Analysis of Photometric Observations of the New Cataclysmic Variable ASASSN-13cx |
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| Authors: | T S Khruzina I B Voloshina S Qian V G Metlov |
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| Institution: | 1.Sternberg Astronomical Institute,Lomonosov Moscow State University,Moscow,Russia;2.Yunnan Observatories,Chinese Academy of Sciences,Kunming,People’s Republic of China;3.Crimean Astronomical Station,Lomonosov Moscow State University,Nauchnyi,Russia |
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| Abstract: | Photometric observations of the variable star ASASSN-13cx acquired in the course of a program of studies of cataclysmic variables and their parameters recently carried out at the Sternberg Astronomical Institute (SAI) are presented. The star was observed with the 50-cm and 60-cm telescopes of the SAI Crimean Astronomical Station and a CCD photometer (～1800 images in the V and Rc filters) during the variable’s outburst of August–September 2014 and in a period of quiescence in October–November 2016. The ASASSN-13cx system is confirmed to be a SU UMa variable. Parameters of the system are derived from eight light curves using a “composite” model that takes into account the presence of a hot spot on the lateral surface of the geometrically thick disk and of a region of enhanced energy release near the disk edge, at the base of the gas flow (the so-called “hot line”). Parameters of the system for three light curves during the outburst were obtained in the framework of a “spiral” model that additionally takes into account the presence of geometric perturbations on the accretion-disk surface. The parameters of ASASSN-13cx determined using these models provide good accuracy in reproducing the system’s light curves in both states. The basic parameters of the system have been determined for the first time: the component mass ratio q = M1/M2 = 7.0 ± 0.2, the orbital inclination i = 79.9°?80.1°, the distance between the components’ centers of mass a0 = 0.821(1) R?, and the sizes and temperatures of the stars: R1 = 0.0124(5)a0 = 0.0102(4) R?, T1 = 12 500 ± 280 K, 〈R2〉 = 0.236(4)a0 = 0.194(3) R?, T2 = 2550 ± 400 K, corresponding to M4–9V for the spectral type of the secondary. Parameters of the accretion disk have been derived for both activity states. The mass of matter in the accretion disk increased by almost a factor of two during ～400 orbital periods in quiescence. |
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