars. This mass is consistent with the mass-period relation of CV donor stars. For the white dwarf, the eclipse durations and contacts of the white dwarf yield an upper limit of the white dwarf's radius corresponding to a lower limit mass of M1≈0.501M\odot. The overestimated radius and previously published spectral data indicate that the boundary layer may has a very high temperature.